Faculty Profiles - INUTSUKA, Shu-ichiro

Papers - INUTSUKA, Shu-ichiro

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A Tale of Three: Magnetic Fields along the Orion Integral-shaped Filament as Revealed by the JCMT BISTRO Survey Reviewed International coauthorship International journal Open Access

Astrophysical Journal Letters Vol. 977 ( 2 ) 2024.12

"Two-dimensional Study of the Propagation of Planetary Wake and the Indication of Gap Opening in an Inviscid Protoplanetary Disk" (vol 724, 448, 2010) Reviewed Open Access

Muto, T; Suzuki, TK; Inutsuka, SI

ASTROPHYSICAL JOURNAL Vol. 973 ( 1 ) 2024.9

FEASTS Combined with Interferometry. II. Significantly Changed H I Surface Densities and Even More Inefficient Star Formation in Galaxy Outer Disks Reviewed International coauthorship Open Access

Wang, J; Lin, XC; Staveley-Smith, L; Yang, D; Walter, F; Liang, ZZ; Shi, Y; Fu, J; Guo, H; Ho, LC; Inutsuka, S; Jiang, FZ; Jiang, P; Qu, ZJ; Shao, L

ASTROPHYSICAL JOURNAL Vol. 973 ( 1 ) 2024.9

Relative alignments between magnetic fields, velocity gradients, and dust emission gradients in NGC 1333 Reviewed International coauthorship Open Access

Chen, MCY; Fissel, LM; Sadavoy, S; Rosolowsky, E; Doi, Y; Arzoumanian, D; Bastien, P; Coude, S; Di Francesco, J; Friesen, R; Furuya, RS; Hwang, J; Inutsuka, S; Johnstone, D; Karoly, J; Kwon, J; Kwon, W; Le Gouellec, VJM; Liu, HL; Mairs, S; Onaka, T; Pattle, K; Rawlings, MG; Tahani, M; Tamura, M; Wang, JW

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY Vol. 533 ( 2 ) page： 1938 - 1959 2024.8

MHD Simulation in Galactic Center Region with Radiative Cooling and Heating Reviewed Open Access

ASTROPHYSICAL JOURNAL Vol. 966 ( 2 ) 2024.5

Discovery of Asymmetric Spike-like Structures of the 10 au Disk around the Very Low-luminosity Protostar Embedded in the Taurus Dense Core MC 27/L1521F with ALMA Reviewed Open Access

Tokuda, K; Harada, N; Omura, M; Matsumoto, T; Onishi, T; Saigo, K; Shoshi, A; Nozaki, S; Tachihara, K; Fukaya, N; Fukui, Y; Inutsuka, S; Machida, MN

ASTROPHYSICAL JOURNAL Vol. 965 ( 2 ) 2024.4

Evolution of the Angular Momentum of Molecular Cloud Cores in Magnetized Molecular Filaments Reviewed International coauthorship Open Access

Misugi, Y; Inutsuka, SI; Arzoumanian, D; Tsukamoto, Y

ASTROPHYSICAL JOURNAL Vol. 963 ( 2 ) 2024.3

The history of the Milky Way: The evolution of star formation, cosmic rays, metallicity, and stellar dynamics over cosmic time Reviewed Open Access

Shimoda, J; Inutsuka, SI; Nagashima, M

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN Vol. 76 ( 1 ) page： 81 - 97 2024.2

Filamentary Network and Magnetic Field Structures Revealed with BISTRO in the High-mass Star-forming Region NGC 2264: Global Properties and Local Magnetogravitational Configurations Reviewed Open Access

Wang, JW; Koch, PM; Clarke, SD; Fuller, G; Peretto, N; Tang, YW; Yen, HW; Lai, SP; Ohashi, N; Arzoumanian, D; Johnstone, D; Furuya, R; Inutsuka, SI; Lee, CW; Ward-Thompson, D; Le Gouellec, VJM; Liu, HL; Fanciullo, L; Hwang, J; Pattle, K; Poidevin, F; Tahani, M; Onaka, T; Rawlings, MG; Chung, EJ; Liu, JH; Lyo, AR; Priestley, F; Hoang, T; Tamura, M; Berry, D; Bastien, P; Ching, TC; Coudé, S; Kwon, W; Chen, MK; Eswaraiah, C; Soam, A; Hasegawa, T; Qiu, KP; Bourke, TL; Byun, D; Chen, ZW; Chen, HRV; Chen, WP; Cho, JY; Choi, M; Choi, Y; Choi, Y; Chrysostomou, A; Dai, SP; Di Francesco, J; Diep, PN; Doi, Y; Duan, Y; Duan, HY; Eden, D; Fiege, J; Fissel, LM; Franzmann, E; Friberg, P; Friesen, R; Gledhill, T; Graves, S; Greaves, J; Griffin, M; Gu, QL; Han, IL; Hayashi, S; Houde, M; Inoue, T; Iwasaki, K; Jeong, I; Könyves, V; Kang, JH; Kang, MJ; Karoly, J; Kataoka, A; Kawabata, K; Khan, Z; Kim, MR; Kim, KT; Kim, KH; Kim, S; Kim, J; Kim, H; Kim, G; Kirchschlager, F; Kirk, J; Kobayashi, MIN; Kusune, T; Kwon, J; Lacaille, K; Law, CY; Lee, SS; Lee, HYS; Lee, JE; Lee, CF; Li, DL; Li, HB; Li, GX; Li, D; Lin, SJ; Liu, T; Liu, SY; Lu, X; Mairs, S; Matsumura, M; Matthews, B; Moriarty-Schieven, G; Nagata, T; Nakamura, F; Nakanishi, H; Ngoc, NB; Park, G; Parsons, H; Pyo, TS; Qian, L; Rao, RMS; Rawlings, J; Retter, B; Richer, J; Rigby, A; Sadavoy, S; Saito, H; Savini, G; Seta, M; Sharma, E; Shimajiri, Y; Shinnaga, H; Tang, XD; Thuong, HD; Tomisaka, K; Tram, L; Tsukamoto, Y; Viti, S; Wang, HC; Whitworth, A; Wu, JT; Xie, JJ; Yang, MZ; Yoo, H; Yuan, JH; Yun, HS; Zenko, T; Zhang, CP; Zhang, YP; Zhang, GY; Zhou, JJ; Zhu, L; de Looze, I; André, P; Dowell, CD; Eyres, S; Falle, S; Robitaille, JF; van Loo, S

ASTROPHYSICAL JOURNAL Vol. 962 ( 2 ) 2024.2

Growth of Massive Molecular Cloud Filament by Accretion Flows. I. Slow-shock Instability versus Ambipolar Diffusion Reviewed Open Access

Abe, Daisei; Inoue, Tsuyoshi; Inutsuka, Shu-ichiro

The Astrophysical Journal Vol. 961 ( 1 ) page： 100 2024.1

An improved dynamical Poisson equation solver for self-gravity Reviewed Open Access

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY Vol. 527 ( 1 ) page： 471 - 477 2024.1

Co-evolution of dust grains and protoplanetary disks Reviewed Open Access

Tsukamoto, Y; Machida, MN; Inutsuka, SI

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN Vol. 75 ( 5 ) page： 835 - 852 2023.10

Giant Impact Events for Protoplanets: Energetics of Atmospheric Erosion by Head-on Collision

Kurosaki, K; Inutsuka, S

ASTROPHYSICAL JOURNAL Vol. 954 ( 2 ) 2023.9

On Secular Gravitational Instability in Vertically Stratified Disks

Tominaga, RT; Inutsuka, S; Takahashi, SZ

ASTROPHYSICAL JOURNAL Vol. 953 ( 1 ) 2023.8

Triple Spiral Arms of a Triple Protostar System Imaged in Molecular Lines Reviewed International coauthorship International journal Open Access

Lee, JE; Matsumoto, T; Kim, HJ; Lee, S; Harsono, D; Bae, J; Evans, J II; Inutsuka, SI; Choi, M; Tatematsu, K; Lee, JJ; Jaffe, D

ASTROPHYSICAL JOURNAL Vol. 953 ( 1 ) 2023.8

The JCMT BISTRO Survey: Studying the Complex Magnetic Field of L43

Karoly, J; Ward-Thompson, D; Pattle, K; Berry, D; Whitworth, A; Kirk, J; Bastien, P; Ching, TC; Coudé, S; Hwang, J; Kwon, W; Soam, A; Wang, JW; Hasegawa, T; Lai, SP; Qiu, KP; Arzoumanian, D; Bourke, TL; Byun, DY; Chen, HRV; Chen, WP; Chen, M; Chen, ZW; Cho, J; Choi, M; Choi, Y; Choi, Y; Chrysostomou, A; Chung, EJ; Dai, S; Debattista, V; Di Francesco, J; Diep, PN; Doi, Y; Duan, HY; Duan, Y; Eswaraiah, C; Fanciullo, L; Fiege, J; Fissel, LM; Franzmann, E; Friberg, P; Friesen, R; Fuller, G; Furuya, R; Gledhill, T; Graves, S; Greaves, J; Griffin, M; Gu, QL; Han, IL; Hoang, T; Houde, M; Hull, CLH; Inoue, T; Inutsuka, S; Iwasaki, K; Jeong, IG; Johnstone, D; Koenyves, V; Kang, JH; Kang, MJ; Kataoka, A; Kawabata, K; Kemper, F; Kim, J; Kim, S; Kim, G; Kim, KH; Kim, MR; Kim, KT; Kim, H; Kirchschlager, F; Kobayashi, MIN; Koch, PM; Kusune, T; Kwon, J; Lacaille, K; Law, CY; Lee, CW; Lee, HYS; Lee, YH; Lee, CF; Lee, JE; Lee, SS; Li, DL; Li, D; Li, GX; Li, HB; Lin, SJ; Liu, HL; Liu, T; Liu, SY; Liu, JH; Longmore, S; Lu, X; Lyo, AR; Mairs, S; Matsumura, M; Matthews, B; Moriarty-Schieven, G; Nagata, T; Nakamura, F; Nakanishi, H; Ngoc, NB; Ohashi, N; Onaka, T; Park, G; Parsons, H; Peretto, N; Priestley, F; Pyo, TS; Qian, L; Rao, RMS; Rawlings, J; Rawlings, M; Retter, B; Richer, J; Rigby, A; Sadavoy, S; Saito, H; Savini, G; Seta, M; Sharma, E; Shimajiri, Y; Shinnaga, H; Tahani, M; Tamura, M; Tang, YW; Tang, XD; Tomisaka, K; Tram, L; Tsukamoto, Y; Viti, S; Wang, HC; Wu, JT; Xie, JJ; Yang, MZ; Yen, HW; Yoo, H; Yuan, JH; Yun, HS; Zenko, T; Zhang, GY; Zhang, YP; Zhang, CP; Zhou, JJ; Zhu, L; de Looze, I; Andre, P; Dowell, CD; Eden, D; Eyres, S; Falle, S; Le Gouellec, VJM; Poidevin, F; Robitaille, JF; van Loo, S

ASTROPHYSICAL JOURNAL Vol. 952 ( 1 ) 2023.7

Efficient radial migration by giant molecular clouds in the first several hundred Myr after the stellar birth

Fujimoto, Y; Inutsuka, SI; Baba, J

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY Vol. 523 ( 2 ) page： 3049 - 3068 2023.5

First BISTRO Observations of the Dark Cloud Taurus L1495A-B10: The Role of the Magnetic Field in the Earliest Stages of Low-mass Star Formation

Ward-Thompson, D; Karoly, J; Pattle, K; Whitworth, A; Kirk, J; Berry, D; Bastien, P; Ching, TC; Coudé, S; Hwang, J; Kwon, W; Soam, A; Wang, JW; Hasegawa, T; Lai, SP; Qiu, KP; Arzoumanian, D; Bourke, TL; Byun, D; Chen, HRV; Chen, WP; Chen, MK; Chen, ZW; Cho, JY; Choi, M; Choi, Y; Choi, Y; Chrysostomou, A; Chung, EJ; Dai, SP; Debattista, V; Di Francesco, J; Diep, PN; Doi, Y; Duan, HY; Duan, Y; Eswaraiah, C; Fanciullo, L; Fiege, J; Fissel, LM; Franzmann, E; Friberg, P; Friesen, R; Fuller, G; Furuya, R; Gledhill, T; Graves, S; Greaves, J; Griffin, M; Gu, QL; Han, IL; Hayashi, S; Hoang, T; Houde, M; Hull, CLH; Inoue, T; Inutsuka, S; Iwasaki, K; Jeong, I; Johnstone, D; Könyves, V; Kang, JH; Kang, MJ; Kataoka, A; Kawabata, K; Kemper, F; Kim, J; Kim, S; Kim, G; Kim, KH; Kim, MR; Kim, KT; Kim, H; Kirchschlager, F; Kobayashi, MIN; Koch, PM; Kusune, T; Kwon, J; Lacaille, K; Law, CY; Lee, CW; Lee, HYS; Lee, YH; Lee, CF; Lee, JE; Lee, SS; Li, DL; Li, D; Li, GX; Li, HB; Lin, SJ; Liu, HL; Liu, T; Liu, SY; Liu, JH; Longmore, S; Lu, X; Lyo, AR; Mairs, S; Matsumura, M; Matthews, B; Moriarty-Schieven, G; Nagata, T; Nakamura, F; Nakanishi, H; Ngoc, NB; Ohashi, N; Onaka, T; Park, G; Parsons, H; Peretto, N; Priestley, F; Pyo, TS; Qian, L; Rao, RMS; Rawlings, J; Rawlings, M; Retter, B; Richer, J; Rigby, A; Sadavoy, S; Saito, H; Savini, G; Seta, M; Shimajiri, Y; Shinnaga, H; Tahani, M; Tamura, M; Tang, YW; Tang, XD; Tomisaka, K; Tram, L; Tsukamoto, Y; Viti, S; Wang, HC; Wu, JT; Xie, JJ; Yang, MZ; Yen, HW; Yoo, H; Yuan, JH; Yun, HS; Zenko, T; Zhang, GY; Zhang, YP; Zhang, CP; Zhou, JJ; Zhu, L; de Looze, I; André, P; Dowell, CD; Eden, D; Eyres, S; Falle, S; Le Gouellec, VJM; Poidevin, F; Robitaille, JF; van Loo, S

ASTROPHYSICAL JOURNAL Vol. 946 ( 2 ) 2023.4

An Origin of Narrow Extended Structure in the Interstellar Medium: An Interstellar Contrail Created by a Fast-moving Massive Object

Kitajima, K; Inutsuka, SI

ASTROPHYSICAL JOURNAL Vol. 945 ( 1 ) 2023.3

Planetesimal Formation by the Gravitational Instability of Dust Ring Structures

Takahashi, SZ; Kokubo, E; Inutsuka, S

ASTROPHYSICAL JOURNAL Vol. 945 ( 2 ) 2023.3

Evolution of the Angular Momentum of Molecular Cloud Cores Formed from Filament Fragmentation International coauthorship

Misugi, Y; Inutsuka, S; Arzoumanian, D

ASTROPHYSICAL JOURNAL Vol. 943 ( 2 ) 2023.2

JCMT BISTRO Observations: Magnetic Field Morphology of Bubbles Associated with NGC 6334

Tahani, M; Bastien, P; Furuya, RS; Pattle, K; Johnstone, D; Arzoumanian, D; Doi, Y; Hasegawa, T; Inutsuka, S; Coudé, S; Fissel, L; Chen, MCY; Poidevin, F; Sadavoy, S; Friesen, R; Koch, PM; Di Francesco, J; Moriarty-Schieven, GH; Chen, ZW; Chung, EJ; Eswaraiah, C; Fanciullo, L; Gledhill, T; Le Gouellec, VJM; Hoang, T; Hwang, J; Kang, JH; Kim, KH; Kirchschlager, F; Kwon, W; Lee, CW; Liu, HL; Onaka, T; Rawlings, MG; Soam, A; Tamura, M; Tang, XD; Tomisaka, K; Whitworth, AP; Kwon, J; Hoang, TD; Redman, M; Berry, D; Ching, TC; Wang, JW; Lai, SP; Qiu, KP; Ward-Thompson, D; Houde, M; Byun, D; Chen, HRV; Chen, WP; Cho, JY; Choi, M; Choi, Y; Chrysostomou, A; Diep, PN; Duan, HY; Fiege, J; Franzmann, E; Friberg, P; Fuller, G; Graves, SF; Greaves, JS; Griffin, MJ; Gu, QL; Han, IL; Hatchell, J; Hayashi, SS; Hull, CLH; Inoue, T; Iwasaki, K; Jeong, I; Kanamori, Y; Kang, MJ; Kang, SJ; Kataoka, A; Kawabata, KS; Kemper, F; Kim, G; Kim, J; Kim, KT; Kim, MR; Kim, S; Kirk, JM; Kobayashi, MIN; Konyves, V; Kusune, T; Lacaille, K; Law, CY; Lee, CF; Lee, HYS; Lee, JE; Lee, SS; Lee, YH; Li, DL; Li, D; Li, HB; Liu, JH; Liu, SY; Liu, T; de Looze, I; Lyo, AR; Mairs, S; Matsumura, M; Matthews, BC; Nagata, T; Nakamura, F; Nakanishi, H; Ohashi, N; Park, G; Parsons, H; Peretto, N; Pyo, TS; Qian, L; Rao, RMS; Retter, B; Richer, J; Rigby, A; Saito, H; Savini, G; Scaife, AMM; Seta, M; Shimajiri, Y; Shinnaga, H; Tang, YW; Tsukamoto, Y; Viti, S; Wang, HC; Yen, HW; Yoo, H; Yuan, JH; Yun, HS; Zenko, T; Zhang, CP; Zhang, GY; Zhang, YP; Zhou, JJ; Zhu, L; André, P; Dowell, CD; Eyres, SPS; Falle, S; van Loo, S; Robitaille, JF

ASTROPHYSICAL JOURNAL Vol. 944 ( 2 ) 2023.2

The JCMT BISTRO-2 Survey: Magnetic Fields of the Massive DR21 Filament International coauthorship

Ching, TC; Qiu, K; Li, D; Ren, ZY; Lai, SP; Berry, D; Pattle, K; Furuya, R; Ward-Thompson, D; Johnstone, D; Koch, PM; Lee, CW; Hoang, T; Hasegawa, T; Kwon, W; Bastien, P; Eswaraiah, C; Wang, JW; Kim, KH; Hwang, J; Soam, A; Lyo, AR; Liu, JH; Le Gouellec, VJM; Arzoumanian, D; Whitworth, A; Di Francesco, J; Poidevin, F; Liu, T; Coudé, S; Tahani, M; Liu, HL; Onaka, T; Li, DL; Tamura, M; Chen, ZW; Tang, XD; Kirchschlager, F; Bourke, TL; Byun, DY; Chen, MK; Chen, HRV; Chen, WP; Cho, J; Choi, Y; Choi, Y; Choi, M; Chrysostomou, A; Chung, EJ; Dai, YS; Diep, PN; Doi, Y; Duan, Y; Duan, HY; Eden, D; Fanciullo, L; Fiege, J; Fissel, LM; Franzmann, E; Friberg, P; Friesen, R; Fuller, G; Gledhill, T; Graves, S; Greaves, J; Griffin, M; Gu, QL; Han, I; Hayashi, S; Houde, M; Hull, CLH; Inoue, T; Inutsuka, SI; Iwasaki, K; Jeong, IG; Könyves, V; Kang, JH; Kang, M; Karoly, J; Kataoka, A; Kawabata, K; Kemper, F; Kim, J; Kim, MR; Kim, S; Kim, H; Kim, KT; Kim, G; Kirk, J; Kobayashi, MIN; Kusune, T; Kwon, J; Lacaille, K; Law, CY; Lee, SS; Lee, H; Lee, JE; Lee, CF; Lee, YH; Li, GX; Li, HB; Lin, SJ; Liu, SY; Lu, X; Mairs, S; Matsumura, M; Matthews, B; Moriarty-Schieven, G; Nagata, T; Nakamura, F; Nakanishi, H; Ngoc, NB; Ohashi, N; Park, G; Parsons, H; Peretto, N; Priestley, F; Pyo, TS; Qian, L; Rao, R; Rawlings, M; Rawlings, J; Retter, B; Richer, J; Rigby, A; Sadavoy, S; Saito, H; Savini, G; Seta, M; Shimajiri, Y; Shinnaga, H; Tang, YW; Tomisaka, K; Tram, LN; Tsukamoto, Y; Viti, S; Wang, HC; Wu, JT; Xie, JJ; Yang, MZ; Yen, HW; Yoo, H; Yuan, JH; Yun, HS; Zenko, T; Zhang, CP; Zhang, YP; Zhang, GY; Zhou, JJ; Zhu, L; De Looze, I; André, P; Dowell, CD; Eyres, S; Falle, S; Robitaille, JF; Van Loo, S

ASTROPHYSICAL JOURNAL Vol. 941 ( 2 ) 2022.12

The JCMT BISTRO Survey: A Spiral Magnetic Field in a Hub-filament Structure, Monoceros R2 Reviewed International coauthorship

Hwang, J; Kim, J; Pattle, K; Lee, CW; Koch, PM; Johnstone, D; Tomisaka, K; Whitworth, A; Furuya, RS; Kang, JH; Lyo, AR; Chung, EJ; Arzoumanian, D; Park, G; Kwon, W; Kim, S; Tamura, M; Kwon, J; Soam, A; Han, I; Hoang, T; Kim, KH; Onaka, T; Eswaraiah, C; Ward-Thompson, D; Liu, HL; Tang, XD; Chen, WP; Matsumura, M; Hoang, TD; Chen, ZW; Le Gouellec, VJM; Kirchschlager, F; Poidevin, F; Bastien, P; Qiu, K; Hasegawa, T; Lai, SP; Byun, DY; Cho, J; Choi, M; Choi, Y; Choi, Y; Jeong, IG; Kang, M; Kim, H; Kim, KT; Lee, JE; Lee, SS; Lee, YH; Lee, H; Kim, MR; Yoo, H; Yun, HS; Chen, M; Di Francesco, J; Fiege, J; Fissel, LM; Franzmann, E; Houde, M; Lacaille, K; Matthews, B; Sadavoy, S; Moriarty-Schieven, G; Tahani, M; Ching, TC; Dai, YS; Duan, Y; Gu, QL; Law, CY; Li, DLL; Li, D; Li, GX; Li, HB; Liu, T; Lu, X; Qian, L; Wang, HC; Wu, JT; Xie, JJ; Yuan, JH; Zhang, CP; Zhang, GY; Zhang, YP; Zhou, J; Zhu, L; Berry, D; Friberg, P; Graves, S; Liu, JH; Mairs, S; Parsons, H; Rawlings, M; Doi, Y; Hayashi, S; Hull, CLH; Inoue, T; Inutsuka, S; Iwasaki, K; Kataoka, A; Kawabata, K; Kim, G; Kobayashi, MIN; Nagata, T; Nakamura, F; Nakanishi, H; Pyo, TS; Saito, H; Seta, M; Shimajiri, Y; Shinnaga, H; Tsukamoto, Y; Zenko, T; Chen, HRV; Duan, HY; Fanciullo, L; Kemper, F; Lee, CF; Lin, SJ; Liu, SY; Ohashi, N; Rao, R; Tang, YW; Wang, JW; Yang, MZ; Yen, HW; Bourke, TL; Chrysostomou, A; Debattista, V; Eden, D; Eyres, S; Falle, S; Fuller, G; Gledhill, T; Greaves, J; Griffin, M; Hatchell, J; Karoly, J; Kirk, J; Könyves, V; Longmore, S; van Loo, S; de Looze, I; Peretto, N; Priestley, F; Rawlings, J; Retter, B; Richer, J; Rigby, A; Savini, G; Scaife, A; Viti, S; Diep, PN; Ngoc, NB; Tram, LN; André, P; Coudé, S; Dowell, CD; Friesen, R; Robitaille, JF

ASTROPHYSICAL JOURNAL Vol. 941 ( 1 ) 2022.12

Nonlinear Outcome of Coagulation Instability in Protoplanetary Disks. II. Dust-ring Formation Mediated by Backreaction and Fragmentation

Tominaga, RT; Tanaka, H; Kobayashi, H; Inutsuka, S

ASTROPHYSICAL JOURNAL Vol. 940 ( 2 ) 2022.12

Nonlinear Outcome of Coagulation Instability in Protoplanetary Disks. I. First Numerical Study of Accelerated Dust Growth and Dust Concentration at Outer Radii Reviewed International coauthorship

Tominaga, RT; Kobayashi, H; Inutsuka, S

ASTROPHYSICAL JOURNAL Vol. 937 ( 1 ) 2022.9

On high-order numerical schemes for viscous relativistic hydrodynamics through the Kelvin-Helmholtz instability Reviewed International coauthorship

Townsend, JF; Inutsuka, S; Könözsy, L; Jenkins, KW

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY Vol. 515 ( 1 ) page： 451 - 472 2022.7

Effects of Magnetic Field Orientations in Dense Cores on Gas Kinematics in Protostellar Envelopes Reviewed International coauthorship

Gupta, A; Yen, HW; Koch, P; Bastien, P; Bourke, TL; Chung, EJ; Hasegawa, T; Hull, CLH; Inutsuka, S; Kwon, J; Kwon, W; Lai, SP; Lee, CW; Lee, CF; Pattle, K; Qiu, KP; Tahani, M; Tamura, M; Ward-Thompson, D

ASTROPHYSICAL JOURNAL Vol. 930 ( 1 ) 2022.5

3D magnetic-field morphology of the Perseus molecular cloud Reviewed International coauthorship

Tahani, M; Lupypciw, W; Glover, J; Plume, R; West, JL; Kothes, R; Inutsuka, S; Lee, MY; Robishaw, T; Knee, LBG; Brown, JC; Doi, Y; Grenier, IA; Haverkorn, M

ASTRONOMY & ASTROPHYSICS Vol. 660 2022.4

Velocity structure of the 50 pc long NGC 6334 filamentary cloud Hints of multiple compressions and their impact on the cloud properties Reviewed International coauthorship

Arzoumanian, D; Russeil, D; Zavagno, A; Chen, MCY; André, P; Inutsuka, SI; Misugi, Y; Sanchez-Monge, A; Schilke, P; Men'shchikov, A; Kohno, M

ASTRONOMY & ASTROPHYSICS Vol. 660 2022.4

Orion A's complete 3D magnetic field morphology Reviewed International coauthorship

Tahani, M; Glover, J; Lupypciw, W; West, JL; Kothes, R; Plume, R; Inutsuka, S; Lee, MY; Grenier, IA; Knee, LBG; Brown, JC; Doi, Y; Robishaw, T; Haverkorn, M

ASTRONOMY & ASTROPHYSICS Vol. 660 2022.4

Filament coalescence and hub structure in Mon R2 Implications for massive star and cluster formation

Kumar, MSN; Arzoumanian, D; Men'shchikov, A; Palmeirim, P; Matsumura, M; Inutsuka, S

ASTRONOMY & ASTROPHYSICS Vol. 658 2022.2

B-fields in Star-forming Region Observations (BISTRO): Magnetic Fields in the Filamentary Structures of Serpens Main

Kwon, W; Pattle, K; Sadavoy, S; Hull, CLH; Johnstone, D; Ward-Thompson, D; Di Francesco, J; Koch, PM; Furuya, R; Doi, Y; Le Gouellec, VJM; Hwang, J; Lyo, AR; Soam, A; Tang, XD; Hoang, T; Kirchschlager, F; Eswaraiah, C; Fanciullo, L; Kim, KH; Onaka, T; Könyves, V; Kang, JH; Lee, CW; Tamura, M; Bastien, P; Hasegawa, T; Lai, SP; Qiu, KP; Berry, D; Arzoumanian, D; Bourke, TL; Byun, DY; Chen, WP; Chen, HRV; Chen, MK; Chen, ZW; Ching, TC; Cho, J; Choi, Y; Choi, M; Chrysostomou, A; Chung, EJ; Coudé, S; Dai, S; Diep, PN; Duan, Y; Duan, HY; Eden, D; Fiege, J; Fissel, LM; Franzmann, E; Friberg, P; Friesen, R; Fuller, G; Gledhill, T; Graves, S; Greaves, J; Griffin, M; Gu, QL; Han, I; Hatchell, J; Hayashi, S; Houde, M; Inoue, T; Inutsuka, S; Iwasaki, K; Jeong, IG; Kang, MJ; Karoly, J; Kataoka, A; Kawabata, K; Kemper, F; Kim, KT; Kim, G; Kim, MR; Kim, S; Kim, J; Kirk, J; Kobayashi, MIN; Kusune, T; Kwon, J; Lacaille, K; Law, CY; Lee, CF; Lee, YH; Lee, H; Lee, JE; Lee, SS; Li, DL; Li, D; Li, HB; Lin, SJ; Liu, SY; Liu, HL; Liu, JH; Liu, T; Lu, X; Mairs, S; Matsumura, M; Matthews, B; Moriarty-Schieven, G; Nagata, T; Nakamura, F; Nakanishi, H; Ngoc, NB; Ohashi, N; Park, G; Parsons, H; Peretto, N; Priestley, F; Pyo, TS; Qian, L; Rao, R; Rawlings, J; Rawlings, MG; Retter, B; Richer, J; Rigby, A; Saito, H; Savini, G; Seta, M; Shimajiri, Y; Shinnaga, H; Tahani, M; Tang, YW; Tomisaka, K; Tram, L; Tsukamoto, Y; Viti, S; Wang, HC; Wang, JW; Whitworth, A; Wu, JT; Xie, JJ; Yen, HW; Yoo, H; Yuan, J; Yun, HS; Zenko, T; Zhang, YP; Zhang, CP; Zhang, GY; Zhou, JJ; Zhu, L; de Looze, I; André, P; Dowell, CD; Eyres, S; Falle, S; Robitaille, JF; van Loo, S

ASTROPHYSICAL JOURNAL Vol. 926 ( 2 ) 2022.2

The Effects of Cosmic-Ray Diffusion and Radiative Cooling on the Galactic Wind of the Milky Way

Shimoda, J; Inutsuka, S

ASTROPHYSICAL JOURNAL Vol. 926 ( 1 ) 2022.2

Coagulation Instability in Protoplanetary Disks: A Novel Mechanism Connecting Collisional Growth and Hydrodynamical Clumping of Dust Particles

Tominaga, RT; Inutsuka, S; Kobayashi, H

ASTROPHYSICAL JOURNAL Vol. 923 ( 1 ) 2021.12

The JCMT BISTRO Survey: Evidence for Pinched Magnetic Fields in Quiescent Filaments of NGC 1333

Doi, Y; Tomisaka, K; Hasegawa, T; Coudé, S; Arzoumanian, D; Bastien, P; Matsumura, M; Tahani, M; Sadavoy, S; Hull, CLH; Johnstone, D; Di Francesco, J; Shimajiri, Y; Furuya, RS; Kwon, J; Tamura, M; Ward-Thompson, D; Le Gouellec, VJM; Hoang, T; Kirchschlager, F; Hwang, J; Eswaraiah, C; Koch, PM; Whitworth, AP; Pattle, K; Kwon, W; Kang, J; Inutsuka, S; Bourke, TL; Tang, XD; Fanciullo, L; Lee, CW; Liu, HL; Lyo, AR; Qiu, KP; Lai, SP

ASTROPHYSICAL JOURNAL LETTERS Vol. 923 ( 1 ) 2021.12

Dispersal of protoplanetary discs by the combination of magnetically driven and photoevaporative winds (vol 492, pg 3849, 2020)

Kunitomo Masanobu, Suzuki Takeru K., Inutsuka Shu-ichiro

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY Vol. 508 ( 2 ) page： 2492 - 2492 2021.12

Dispersal of protoplanetary discs by the combination of magnetically driven and photoevaporative winds (vol 492, pg 3849, 2020)

Kunitomo Masanobu, Suzuki Takeru K., Inutsuka Shu-ichiro

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY Vol. 508 ( 2 ) page： 2492 - 2492 2021.10

"Ashfall" Induced by Molecular Outflow in Protostar Evolution

Tsukamoto, Y; Machida, MN; Inutsuka, S

ASTROPHYSICAL JOURNAL LETTERS Vol. 920 ( 2 ) 2021.10

The JCMT Transient Survey: Four-year Summary of Monitoring the Submillimeter Variability of Protostars

Lee, YH; Johnstone, D; Lee, JE; Herczeg, G; Mairs, S; Contreras-Peña, C; Hatchell, J; Naylor, T; Bell, GS; Bourke, TL; Broughton, C; Francis, L; Gupta, A; Harsono, D; Liu, SY; Park, G; Plovie, S; Moriarty-Schieven, GH; Scholz, A; Sharma, T; Teixeira, PS; Wang, YT; Aikawa, Y; Bower, GC; Chen, HRV; Bae, J; Baek, G; Chapman, S; Chen, WP; Du, FJ; Dutta, S; Forbrich, J; Guo, Z; Inutsuka, S; Kang, M; Kirk, H; Kuan, YJ; Kwon, W; Lai, SP; Lalchand, B; Lane, JMM; Lee, CF; Liu, T; Morata, O; Pearson, S; Pon, A; Sahu, D; Shang, H; Stamatellos, D; Tang, SY; Xu, ZY; Yoo, H; Rawlings, JMC

ASTROPHYSICAL JOURNAL Vol. 920 ( 2 ) 2021.10

SPH simulations for shape deformation of rubble-pile asteroids through spinup: The challenge for making top-shaped asteroids Ryugu and Bennu

Sugiura, K; Kobayashi, H; Watanabe, S; Genda, H; Hyodo, R; Inutsuka, S

ICARUS Vol. 365 2021.9

Associated Molecular and Atomic Clouds with X-Ray Shell of Superbubble 30 Doradus C in the LMC

Yamane, Y; Sano, H; Filipovic, MD; Tokuda, K; Fujii, K; Babazaki, Y; Mitsuishi, I; Inoue, T; Aharonian, F; Inaba, T; Inutsuka, S; Maxted, N; Mizuno, N; Onishi, T; Rowell, G; Tsuge, K; Voisin, F; Yoshiike, S; Fukuda, T; Kawamura, A; Bamba, A; Tachihara, K; Fukui, Y

ASTROPHYSICAL JOURNAL Vol. 918 ( 1 ) 2021.9

The JCMT BISTRO Survey: An 850/450 μm Polarization Study of NGC 2071IR in Orion B

Lyo, AR; Kim, J; Sadavoy, S; Johnstone, D; Berry, D; Pattle, K; Kwon, W; Bastien, P; Onaka, T; Di Francesco, J; Kang, JH; Furuya, R; Hull, CLH; Tamura, M; Koch, PM; Ward-Thompson, D; Hasegawa, T; Hoang, T; Arzoumanian, D; Lee, CW; Lee, CF; Byun, DY; Kirchschlager, F; Doi, Y; Kim, KT; Hwang, J; Diep, PN; Fanciullo, L; Lee, SS; Park, G; Yoo, H; Chung, EJ; Whitworth, A; Mairs, S; Soam, A; Liu, T; Tang, XD; Coudé, S; André, P; Bourke, TL; Chen, HRV; Chen, ZW; Chen, WP; Chen, MK; Ching, TC; Cho, J; Choi, M; Choi, Y; Chrysostomou, A; Dai, S; Dowell, CD; Duan, HY; Duan, Y; Eden, D; Eswaraiah, C; Eyres, S; Fiege, J; Fissel, LM; Franzmann, E; Friberg, P; Friesen, R; Fuller, G; Gledhill, T; Graves, S; Greaves, J; Griffin, M; Gu, QL; Han, I; Hatchell, J; Hayashi, S; Houde, M; Inoue, T; Inutsuka, S; Iwasaki, K; Jeong, IG; Kang, MJ; Kataoka, A; Kawabata, K; Kemper, F; Kim, G; Kim, MR; Kim, S; Kim, KH; Kirk, J; Kobayashi, MIN; Könyves, V; Kusune, T; Kwon, J; Lacaille, K; Lai, SP; Law, CY; Lee, JE; Lee, YH; Lee, H; Li, DL; Li, D; Li, HB; Liu, HL; Liu, JH; Liu, SY; Lu, X; Matsumura, M; Matthews, B; Moriarty-Schieven, G; Nagata, T; Nakamura, F; Nakanishi, H; Ngoc, NB; Ohashi, N; Parsons, H; Peretto, N; Priestley, F; Pyo, TS; Qian, L; Qiu, K; Rao, R; Rawlings, J; Rawlings, MG; Retter, B; Richer, J; Rigby, A; Saito, H; Savini, G; Scaife, A; Seta, M; Shimajiri, Y; Shinnaga, H; Tahani, M; Tang, YW; Tomisaka, K; Tram, LN; Tsukamoto, Y; Viti, S; Wang, JW; Wang, HC; Xie, JJ; Yen, HW; Yuan, JH; Yun, HS; Zenko, T; Zhang, GY; Zhang, CP; Zhang, YP; Zhou, JJ; Zhu, L; de Looze, I; Dowell, CD; Falle, S; Robitaille, JF; van Loo, S

ASTROPHYSICAL JOURNAL Vol. 918 ( 2 ) 2021.9

Classification of Filament Formation Mechanisms in Magnetized Molecular Clouds

Abe, D; Inoue, T; Inutsuka, S; Matsumoto, T

ASTROPHYSICAL JOURNAL Vol. 916 ( 2 ) 2021.8

Conditions for Justifying Single-fluid Approximation for Charged and Neutral Dust Fluids and a Smoothed Particle Magnetohydrodynamics Method for Dust-Gas Mixture

Tsukamoto, Y; Machida, MN; Inutsuka, S

ASTROPHYSICAL JOURNAL Vol. 913 ( 2 ) 2021.6

Two-component Magnetic Field along the Line of Sight to the Perseus Molecular Cloud: Contribution of the Foreground Taurus Molecular Cloud

Doi, Y; Hasegawa, T; Bastien, P; Tahani, M; Arzoumanian, D; Coudé, S; Matsumura, M; Sadavoy, S; Hull, CLH; Shimajiri, Y; Furuya, RS; Johnstone, D; Plume, R; Inutsuka, S; Kwon, J; Tamura, M

ASTROPHYSICAL JOURNAL Vol. 914 ( 2 ) 2021.6

OMC-1 dust polarization in ALMA Band 7: diagnosing grain alignment mechanisms in the vicinity of Orion Source I

Pattle Kate, Lai Shih-Ping, Wright Melvyn, Coude Simon, Plambeck Richard, Thiem Hoang, Tang Ya-Wen, Bastien Pierre, Eswaraiah Chakali, Furuya Ray S., Hwang Jihye, Inutsuka Shu-ichiro, Kim Kee-Tae, Kirchschlager Florian, Kwon Woojin, Lee Chang Won, Liu Sheng-Yuan, Lyo Aran, Ohashi Nagayoshi, Rawlings Mark G., Tahani Mehrnoosh, Tamura Motohide, Soam Archana, Wang Jia-Wei, Ward-Thompson Derek

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY Vol. 503 ( 3 ) page： 3414 - 3433 2021.5

The JCMT BISTRO Survey: Revealing the Diverse Magnetic Field Morphologies in Taurus Dense Cores with Sensitive Submillimeter Polarimetry

Chakali, E; Li, D; Furuya, RS; Hasegawa, T; Ward-Thompson, D; Qiu, KP; Ohashi, N; Pattle, K; Sadavoy, S; Hull, CLH; Berry, D; Doi, Y; Ching, TC; Lai, SP; Wang, JW; Koch, PM; Kwon, J; Kwon, W; Bastien, P; Arzoumanian, D; Coudé, S; Soam, A; Fanciullo, L; Yen, HW; Liu, JH; Hoang, T; Chen, WP; Shimajiri, Y; Liu, T; Chen, ZW; Li, HB; Lyo, AR; Hwang, J; Johnstone, D; Rao, R; Ngoc, NB; Diep, PN; Mairs, S; Parsons, H; Tamura, M; Tahani, M; Chen, HRV; Nakamura, F; Shinnaga, H; Tang, YW; Cho, J; Lee, CW; Inutsuka, SI; Inoue, T; Iwasaki, K; Qian, L; Xie, JJ; Li, DL; Liu, HL; Zhang, CP; Chen, MK; Zhang, GY; Zhu, L; Zhou, JJ; André, P; Liu, SY; Yuan, JH; Lu, X; Peretto, N; Bourke, TL; Byun, DY; Dai, S; Duan, Y; Duan, HY; Eden, D; Matthews, B; Fiege, J; Fissel, LM; Kim, KT; Lee, CF; Kim, J; Pyo, TS; Choi, Y; Choi, M; Chrysostomou, A; Chung, EJ; Tram, L; Franzmann, E; Friberg, P; Friesen, R; Fuller, G; Gledhill, T; Graves, S; Greaves, J; Griffin, M; Gu, QL; Han, I; Hatchell, J; Hayashi, S; Houde, M; Kawabata, K; Jeong, IG; Kang, JH; Kang, SJ; Kang, M; Kataoka, A; Kemper, F; Rawlings, M; Rawlings, J; Retter, B; Richer, J; Rigby, A; Saito, H; Savini, G; Scaife, A; Seta, M; Kim, G; Kim, KH; Kim, MR; Kirchschlager, F; Kirk, J; Kobayashi, MIN; Konyves, V; Kusune, T; Lacaille, K; Law, CY; Lee, SS; Lee, YH; Matsumura, M; Moriarty-Schieven, G; Nagata, T; Nakanishi, H; Onaka, T; Park, G; Tang, XD; Tomisaka, K; Tsukamoto, Y; Viti, S; Wang, HC; Whitworth, A; Yoo, H; Yun, HS; Zenko, T; Zhang, YP; de Looze, I; Dowell, CD; Eyres, S; Falle, S; Robitaille, JF; van Loo, S

ASTROPHYSICAL JOURNAL LETTERS Vol. 912 ( 2 ) 2021.5

The JCMT BISTRO Survey: Magnetic Fields Associated with a Network of Filaments in NGC 1333 (vol 899, 28, 2020)

Doi, Y; Hasegawa, T; Furuya, RS; Coudé, S; Hull, CLH; Arzoumanian, D; Bastien, P; Chen, MCY; Di Francesco, J; Friesen, R; Houde, M; Inutsuka, SI; Mairs, S; Matsumura, M; Onaka, T; Sadavoy, S; Shimajiri, Y; Tahani, M; Tomisaka, K; Eswaraiah, C; Koch, PM; Pattle, K; Lee, CW; Tamura, M; Berry, D; Ching, TC; Hwang, J; Kwon, W; Soam, A; Wang, JW; Lai, SP; Qiu, KP; Ward-Thompson, D; Byun, D; Chen, HRV; Chen, WP; Chen, ZW; Cho, J; Choi, M; Choi, Y; Chrysostomou, A; Chung, EJ; Diep, PN; Duan, HY; Fanciullo, L; Fiege, J; Franzmann, E; Friberg, P; Fuller, G; Gledhill, T; Graves, SF; Greaves, JS; Griffin, MJ; Gu, QL; Han, I; Hatchell, J; Hayashi, SS; Hoang, T; Inoue, T; Iwasaki, K; Jeong, I; Johnstone, D; Kanamori, Y; Kang, JH; Kang, M; Kang, SJ; Kataoka, A; Kawabata, KS; Kemper, F; Kim, G; Kim, J; Kim, KT; Kim, KH; Kim, MR; Kim, S; Kirk, JM; Kobayashi, MIN; Konyves, V; Kusune, T; Kwon, J; Lacaille, K; Law, CY; Lee, CF; Lee, H; Lee, JE; Lee, SS; Lee, YH; Li, DL; Li, D; Li, HB; Liu, HL; Liu, JH; Liu, SY; Liu, T; de Looze, I; Lyo, AR; Matthews, BC; Moriarty-Schieven, GH; Nagata, T; Nakamura, F; Nakanishi, H; Ohashi, N; Park, G; Parsons, H; Peretto, N; Pyo, TS; Qian, L; Rao, RM; Rawlings, MG; Retter, B; Richer, J; Rigby, A; Saito, H; Savini, G; Scaife, AMM; Seta, M; Shinnaga, H; Tang, YW; Tsukamoto, Y; Viti, S; Wang, HC; Whitworth, AP; Yen, HW; Yoo, H; Yuan, JH; Yun, HS; Zenko, T; Zhang, CP; Zhang, GY; Zhang, YP; Zhou, JJ; Zhu, L; André, P; Dowell, CD; Eyres, SPS; Falle, S; van Loo, S; Robitaille, JF

ASTROPHYSICAL JOURNAL Vol. 911 ( 1 ) 2021.4

OMC-1 dust polarization in ALMA Band 7: diagnosing grain alignment mechanisms in the vicinity of Orion Source I

Pattle Kate, Lai Shih-Ping, Wright Melvyn, Coude Simon, Plambeck Richard, Hoang Thiem, Tang Ya-Wen, Bastien Pierre, Eswaraiah Chakali, Furuya Ray S., Hwang Jihye, Inutsuka Shu-ichiro, Kim Kee-Tae, Kirchschlager Florian, Kwon Woojin, Lee Chang Won, Liu Sheng-Yuan, Lyo Aran, Ohashi Nagayoshi, Rawlings Mark G., Tahani Mehrnoosh, Tamura Motohide, Soam Archana, Wang Jia-Wei, Ward-Thompson Derek

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY Vol. 503 ( 3 ) page： 3414 - 3433 2021.3

Dust polarized emission observations of NGC 6334 BISTRO reveals the details of the complex but organized magnetic field structure of the high-mass star-forming hub-filament network Reviewed International coauthorship

Arzoumanian, D; Furuya, RS; Hasegawa, T; Tahani, M; Sadavoy, S; Hull, CLH; Johnstone, D; Koch, PM; Inutsuka, S; Doi, Y; Hoang, T; Onaka, T; Iwasaki, K; Shimajiri, Y; Inoue, T; Peretto, N; André, P; Bastien, P; Berry, D; Chen, HRV; Di Francesco, J; Eswaraiah, C; Fanciullo, L; Fissel, LM; Hwang, J; Kang, JH; Kim, G; Kim, KT; Kirchschlager, F; Kwon, W; Lee, CW; Liu, HL; Lyo, AR; Pattle, K; Soam, A; Tang, X; Whitworth, A; Ching, TC; Coudé, S; Wang, JW; Ward-Thompson, D; Lai, SP; Qiu, K; Bourke, TL; Byun, DY; Chen, M; Chen, Z; Chen, WP; Cho, J; Choi, Y; Choi, M; Chrysostomou, A; Chung, EJ; Dai, S; Diep, PN; Duan, HY; Duan, Y; Eden, D; Fiege, J; Franzmann, E; Friberg, P; Fuller, G; Gledhill, T; Graves, S; Greaves, J; Griffin, M; Gu, Q; Han, I; Hatchell, J; Hayashi, S; Houde, M; Jeong, IG; Kang, M; Kang, SJ; Kataoka, A; Kawabata, K; Kemper, F; Kim, MR; Kim, KH; Kim, J; Kim, S; Kirk, J; Kobayashi, MIN; Könyves, V; Kusune, T; Kwon, J; Lacaille, K; Law, CY; Lee, CF; Lee, YH; Lee, SS; Lee, H; Lee, JE; Li, HB; Li, D; Li, DL; Liu, J; Liu, T; Liu, SY; Lu, X; Mairs, S; Matsumura, M; Matthews, B; Moriarty-Schieven, G; Nagata, T; Nakamura, F; Nakanishi, H; Ngoc, NB; Ohashi, N; Park, G; Parsons, H; Pyo, TS; Qian, L; Rao, R; Rawlings, J; Rawlings, M; Retter, B; Richer, J; Rigby, A; Saito, H; Savini, G; Scaife, A; Seta, M; Shinnaga, H; Tamura, M; Tang, YW; Tomisaka, K; Tram, LN; Tsukamoto, Y; Viti, S; Wang, H; Xie, J; Yen, HW; Yoo, H; Yuan, J; Yun, HS; Zenko, T; Zhang, G; Zhang, CP; Zhang, Y; Zhou, J; Zhu, L; de Looze, I; Dowell, CD; Eyres, S; Falle, S; Friesen, R; Robitaille, JF; van Loo, S

ASTRONOMY & ASTROPHYSICS Vol. 647 2021.3

ALMA Observations of Massive Clouds in the Central Molecular Zone: Ubiquitous Protostellar Outflows Reviewed International coauthorship

Lu, X; Li, SH; Ginsburg, A; Longmore, SN; Kruijssen, JMD; Walker, DL; Feng, SY; Zhang, QZ; Battersby, C; Pillai, T; Mills, EAC; Kauffmann, J; Cheng, Y; Inutsuka, S

ASTROPHYSICAL JOURNAL Vol. 909 ( 2 ) 2021.3

FAUST. II. Discovery of a Secondary Outflow in IRAS 15398-3359: Variability in Outflow Direction during the Earliest Stage of Star Formation? Reviewed International coauthorship

Okoda, Y; Oya, Y; Francis, L; Johnstone, D; Inutsuka, S; Ceccarelli, C; Codella, C; Chandler, C; Sakai, N; Aikawa, Y; Alves, FO; Balucani, N; Bianchi, E; Bouvier, M; Caselli, P; Caux, E; Charnley, S; Choudhury, S; De Simone, M; Dulieu, F; Durán, A; Evans, L; Favre, C; Fedele, D; Feng, SY; Fontani, F; Hama, T; Hanawa, T; Herbst, E; Hirota, T; Imai, M; Isella, A; Jímenez-Serra, I; Kahane, C; Lefloch, B; Loinard, L; López-Sepulcre, A; Maud, LT; Maureira, MJ; Menard, F; Mercimek, S; Miotello, A; Moellenbrock, G; Mori, S; Murillo, NM; Nakatani, R; Nomura, H; Oba, Y; O'Donoghue, R; Ohashi, S; Ospina-Zamudio, J; Pineda, JE; Podio, L; Rimola, A; Sakai, T; Segura-Cox, D; Shirley, Y; Svoboda, B; Taquet, V; Testi, L; Vastel, C; Viti, S; Watanabe, N; Watanabe, Y; Witzel, A; Xue, C; Zhang, YC; Zhao, B; Yamamoto, S

ASTROPHYSICAL JOURNAL Vol. 910 ( 1 ) 2021.3

Observations of Magnetic Fields Surrounding LkHα 101 Taken by the BISTRO Survey with JCMT-POL-2 Reviewed International coauthorship

Ngoc, NB; Diep, PN; Parsons, H; Pattle, K; Hoang, T; Ward-Thompson, D; Tram, LN; Hull, CLH; Tahani, M; Furuya, R; Bastien, P; Qiu, KP; Hasegawa, T; Kwon, W; Doi, Y; Lai, SP; Coudé, S; Berry, D; Ching, TC; Hwang, J; Soam, A; Wang, JW; Arzoumanian, D; Bourke, TL; Byun, D; Chen, HRV; Chen, ZW; Chen, WP; Chen, MK; Cho, J; Choi, Y; Choi, M; Chrysostomou, A; Chung, EJ; Dai, SP; Di Francesco, J; Duan, Y; Duan, HY; Eden, D; Eswaraiah, C; Fanciullo, L; Fiege, J; Fissel, LM; Franzmann, E; Friberg, P; Friesen, R; Fuller, G; Gledhill, T; Graves, S; Greaves, J; Griffin, M; Gu, QL; Han, I; Hatchell, J; Hayashi, S; Houde, M; Inoue, T; Inutsuka, S; Iwasaki, K; Jeong, IG; Johnstone, D; Kang, JH; Kang, SJ; Kang, M; Kataoka, A; Kawabata, K; Kemper, F; Kim, KT; Kim, J; Pyo, TS; Qian, L; Rao, RM; Rawlings, M; Rawlings, J; Retter, B; Richer, J; Rigby, A; Sadavoy, S; Saito, H; Savini, G; Scaife, A; Seta, M; Kim, G; Kim, S; Kim, KH; Kim, MR; Kirchschlager, F; Kirk, J; Kobayashi, MIN; Koch, PM; Konyves, V; Kusune, T; Kwon, J; Lacaille, K; Law, CY; Lee, SS; Lee, YH; Lee, CF; Lee, JE; Lee, H; Lee, CW; Li, D; Li, HB; Li, DL; Liu, HL; Liu, JH; Liu, T; Liu, SY; Lu, X; Lyo, AR; Mairs, S; Matsumura, M; Matthews, B; Moriarty-Schieven, G; Nagata, T; Nakamura, F; Nakanishi, H; Ohashi, N; Onaka, T; Park, G; Peretto, N; Shimajiri, Y; Shinnaga, H; Tamura, M; Tang, YW; Tang, XD; Tomisaka, K; Tsukamoto, Y; Viti, S; Wang, HC; Whitworth, A; Xie, JJ; Yen, HW; Yoo, H; Yuan, JH; Yun, HS; Zenko, T; Zhang, YP; Zhang, CAP; Zhang, GY; Zhou, JJ; Zhu, L; de Looze, I; André, P; Dowell, CD; Eyres, S; Falle, S; Robitaille, JF; van Loo, S

ASTROPHYSICAL JOURNAL Vol. 908 ( 1 ) 2021.2

The JCMT BISTRO Survey: Alignment between Outflows and Magnetic Fields in Dense Cores/Clumps Reviewed International coauthorship

Yen, HW; Koch, PM; Hull, CLH; Ward-Thompson, D; Bastien, P; Hasegawa, T; Kwon, W; Lai, SP; Qiu, KP; Ching, TC; Chung, EJ; Coudé, S; Di Francesco, J; Diep, PN; Doi, Y; Eswaraiah, C; Falle, S; Fuller, G; Furuya, RS; Han, I; Hatchell, J; Houde, M; Inutsuka, SI; Johnstone, D; Kang, JH; Kang, M; Kim, KT; Kirchschlager, F; Kwon, J; Lee, CW; Lee, CF; Liu, HL; Liu, T; Lyo, AR; Ohashi, N; Onaka, T; Pattle, K; Sadavoy, S; Saito, H; Shinnaga, H; Soam, A; Tahani, M; Tamura, M; Tang, YW; Tang, XD; Zhang, CP

ASTROPHYSICAL JOURNAL Vol. 907 ( 1 ) 2021.1

Progress in Star Formation Theory Invited Reviewed Open Access

犬塚修一郎

The Astronomical Herald Vol. 114 page： 109 - 119 2021

Star Formation in The Galactic Disk and The Galactic Center Invited Reviewed International journal Open Access

犬塚修一郎

ASP Conference Series, Vol. 528: New Horizons in Galactic Center Astronomy and Beyond Vol. 528 page： 271 - 280 2021

ALMA CO Observations of the Gamma-Ray Supernova Remnant RX J1713.7-3946: Discovery of Shocked Molecular Cloudlets and Filaments at 0.01 pc Scales Reviewed International coauthorship

Sano, H; Inoue, T; Tokuda, K; Tanaka, T; Yamazaki, R; Inutsuka, S; Aharonian, F; Rowell, G; Filipovic, MD; Yamane, Y; Yoshiike, S; Maxted, N; Uchida, H; Hayakawa, T; Tachihara, K; Uchiyama, Y; Fukui, Y

ASTROPHYSICAL JOURNAL LETTERS Vol. 904 ( 2 ) 2020.12

Bimodal Behavior and Convergence Requirement in Macroscopic Properties of the Multiphase Interstellar Medium Formed by Atomic Converging Flows Reviewed

Kobayashi, MIN; Inoue, T; Inutsuka, S; Tomida, K; Iwasaki, K; Tanaka, KEI

ASTROPHYSICAL JOURNAL Vol. 905 ( 2 ) 2020.12

Formation and evolution of the local interstellar environment: combined constraints from nucleosynthetic and X-ray data Reviewed International coauthorship

Fujimoto, Y; Krumholz, MR; Inutsuka, S; Boss, AP; Nittler, LR

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY Vol. 498 ( 4 ) page： 5532 - 5540 2020.11

Unifying low- and high-mass star formation through density-amplified hubs of filaments The highest mass stars (>100 M⊙) form only in hubs? Reviewed International coauthorship

Kumar, MSN; Palmeirim, P; Arzoumanian, D; Inutsuka, SI

ASTRONOMY & ASTROPHYSICS Vol. 642 2020.10

ALMA CO Observations of Gamma-Ray Supernova Remnant N132D in the Large Magellanic Cloud: Possible Evidence for Shocked Molecular Clouds Illuminated by Cosmic-Ray Protons Reviewed International coauthorship

Sano, H; Plucinsky, PP; Bamba, A; Sharda, P; Filipovic, MD; Law, CJ; Alsaberi, RZE; Yamane, Y; Tokuda, K; Acero, F; Sasaki, M; Vink, J; Inoue, T; Inutsuka, S; Shimoda, J; Tsuge, K; Fujii, K; Voisin, F; Maxted, N; Rowell, G; Onishi, T; Kawamura, A; Mizuno, N; Yamamoto, H; Tachihara, K; Fukui, Y

ASTROPHYSICAL JOURNAL Vol. 902 ( 1 ) 2020.10

Distribution and kinematics of 26Al in the Galactic disc Reviewed International coauthorship

Fujimoto, Y; Krumholz, MR; Inutsuka, S

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY Vol. 497 ( 2 ) page： 2442 - 2454 2020.9

Secular Gravitational Instability of Drifting Dust in Protoplanetary Disks: Formation of Dusty Rings without Significant Gas Substructures Reviewed

Tominaga, RT; Takahashi, SZ; Inutsuka, S

ASTROPHYSICAL JOURNAL Vol. 900 ( 2 ) 2020.9

A Low-velocity Bipolar Outflow from a Deeply Embedded Object in Taurus Revealed by the Atacama Compact Array Reviewed International coauthorship

Fujishiro, K; Tokuda, K; Tachihara, K; Takashima, T; Fukui, Y; Zahorecz, S; Saigo, K; Matsumoto, T; Tomida, K; Machida, MN; Inutsuka, S; André, P; Kawamura, A; Onishi, T

ASTROPHYSICAL JOURNAL LETTERS Vol. 899 ( 1 ) 2020.8

FRagmentation and Evolution of Dense Cores Judged by ALMA (FREJA). I. Overview: Inner ∼1000 au Structures of Prestellar/Protostellar Cores in Taurus Reviewed International coauthorship

Tokuda, K; Fujishiro, K; Tachihara, K; Takashima, T; Fukui, Y; Zahorecz, S; Saigo, K; Matsumoto, T; Tomida, K; Machida, MN; Inutsuka, S; André, P; Kawamura, A; Onishi, T

ASTROPHYSICAL JOURNAL Vol. 899 ( 1 ) 2020.8

The JCMT BISTRO Survey: Magnetic Fields Associated with a Network of Filaments in NGC 1333 Reviewed International coauthorship

Doi, Y; Hasegawa, T; Furuya, RS; Coudé, S; Hull, CLH; Arzoumanian, D; Bastien, P; Chen, MCY; Di Francesco, J; Friesen, R; Houde, M; Inutsuka, SI; Mairs, S; Matsumura, M; Onaka, T; Sadavoy, S; Shimajiri, Y; Tahani, M; Tomisaka, K; Eswaraiah, C; Koch, PM; Pattle, K; Lee, CW; Tamura, M; Berry, D; Ching, TC; Hwang, J; Kwon, W; Soam, A; Wang, JW; Lai, SP; Qiu, K; Ward-Thompson, D; Byun, DY; Chen, HRV; Chen, WP; Chen, ZW; Cho, J; Choi, M; Choi, Y; Chrysostomou, A; Chung, EJ; Diep, PN; Duan, HY; Fanciullo, L; Fiege, J; Franzmann, E; Friberg, P; Fuller, G; Gledhill, T; Graves, SF; Greaves, JS; Griffin, MJ; Gu, QL; Han, I; Hatchell, J; Hayashi, SS; Hoang, T; Inoue, T; Iwasaki, K; Jeong, IG; Johnstone, D; Kanamori, Y; Kang, JH; Kang, M; Kang, SJ; Kataoka, A; Kawabata, KS; Kemper, F; Kim, G; Kim, J; Kim, KT; Kim, KH; Kim, MR; Kim, S; Kirk, JM; Kobayashi, MIN; Konyves, V; Kusune, T; Kwon, J; Lacaille, K; Law, CY; Lee, CF; Lee, H; Lee, JE; Lee, SS; Lee, YH; Li, DL; Li, D; Li, HB; Liu, HL; Liu, J; Liu, SY; Liu, T; de Looze, I; Lyo, AR; Matthews, BC; Moriarty-Schieven, GH; Nagata, T; Nakamura, F; Nakanishi, H; Ohashi, N; Park, G; Parsons, H; Peretto, N; Pyo, TS; Qian, L; Rao, R; Rawlings, MG; Retter, B; Richer, J; Rigby, A; Saito, H; Savini, G; Scaife, AMM; Seta, M; Shinnaga, H; Tang, YW; Tsukamoto, Y; Viti, S; Wang, HC; Whitworth, AP; Yen, HW; Yoo, H; Yuan, JH; Yun, HS; Zenko, T; Zhang, CP; Zhang, GY; Zhang, YP; Zhou, JJ; Zhu, L; André, P; Dowell, CD; Eyres, SPS; Falle, S; van Loo, S; Robitaille, JF

ASTROPHYSICAL JOURNAL Vol. 899 ( 1 ) 2020.8

The Origin of the Stellar Mass Distribution and Multiplicity

Lee, YN; Offner, SSR; Hennebelle, P; André, P; Zinnecker, H; Ballesteros-Paredes, J; Inutsuka, S; Kruijssen, JMD

SPACE SCIENCE REVIEWS Vol. 216 ( 4 ) 2020.6

Early Evolution of Disk, Outflow, and Magnetic Field of Young Stellar Objects: Impact of Dust Model Reviewed

Tsukamoto, Y; Machida, MN; Susa, H; Nomura, H; Inutsuka, S

ASTROPHYSICAL JOURNAL Vol. 896 ( 2 ) 2020.6

The Molecular Cloud Lifecycle International coauthorship

Chevance, M; Kruijssen, JMD; Vazquez-Semadeni, E; Nakamura, F; Klessen, R; Ballesteros-Paredes, J; Inutsuka, S; Adamo, A; Hennebelle, P

SPACE SCIENCE REVIEWS Vol. 216 ( 4 ) 2020.4

Preface Invited Reviewed

Inutsuka S.

Planetary People - The Japanese Society for Planetary Sciences Vol. 29 ( 1 ) page： 3 - 3 2020.3

Dispersal of protoplanetary discs by the combination of magnetically driven and photoevaporative winds Reviewed

Kunitomo, M; Suzuki, TK; Inutsuka, S

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY Vol. 492 ( 3 ) page： 3849 - 3858 2020.3

High-resolution simulations of catastrophic disruptions: Resultant shape distributions Reviewed

Sugiura, K; Kobayashi, H; Inutsuka, S

PLANETARY AND SPACE SCIENCE Vol. 181 2020.2

Possibility of the formation of the extremely elongated shape of 1I/`Oumuamua through a planetesimal collision

Sugiura K., Kobayashi H., Inutsuka S.-i.

Planetary People - The Japanese Society for Planetary Sciences Vol. 28 ( 4 ) page： 323 - 331 2019.12

FOREST Unbiased Galactic Plane Imaging Survey with the Nobeyama 45 m telescope (FUGIN). V. Dense gas mass fraction of molecular gas in the Galactic plane

Torii, K; Fujita, S; Nishimura, A; Tokuda, K; Kohno, M; Tachihara, K; Inutsuka, S; Matsuo, M; Kuriki, M; Tsuda, Y; Minamidani, T; Umemoto, T; Kuno, N; Miyamoto, Y

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN Vol. 71 2019.12

Macroscopic Dynamics of Dust Grains and Formation of Multiple Rings in Protoplanetary Disks Reviewed

Tominaga R. T., Takahashi S. Z., Inutsuka S.-i.

Planetary People - The Japanese Society for Planetary Sciences Vol. 28 ( 3 ) page： 172 - 181 2019.9

Constraints on the formation of brown dwarfs by turbulent compression

Stamer, T; Inutsuka, S

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY Vol. 488 ( 2 ) page： 2644 - 2649 2019.9

An Origin for the Angular Momentum of Molecular Cloud Cores: A Prediction from Filament Fragmentation

Misugi, Y; Inutsuka, S; Arzoumanian, D

ASTROPHYSICAL JOURNAL Vol. 881 ( 1 ) 2019.8

Revised Description of Dust Diffusion and a New Instability Creating Multiple Rings in Protoplanetary Disks

Tominaga, RT; Takahashi, SZ; Inutsuka, S

ASTROPHYSICAL JOURNAL Vol. 881 ( 1 ) 2019.8

Discovery of Shocked Molecular Clouds Associated with the Shell-type Supernova Remnant RX J0046.5-7308 in the Small Magellanic Cloud

Sano, H; Matsumura, H; Yamane, Y; Maggi, P; Fujii, K; Tsuge, K; Tokuda, K; Alsaberi, RZE; Filipovic, MD; Maxted, N; Rowell, G; Uchida, H; Tanaka, T; Muraoka, K; Takekoshi, T; Onishi, T; Kawamura, A; Minamidani, T; Mizuno, N; Yamamoto, H; Tachihara, K; Inoue, T; Inutsuka, S; Voisin, F; Tothill, NFH; Sasaki, M; McClure-Griffiths, NM; Fukui, Y

ASTROPHYSICAL JOURNAL Vol. 881 ( 1 ) 2019.8

A centrally concentrated sub-solar-mass starless core in the Taurus L1495 filamentary complex

Tokuda, K; Tachihara, K; Saigo, K; André, P; Miyamoto, Y; Zahorecz, S; Inutsuka, S; Matsumoto, T; Takashima, T; Machida, MN; Tomida, K; Taniguchi, K; Fukui, Y; Kawamura, A; Tatematsu, K; Kandori, R; Onishi, T

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN Vol. 71 ( 4 ) 2019.8

Collisional elongation: Possible origin of extremely elongated shape of 1I/'Oumuamua

Sugiura, K; Kobayashi, H; Inutsuka, S

ICARUS Vol. 328 page： 14 - 22 2019.8

The Generalized Nonlinear Ohm's Law: How a Strong Electric Field Influences Nonideal MHD Effects in Dusty Protoplanetary Disks

Okuzumi, S; Mori, S; Inutsuka, S

ASTROPHYSICAL JOURNAL Vol. 878 ( 2 ) 2019.6

The JCMT BISTRO Survey: The Magnetic Field of the Barnard 1 Star-forming Region

Coudé, S; Bastien, P; Houde, M; Sadavoy, S; Friesen, R; Di Francesco, J; Johnstone, D; Mairs, S; Hasegawa, T; Kwon, W; Lai, SP; Qiu, KP; Ward-Thompson, D; Berry, D; Chen, MCY; Fiege, J; Franzmann, E; Hatchell, J; Lacaille, K; Matthews, BC; Moriarty-Schieven, GH; Pon, A; André, P; Arzoumanian, D; Aso, Y; Byun, DY; Eswaraiah, C; Chen, HR; Chen, WP; Ching, TC; Cho, J; Choi, M; Chrysostomou, A; Chung, EJ; Doi, Y; Drabek-Maunder, E; Dowell, CD; Eyres, SPS; Falle, S; Friberg, P; Fuller, G; Furuya, RS; Gledhill, T; Graves, SF; Greaves, JS; Griffin, MJ; Gu, QL; Hayashi, SS; Hoang, T; Holland, W; Inoue, T; Inutsuka, S; Iwasaki, K; Jeong, IG; Kanamori, Y; Kataoka, A; Kang, JH; Kang, MJ; Kang, SJ; Kawabata, KS; Kemper, F; Kim, G; Kim, J; Kim, KT; Kim, KH; Kim, MR; Kim, S; Kirk, JM; Kobayashi, MIN; Koch, PM; Kwon, J; Lee, JE; Lee, CW; Lee, SS; Li, DL; Li, D; Li, HB; Liu, HL; Liu, JH; Liu, SY; Liu, T; van Loo, S; Lyo, AR; Matsumura, M; Nagata, T; Nakamura, F; Nakanishi, H; Ohashi, N; Onaka, T; Parsons, H; Pattle, K; Peretto, N; Pyo, TS; Qian, L; Rao, R; Rawlings, MG; Retter, B; Richer, J; Rigby, A; Robitaille, JF; Saito, H; Savini, G; Scaife, AMM; Seta, M; Shinnaga, H; Soam, A; Tamura, M; Tang, YW; Tomisaka, K; Tsukamoto, Y; Wang, HC; Wang, JW; Whitworth, AP; Yen, HW; Yoo, H; Yuan, JH; Zenko, T; Zhang, CP; Zhang, GY; Zhou, JJ; Zhu, L

ASTROPHYSICAL JOURNAL Vol. 877 ( 2 ) 2019.6

The JCMT BISTRO Survey: The Magnetic Field in the Starless Core ρ Ophiuchus C

Liu, JH; Qiu, KP; Berry, D; Di Francesco, J; Bastien, P; Koch, PM; Furuya, RS; Kim, KT; Coudé, S; Lee, CW; Soam, A; Eswaraiah, C; Li, D; Hwang, J; Lyo, AR; Pattle, K; Hasegawa, T; Kwon, W; Lai, SP; Ward-Thompson, D; Ching, TC; Chen, ZW; Gu, QL; Li, DL; Li, HB; Liu, HL; Qian, L; Wang, HC; Yuan, JH; Zhang, CP; Zhang, GY; Zhang, YP; Zhou, JJ; Zhu, L; André, P; Arzoumanian, D; Aso, Y; Byun, DY; Chen, MCY; Chen, HRV; Chen, WP; Cho, J; Choi, M; Chrysostomou, A; Chung, EJ; Doi, Y; Drabek-Maunder, E; Dowell, CD; Eyres, SPS; Falle, S; Fanciullo, L; Fiege, J; Franzmann, E; Friberg, P; Friesen, RK; Fuller, G; Gledhill, T; Graves, SF; Greaves, JS; Griffin, MJ; Han, I; Hatchell, J; Hayashi, SS; Hoang, T; Holland, W; Houde, M; Inoue, T; Inutsuka, S; Iwasaki, K; Jeong, IG; Johnstone, D; Kanamori, Y; Kang, JH; Kang, MJ; Kang, SJ; Kataoka, A; Kawabata, KS; Kemper, F; Kim, G; Kim, J; Kim, KH; Kim, MR; Kim, S; Kirk, JM; Kobayashi, MIN; Kusune, T; Kwon, J; Lacaille, KM; Lee, CF; Lee, JE; Lee, H; Lee, SS; Liu, SY; Liu, T; van Loo, S; Mairs, S; Matsumura, M; Matthews, BC; Moriarty-Schieven, GH; Nagata, T; Nakamura, F; Nakanishi, H; Ohashi, N; Onaka, T; Parker, J; Parsons, H; Pascale, E; Peretto, N; Pon, A; Pyo, TS; Rao, R; Rawlings, MG; Retter, B; Richer, J; Rigby, A; Robitaille, JF; Sadavoy, S; Saito, H; Savini, G; Scaife, AMM; Seta, M; Shinnaga, H; Tamura, M; Tang, YW; Tomisaka, K; Tsukamoto, Y; Wang, JW; Whitworth, AP; Yen, HW; Yoo, H; Zenko, T

ASTROPHYSICAL JOURNAL Vol. 877 ( 1 ) 2019.5

JCMT BISTRO Survey: Magnetic Fields within the Hub-filament Structure in IC 5146

Wang, JW; Lai, SP; Eswaraiah, C; Pattle, K; Di Francesco, J; Johnstone, D; Koch, PM; Liu, T; Tamura, M; Furuya, RS; Onaka, T; Ward-Thompson, D; Soam, A; Kim, KT; Lee, CW; Lee, CF; Mairs, S; Arzoumanian, D; Kim, G; Hoang, T; Hwang, J; Liu, SY; Berry, D; Bastien, P; Hasegawa, T; Kwon, W; Qiu, KP; Andre, P; Aso, Y; Byun, DY; Chen, HR; Chen, MC; Chen, WP; Ching, TC; Cho, J; Choi, M; Chrysostomou, A; Chung, EJ; Coude, S; Doi, YS; Dowell, CD; Drabek-Maunder, E; Duan, HY; Eyres, SPS; Falle, S; Fanciullo, L; Fiege, J; Franzmann, E; Friberg, P; Friesen, RK; Fuller, G; Gledhill, T; Graves, SF; Greaves, JS; Griffin, MJ; Gu, Q; Han, I; Hatchell, J; Hayashi, SS; Holland, W; Houde, M; Inoue, T; Inutsuka, S; Iwasaki, K; Jeong, IG; Kanamori, Y; Kang, J; Kang, MJ; Kang, S; Kataoka, A; Kawabata, KS; Kemper, F; Kim, J; Kim, KH; Kim, MR; Kim, S; Kirk, JM; Kobayashi, MIN; Konyves, V; Kwon, J; Lacaille, KM; Lee, H; Lee, JE; Lee, SS; Lee, YH; Li, DL; Li, D; Li, HB; Liu, HL; Liu, JH; Lyo, AR; Matsumura, M; Matthews, BC; Moriarty-Schieven, GH; Nagata, T; Nakamura, F; Nakanishi, H; Ohashi, N; Park, G; Parsons, H; Pascale, E; Peretto, N; Pon, A; Pyo, TS; Qian, L; Rao, R; Rawlings, MG; Retter, B; Richer, J; Rigby, A; Robitaille, JF; Sadavoy, S; Saito, H; Savini, G; Scaife, AMM; Seta, M; Shinnaga, H; Tang, YW; Tomisaka, K; Tsukamoto, Y; van Loo, S; Wang, HC; Whitworth, AP; Yen, HW; Yoo, H; Yuan, J; Yun, HS; Zenko, T; Zhang, CP; Zhang, GY; Zhang, YP; Zhou, JJ; Zhu, L

ASTROPHYSICAL JOURNAL Vol. 876 ( 1 ) 2019.5

Possible Evidence for Cosmic-Ray Acceleration in the Type Ia SNR RCW 86: Spatial Correlation between TeV Gamma-Rays and Interstellar Atomic Protons

Sano, H; Rowell, G; Reynoso, EM; Jung-Richardt, I; Yamane, Y; Nagaya, T; Yoshiike, S; Hayashi, K; Torii, K; Maxted, N; Mitsuishi, I; Inoue, T; Inutsuka, S; Yamamoto, H; Tachihara, K; Fukui, Y

ASTROPHYSICAL JOURNAL Vol. 876 ( 1 ) 2019.5

The Role of Magnetic Field in Molecular Cloud Formation and Evolution

Hennebelle, P; Inutsuka, S

FRONTIERS IN ASTRONOMY AND SPACE SCIENCES Vol. 6 2019.3

ALMA CO Observations of Supernova Remnant N63A in the Large Magellanic Cloud: Discovery of Dense Molecular Clouds Embedded within Shock-ionized and Photoionized Nebulae

Sano, H; Matsumura, H; Nagaya, T; Yamane, Y; Alsaberi, RZE; Filipovic, MD; Tachihara, K; Fujii, K; Tokuda, K; Tsuge, K; Yoshiike, S; Onishi, T; Kawamura, A; Minamidani, T; Mizuno, N; Yamamoto, H; Inutsuka, S; Inoue, T; Maxted, N; Rowell, G; Sasaki, M; Fukui, Y

ASTROPHYSICAL JOURNAL Vol. 873 ( 1 ) 2019.3

The Early Stage of Molecular Cloud Formation by Compression of Two-phase Atomic Gases

Iwasaki, K; Tomida, K; Inoue, T; Inutsuka, S

ASTROPHYSICAL JOURNAL Vol. 873 ( 1 ) 2019.3

An Origin of Multiple Ring Structure and Hidden Planets in HL Tau: A Unified Picture by Secular Gravitational Instability (vol 152, 184, 2016)

Takahashi, SZ; Inutsuka, S

ASTRONOMICAL JOURNAL Vol. 157 ( 3 ) 2019.3

Two-component Secular Gravitational Instability in a Protoplanetary Disk: A Possible Mechanism for Creating Ring-like Structures (vol 794, 55, 2014)

Takahashi, SZ; Inutsuka, S

ASTROPHYSICAL JOURNAL Vol. 871 ( 1 ) 2019.1

The Exchange of Mass and Angular Momentum in the Impact Event of Ice Giant Planets: Implications for the Origin of Uranus

Kurosaki, K; Inutsuka, S

ASTRONOMICAL JOURNAL Vol. 157 ( 1 ) 2019.1

Radiation-hydrodynamic Simulations of Spherical Protostellar Collapse for Very Low-mass Objects

Stamer, T; Inutsuka, S

ASTROPHYSICAL JOURNAL Vol. 869 ( 2 ) 2018.12

Toward understanding the origin of asteroid geometries Variety in shapes produced by equal-mass impacts

Sugiura, K; Kobayashi, H; Inutsuka, S

ASTRONOMY & ASTROPHYSICS Vol. 620 2018.12

Properties of an accretion disc with a power-law stress-pressure relationship

Shadmehri, M; Khajenabi, F; Dib, S; Inutsuka, S

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY Vol. 481 ( 4 ) page： 5170 - 5179 2018.12

ALMA Reveals a Misaligned Inner Gas Disk inside the Large Cavity of a Transitional Disk

Mayama, S; Akiyama, E; Panic, O; Miley, J; Tsukagoshi, T; Muto, T; Dong, RB; de Leon, J; Mizuki, T; Oh, D; Hashimoto, J; Sai, J; Currie, T; Takami, M; Grady, CA; Hayashi, M; Tamura, M; Inutsuka, S

ASTROPHYSICAL JOURNAL LETTERS Vol. 868 ( 1 ) 2018.11

Does Misalignment between Magnetic Field and Angular Momentum Enhance or Suppress Circumstellar Disk Formation?

Tsukamoto, Y; Okuzumi, S; Iwasaki, K; Machida, MN; Inutsuka, S

ASTROPHYSICAL JOURNAL Vol. 868 ( 1 ) 2018.11

Molecular filament formation and filament-cloud interaction: Hints from Nobeyama 45 m telescope observations

Arzoumanian, D; Shimajiri, Y; Inutsuka, S; Inoue, T; Tachihara, K

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN Vol. 70 ( 5 ) 2018.10

ALMA Observations of Supernova Remnant N49 in the LMC. I. Discovery of CO Clumps Associated with X-Ray and Radio Continuum Shells

Yamane, Y; Sano, H; van Loon, JT; Filipovic, MD; Fujii, K; Tokuda, K; Tsuge, K; Nagaya, T; Yoshiike, S; Grieve, K; Voisin, F; Rowell, G; Indebetouw, R; Lakicevic, M; Temim, T; Staveley-Smith, L; Rho, J; Long, KS; Park, S; Seok, J; Mizuno, N; Kawamura, A; Onishi, T; Inoue, T; Inutsuka, S; Tachihara, K; Fukui, Y

ASTROPHYSICAL JOURNAL Vol. 863 ( 1 ) 2018.8

Warm CO Gas Generated by Possible Turbulent Shocks in a Low-mass Star-forming Dense Core in Taurus

Tokuda, K; Onishi, T; Saigo, K; Matsumoto, T; Inoue, T; Inutsuka, S; Fukui, Y; Machida, MN; Tomida, K; Hosokawa, T; Kawamura, A; Tachihara, K

ASTROPHYSICAL JOURNAL Vol. 862 ( 1 ) 2018.7

Magnetic Fields toward Ophiuchus-B Derived from SCUBA-2 Polarization Measurements

Soam, A; Pattle, K; Ward-Thompson, D; Lee, CW; Sadavoy, S; Koch, PM; Kim, G; Kwon, J; Kwon, W; Arzoumanian, D; Berry, D; Hoang, T; Tamura, M; Lee, SS; Liu, T; Kim, KT; Johnstone, D; Nakamura, F; Lyo, AR; Onaka, T; Kim, J; Furuya, RS; Hasegawa, T; Lai, SP; Bastien, P; Chung, EJ; Kim, S; Parsons, H; Rawlings, MG; Mairs, S; Graves, SF; Robitaille, JF; Liu, HL; Whitworth, AP; Eswaraiah, C; Rao, R; Yoo, H; Houde, M; Kang, JH; Doi, Y; Choi, M; Kang, M; Coudé, S; Li, HB; Matsumura, M; Matthews, BC; Pon, A; Di Francesco, J; Hayashi, SS; Kawabata, KS; Inutsuka, SI; Qiu, K; Franzmann, E; Friberg, P; Greaves, JS; Kirk, JM; Li, D; Shinnaga, H; van Loo, S; Aso, Y; Byun, DY; Chen, HR; Chen, MCY; Chen, WP; Ching, TC; Cho, J; Chrysostomou, A; Drabek-Maunder, E; Eyres, SPS; Fiege, J; Friesen, RK; Fuller, G; Gledhill, T; Griffin, MJ; Gu, QL; Hatchell, J; Holland, W; Inoue, T; Iwasaki, K; Jeong, IG; Kang, SJ; Kemper, F; Kim, KH; Kim, MR; Lacaille, KM; Lee, JE; Li, DL; Liu, JH; Liu, SY; Moriarty-Schieven, GH; Nakanishi, H; Ohashi, N; Peretto, N; Pyo, TS; Qian, L; Retter, B; Richer, J; Rigby, A; Savini, G; Scaife, AMM; Tang, YW; Tomisaka, K; Wang, HC; Wang, JW; Yen, HW; Yuan, JH; Zhang, CP; Zhang, GY; Zhou, JJ; Zhu, L; André, P; Dowell, D; Falle, S; Tsukamoto, Y; Kanamori, Y; Kataoka, A; Kobayashi, MIN; Nagata, T; Saito, H; Seta, M; Hwang, J; Han, I; Lee, H; Zenko, T

ASTROPHYSICAL JOURNAL Vol. 861 ( 1 ) 2018.7

The diverse lives of massive protoplanets in self-gravitating discs

Stamatellos, D; Inutsuka, S

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY Vol. 477 ( 3 ) page： 3110 - 3135 2018.7

A Fast and Accurate Method of Radiation Hydrodynamics Calculation in Spherical Symmetry

Stamer, T; Inutsuka, S

ASTRONOMICAL JOURNAL Vol. 155 ( 6 ) 2018.6

A First Look at BISTRO Observations of the ρ Oph-A core

Kwon, J; Doi, Y; Tamura, M; Matsumura, M; Pattle, K; Berry, D; Sadavoy, S; Matthews, BC; Ward-Thompson, D; Hasegawa, T; Furuya, RS; Pon, A; Di Francesco, J; Arzoumanian, D; Hayashi, SS; Kawabata, KS; Onaka, T; Choi, M; Kang, M; Hoang, T; Lee, CW; Lee, SS; Liu, HL; Liu, T; Inutsuka, S; Eswaraiah, C; Bastien, P; Kwon, W; Lai, SP; Qiu, KP; Coudé, S; Franzmann, E; Friberg, P; Graves, SF; Greaves, JS; Houde, M; Johnstone, D; Kirk, JM; Koch, PM; Di Li, D; Parsons, H; Rao, R; Rawlings, MG; Shinnaga, H; van Loo, S; Aso, Y; Byun, DY; Chen, HR; Chen, MCY; Chen, WP; Ching, TC; Cho, J; Chrysostomou, A; Chung, EJ; Drabek-Maunder, E; Eyres, SPS; Fiege, J; Friesen, RK; Fuller, G; Gledhill, T; Griffin, MJ; Gu, Q; Hatchell, J; Holland, W; Inoue, T; Iwasaki, K; Jeong, IG; Kang, JH; Kang, SJ; Kemper, F; Kim, G; Kim, J; Kim, KT; Kim, KH; Kim, MR; Kim, S; Lacaille, KM; Lee, JE; Li, DL; Li, HB; Liu, JH; Liu, SY; Lyo, AR; Mairs, S; Moriarty-Schieven, GH; Nakamura, F; Nakanishi, H; Ohashi, N; Peretto, N; Pyo, TS; Qian, L; Retter, B; Richer, J; Rigby, A; Robitaille, JF; Savini, G; Scaife, AMM; Soam, A; Tang, YW; Tomisaka, K; Wang, HC; Wang, JW; Whitworth, AP; Yen, HW; Yoo, H; Yuan, JH; Zhang, CP; Zhang, GY; Zhou, JJ; Zhu, L; André, P; Dowell, CD; Falle, S; Tsukamoto, Y; Nakagawa, T; Kanamori, Y; Kataoka, A; Kobayashi, MIN; Nagata, T; Saito, H; Seta, M; Zenko, T

ASTROPHYSICAL JOURNAL Vol. 859 ( 1 ) 2018.5

Differences in the Gas and Dust Distribution in the Transitional Disk of a Sun-like Young Star, PDS 70

Long, ZC; Akiyama, E; Sitko, M; Fernandes, RB; Assani, K; Grady, CA; Cure, M; Danchi, WC; Dong, RB; Fukagawa, M; Hasegawa, Y; Hashimoto, J; Henning, T; Inutsuka, SI; Kraus, S; Kwon, J; Lisse, CM; Liu, HB; Mayama, S; Muto, T; Nakagawa, T; Takami, M; Tamura, M; Currie, T; Wisniewski, JP; Yang, Y

ASTROPHYSICAL JOURNAL Vol. 858 ( 2 ) 2018.5

Star formation induced by cloud-cloud collisions and galactic giant molecular cloud evolution

Kobayashi, MIN; Kobayashi, H; Inutsuka, S; Fukui, Y

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN Vol. 70 2018.5

The formation of massive molecular filaments and massive stars triggered by a magnetohydrodynamic shock wave

Inoue, T; Hennebelle, P; Fukui, Y; Matsumoto, T; Iwasaki, K; Inutsuka, S

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN Vol. 70 2018.5

Two-fluid Magnetohydrodynamics Simulations of Converging of HI Flows in the Interstellar Medium. II. Are Molecular Clouds Generated Directly from Warm Neutral Medium? (vol 704, 161, 2009)

Inoue, T; Inutsuka, S

ASTROPHYSICAL JOURNAL Vol. 855 ( 1 ) 2018.3

A revised condition for self-gravitational fragmentation of protoplanetary discs (vol 458, pg 3597, 2016)

Takahashi, SZ; Tsukamoto, Y; Inutsuka, S

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY Vol. 473 ( 2 ) page： 1718 - 1718 2018.1

Non-linear development of secular gravitational instability in protoplanetary disks

Tominaga, RT; Inutsuka, S; Takahashi, SZ

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN Vol. 70 ( 1 ) 2018.1

The impact of the Hall effect during cloud core collapse: Implications for circumstellar disk evolution

Tsukamoto, Y; Okuzumi, S; Iwasaki, K; Machida, MN; Inutsuka, S

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN Vol. 69 ( 6 ) 2017.12

A Detached Protostellar Disk around a similar to 0.2M(circle dot) Protostar in a Possible Site of a Multiple Star Formation in a Dynamical Environment in Taurus Reviewed

Tokuda Kazuki, Onishi Toshikazu, Saigo Kazuya, Hosokawa Takashi, Matsumoto Tomoaki, Inutsuka Shu-ichiro, Machida Masahiro N., Tomida Kengo, Kunitomo Masanobu, Kawamura Akiko, Fukui Yasuo, Tachihara Kengo

ASTROPHYSICAL JOURNAL Vol. 849 ( 2 ) 2017.11

Electron Heating and Saturation of Self-regulating Magnetorotational Instability in Protoplanetary Disks Reviewed

Mori Shoji, Muranushi Takayuki, Okuzumi Satoshi, Inutsuka Shu-ichiro

ASTROPHYSICAL JOURNAL Vol. 849 ( 2 ) 2017.11

How Do Stars Gain Their Mass? A JCMT/SCUBA-2 Transient Survey of Protostars in Nearby Star-forming Regions Reviewed

Herczeg Gregory J., Johnstone Doug, Mairs Steve, Hatchell Jennifer, Lee Jeong-Eun, Bower Geoffrey C., Chen Huei-Ru Vivien, Aikawa Yuri, Yoo Hyunju, Kang Sung-Ju, Kang Miju, Chen Wen-Ping, Williams Jonathan P., Bae Jaehan, Dunham Michael M., Vorobyov Eduard I., Zhu Zhaohuan, Rao Ramprasad, Kirk Helen, Takahashi Satoko, Morata Oscar, Lacaille Kevin, Lane James, Pon Andy, Scholz Aleks, Samal Manash R., Bell Graham S., Graves Sarah, Lee E'lisa M., Parsons Harriet, He Yuxin, Zhou Jianjun, Kim Mi-Ryang, Chapman Scott, Drabek-Maunder Emily, Chung Eun Jung, Eyres Stewart P. S., Forbrich Jan, Hillenbrand Lynne A., Inutsuka Shu-ichiro, Kim Gwanjeong, Kim Kyoung Hee, Kuan Yi-Jehng, Kwon Woojin, Lai Shih-Ping, Lalchand Bhavana, Lee Chang Won, Lee Chin-Fei, Long Feng, Lyo A-Ran, Qian Lei, Scicluna Peter, Soam Archana, Stamatellos Dimitris, Takakuwa Shigehisa, Tang Ya-Wen, Wang Hongchi, Wang Yiren

ASTROPHYSICAL JOURNAL Vol. 849 ( 1 ) 2017.11

First Results from BISTRO: A SCUBA-2 Polarimeter Survey of the Gould Belt Reviewed

Ward-Thompson Derek, Pattle Kate, Bastien Pierre, Furuya Ray S., Kwon Woojin, Lai Shih-Ping, Qiu Keping, Berry David, Choi Minho, Coude Simon, Di Francesco James, Hoang Thiem, Franzmann Erica, Friberg Per, Graves Sarah F., Greaves Jane S., Houde Martin, Johnstone Doug, Kirk Jason M., Koch Patrick M., Kwon Jungmi, Lee Chang Won, Li Di, Matthews Brenda C., Mottram Joseph C., Parsons Harriet, Pon Andy, Rao Ramprasad, Rawlings Mark, Shinnaga Hiroko, Sadavoy Sarah, van Loo Sven, Aso Yusuke, Byun Do-Young, Eswaraiah Chakali, Chen Huei-Ru, Chen Mike C. -Y., Chen Wen Ping, Ching Tao-Chung, Cho Jungyeon, Chrysostomou Antonio, Chung Eun Jung, Doi Yasuo, Drabek-Maunder Emily, Eyres Stewart P. S., Fiege Jason, Friesen Rachel K., Fuller Gary, Gledhill Tim, Griffin Matt J., Gu Qilao, Hasegawa Tetsuo, Hatchell Jennifer, Hayashi Saeko S., Holland Wayne, Inoue Tsuyoshi, Inutsuka Shu-ichiro, Iwasaki Kazunari, Jeong Il-Gyo, Kang Ji-hyun, Kang Miju, Kang Sung-ju, Kawabata Koji S., Kemper Francisca, Kim Gwanjeong, Kim Jongsoo, Kim Kee-Tae, Kim Kyoung Hee, Kim Mi-Ryang, Kim Shinyoung, Lacaille Kevin M., Lee Jeong-Eun, Lee Sang-Sung, Li Dalei, Li Hua-bai, Liu Hong-Li, Liu Junhao, Liu Sheng-Yuan, Liu Tie, Lyo A-Ran, Mairs Steve, Matsumura Masafumi, Moriarty-Schieven Gerald H., Nakamura Fumitaka, Nakanishi Hiroyuki, Ohashi Nagayoshi, Onaka Takashi, Peretto Nicolas, Pyo Tae-Soo, Qian Lei, Retter Brendan, Richer John, Rigby Andrew, Robitaille Jean-Francois, Savini Giorgio, Scaife Anna M. M., Soam Archana, Tamura Motohide, Tang Ya-Wen, Tomisaka Kohji, Wang Hongchi, Wang Jia-Wei, Whitworth Anthony P., Yen Hsi-Wei, Yoo Hyunju, Yuan Jinghua, Zhang Chuan-Peng, Zhang Guoyin, Zhou Jianjun, Zhu Lei, Andre Philippe, Dowell C. Darren, Falle Sam, Tsukamoto Yusuke

ASTROPHYSICAL JOURNAL Vol. 842 ( 1 ) 2017.6

Planet Formation in AB Aurigae: Imaging of the Inner Gaseous Spirals Observed inside the Dust Cavity Reviewed

Tang Ya-Wen, Guilloteau Stephane, Dutrey Anne, Muto Takayuki, Shen Bo-Ting, Gu Pin-Gao, Inutsuka Shu-ichiro, Momose Munetake, Pietu Vincent, Fukagawa Misato, Chapillon Edwige, Ho Paul T. P., di Folco Emmanuel, Corder Stuartt, Ohashi Nagayoshi, Hashimoto Jun

ASTROPHYSICAL JOURNAL Vol. 840 ( 1 ) 2017.5

Faint warm debris disks around nearby bright stars explored by AKARI and IRSF

Ishihara, D; Takeuchi, N; Kobayashi, H; Nagayama, T; Kaneda, H; Inutsuka, S; Fujiwara, H; Onaka, T

ASTRONOMY & ASTROPHYSICS Vol. 601 2017.5

Circumstellar Disks and Outflows in Turbulent Molecular Cloud Cores: Possible Formation Mechanism for Misaligned Systems Reviewed

Matsumoto Tomoaki, Machida Masahiro N., Inutsuka Shu-ichiro

ASTROPHYSICAL JOURNAL Vol. 839 ( 1 ) 2017.4

An extension of Godunov SPH II: Application to elastic dynamics Reviewed

Sugiura Keisuke, Inutsuka Shu-ichiro

JOURNAL OF COMPUTATIONAL PHYSICS Vol. 333 page： 78 - 103 2017.3

Evolutionary Description of Giant Molecular Cloud Mass Functions on Galactic Disks Reviewed

Kobayashi Masato I. N., Inutsuka Shu-ichiro, Kobayashi Hiroshi, Hasegawa Kenji

ASTROPHYSICAL JOURNAL Vol. 836 ( 2 ) 2017.2

Time Evolution of the Giant Molecular Cloud Mass Functions across Galactic Disks

Kobayashi, MIN; Inutsuka, SI; Kobayashi, H; Hasegawa, K

MULTI-MESSENGER ASTROPHYSICS OF THE GALACTIC CENTRE Vol. 11 ( S322 ) page： 158 - 159 2017

An origin of accelerating star formation a reply to Palla & Stahler (2000) Reviewed International journal

Inutsuka S.

Memorie della Societa Astronomica Italiana - Journal of the Italian Astronomical Society Vol. 88 ( 4 ) page： 554 - 556 2017

Authorship：Lead author,　Last author,　Corresponding author Language：English Publishing type：Research paper (scientific journal) Publisher：Memorie della Societa Astronomica Italiana - Journal of the Italian Astronomical Society

Recent theoretical investigation provides a picture of molecular cloud formation in interacting shells or bubbles in the Galactic disk. Filametary molecular clouds are ubiquitously formed in magnetized dense shells created by expanding bubbles. Star formation starts in dense cores in filamentary molecular cloud, once the mass per unit length of the filament exceeds the critical line-mass. An integrated picture of the cloud formation explains many observational properties such as, cloud-to-cloud velocity dispersions, molecular cloud mass function, dense core mass function, and very low star formation efficiencies in the Galactic disk, as well as the reason for the acceleration of star formation in each star forming region.

Scopus

Time evolution of giant molecular cloud mass functions with cloud-cloud collisions and gas resurrection in various environments International journal

Kobayashi M., Inutsuka S., Kobayashi H., Hasegawa K.

Memorie della Societa Astronomica Italiana - Journal of the Italian Astronomical Society Vol. 88 ( 4 ) page： 741 - 742 2017

Language：English Publishing type：Research paper (scientific journal) Publisher：Memorie della Societa Astronomica Italiana - Journal of the Italian Astronomical Society

We formulate the evolution equation for the giant molecular cloud (GMC) mass functions including self-growth of GMCs through the thermal instability, self-dispersal due to massive stars born in GMCs, cloud-cloud collisions (CCCs), and gas resurrection that replenishes the minimum-mass GMC population. The computed time evolutions obtained from this formulation suggest that the slope of GMC mass function in the mass range < 10355 MO is governed by the ratio of GMC formation timescale to its dispersal timescale, and that the CCC process modifies only the massive end of the mass function. Our results also suggest that most of the dispersed gas contributes to the mass growth of pre-existing GMCs in arm regions whereas less than 60 per cent contributes in inter-arm regions.

Scopus

ALMA observations of massive clouds in the central molecular zone: slim filaments tracing parsec-scale shocks Reviewed International coauthorship International journal Open Access

Yang, K; Lu, X; Zhang, YC; Liu, XC; Ginsburg, A; Liu, HB; Cheng, Y; Feng, SY; Liu, T; Zhang, QZ; Mills, EAC; Walker, DL; Inutsuka, SI; Battersby, C; Longmore, SN; Tang, XD; Kauffmann, J; Gu, QL; Li, SH; Luo, QY; Kruijssen, JMD; Pillai, T; Qiao, HH; Qiu, KP; Shen, ZQ

ASTRONOMY & ASTROPHYSICS Vol. 694 2025.2

The JCMT BISTRO Survey: The Magnetic Fields of the IC 348 Star-forming Region Reviewed International coauthorship International journal Open Access

Choi, Y; Kwon, W; Pattle, K; Arzoumanian, D; Bourke, TL; Hoang, T; Hwang, J; Koch, PM; Sadavoy, S; Bastien, P; Furuya, R; Lai, SP; Qiu, KP; Ward-Thompson, D; Berry, D; Byun, DY; Chen, HRV; Chen, WP; Chen, M; Chen, ZW; Ching, TC; Cho, J; Choi, M; Choi, Y; Coudé, S; Chrysostomou, A; Chung, EJ; Dai, S; Debattista, V; Di Francesco, J; Diep, PN; Doi, Y; Duan, HY; Duan, Y; Eswaraiah, C; Fanciullo, L; Fiege, J; Fissel, LM; Franzmann, E; Friberg, P; Friesen, R; Fuller, G; Gledhill, T; Graves, S; Greaves, J; Griffin, M; Gu, QL; Han, I; Hasegawa, T; Houde, M; Hull, CLH; Inoue, T; Inutsuka, S; Iwasaki, K; Jeong, IG; Johnstone, D; Karoly, J; Könyves, V; Kang, JH; Kang, MJ; Kataoka, A; Kawabata, K; Kemper, F; Kim, J; Kim, S; Kim, G; Kim, KH; Kim, MR; Kim, KT; Kim, H; Kirchschlager, F; Kirk, J; Kobayashi, MIN; Kusune, T; Kwon, J; Lacaille, K; Law, CY; Lee, CW; Lee, H; Lee, CF; Lee, JE; Lee, SS; Li, DL; Li, D; Li, GX; Li, HB; Lin, SJ; Liu, HL; Liu, T; Liu, SY; Liu, JH; Longmore, S; Lu, X; Lyo, AR; Mairs, S; Matsumura, M; Matthews, B; Moriarty-Schieven, G; Nagata, T; Nakamura, F; Nakanishi, H; Ngoc, NB; Ohashi, N; Onaka, T; Park, G; Parsons, H; Peretto, N; Priestley, F; Pyo, TS; Qian, L; Rao, R; Rawlings, J; Rawlings, M; Retter, B; Richer, J; Rigby, A; Saito, H; Savini, G; Seta, M; Sharma, E; Shimajiri, Y; Shinnaga, H; Soam, A; Tahani, M; Tamura, M; Tang, YW; Tang, XD; Tomisaka, K; Tram, LN; Tsukamoto, Y; Viti, S; Wang, HC; Wang, JW; Whitworth, A; Wu, JT; Xie, JJ; Yang, MZ; Yen, HW; Yoo, H; Yuan, JH; Yun, HS; Zenko, T; Zhang, GY; Zhang, YP; Zhang, CP; Zhou, JJ; Zhu, L; de Looze, I; André, P; Dowell, CD; Eden, D; Eyres, S; Falle, S; Le Gouellec, VJM; Poidevin, F; van Loo, S

ASTROPHYSICAL JOURNAL Vol. 977 ( 1 ) 2024.12

Theoretical Models of Protostellar Binary and Multiple Systems with AMR Simulations

Matsumoto Tomoaki, Tokuda Kazuki, Onishi Toshikazu, Inutsuka Shu-Ichiro, Saigo Kazuya, Takakuwa Shigehisa

11TH INTERNATIONAL CONFERENCE ON NUMERICAL MODELING OF SPACE PLASMA FLOWS (ASTRONUM-2016) Vol. 837 2017

The origin of rotation profiles in star-forming clouds Reviewed

Takahashi Sanemichi Z., Tomida Kengo, Machida Masahiro N., Inutsuka Shu-ichiro

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY Vol. 463 ( 2 ) page： 1390-1399 2016.12

AN ORIGIN OF MULTIPLE RING STRUCTURE AND HIDDEN PLANETS IN HL TAU: A UNIFIED PICTURE BY SECULAR GRAVITATIONAL INSTABILITY Reviewed

Takahashi Sanemichi Z., Inutsuka Shu-ichiro

ASTRONOMICAL JOURNAL Vol. 152 ( 6 ) 2016.12

Conditions for circumstellar disc formation - II. Effects of initial cloud stability and mass accretion rate Reviewed

Machida Masahiro N., Matsumoto Tomoaki, Inutsuka Shu-ichiro

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY Vol. 463 ( 4 ) page： 4246-4267 2016.12

Conditions for circumstellar disc formation - II. Effects of initial cloud stability and mass accretion rate Reviewed

M. N. Machida, T. Matsumoto, S. Inutsuka

Monthly Notices of the Royal Astronomical Society Vol. 463 ( 4 ) page： 4246-4267 2016.9

Authorship：Lead author Language：English Publishing type：Research paper (scientific journal)

Disc formation in strongly magnetized cloud cores is investigated using a three-dimensional magnetohydrodynamic simulation with a focus on the effects of the initial cloud stability and the mass accretion rate. The initial cloud stability greatly alters the disc formation process even for prestellar clouds with the same mass-to-flux ratio. A high mass accretion rate on to the disc-forming region is realized in initially unstable clouds, and a large angular momentum is introduced into the circumstellar region in a short time. The region around the protostar has both a thin infalling envelope and a weak magnetic field, which both weaken the effect of magnetic braking. The growth of the rotation-supported disc is promoted in such unstable clouds. Conversely, clouds in an initially near-equilibrium state show lower accretion rates of mass and angular momentum. The angular momentum is transported to the outer envelope before protostar formation. After protostar formation, the circumstellar region has a thick infalling envelope and a strong magnetic field that effectively brakes the disc. As a result, disc formation is suppressed when the initial cloud is in a nearly stable state. The density distribution of the initial cloud also affects the disc formation process. Disc growth strongly depends on the initial conditions when the prestellar cloud has a uniform density, whereas there is no significant difference in the disc formation process in prestellar clouds with non-uniform densities.

DOI： 10.1093/mnras/stw2256

REVEALING A DETAILED MASS DISTRIBUTION OF A HIGH-DENSITY CORE MC27/L1521F IN TAURUS WITH ALMA Reviewed

Tokuda Kazuki, Onishi Toshikazu, Matsumoto Tomoaki, Saigo Kazuya, Kawamura Akiko, Fukui Yasuo, Inutsuka Shu-ichiro, Machida Masahiro N., Tomida Kengo, Tachihara Kengo, Andre Philippe

ASTROPHYSICAL JOURNAL Vol. 826 ( 1 ) 2016.7

Atmospheric Electrification in Dusty, Reactive Gases in the Solar System and Beyond Reviewed

Helling Christiane, Harrison R. Giles, Honary Farideh, Diver Declan A., Aplin Karen, Dobbs-Dixon Ian, Ebert Ute, Inutsuka Shu-ichiro, Gordillo-Vazquez Francisco J., Littlefair Stuart

SURVEYS IN GEOPHYSICS Vol. 37 ( 4 ) page： 705-756 2016.7

DUST DYNAMICS IN PROTOPLANETARY DISK WINDS DRIVEN BY MAGNETOROTATIONAL TURBULENCE: A MECHANISM FOR FLOATING DUST GRAINS WITH CHARACTERISTIC SIZES Reviewed

Miyake Tomoya, Suzuki Takeru K., Inutsuka Shu-Ichiro

ASTROPHYSICAL JOURNAL Vol. 821 ( 1 ) 2016.4

An extension of Godunov SPH: Application to negative pressure media Reviewed

Sugiura Keisuke, Inutsuka Shu-ichiro

JOURNAL OF COMPUTATIONAL PHYSICS Vol. 308 page： 171-197 2016.3

Diffusion of cosmic rays in a multiphase interstellar medium swept-up by a supernova remnant blast wave Reviewed

Roh Soonyoung, Inutsuka Shu-ichiro, Inoue Tsuyoshi

ASTROPARTICLE PHYSICS Vol. 73 page： 1-7 2016.1

ALMA Observations of a High-density Core in Taurus: Dynamical Gas Interaction at the Possible Site of a Multiple Star Formation Reviewed

Tokuda Kazuki, Onishi Toshikazu, Saigo Kazuya, Kawamura Akiko, Fukui Yasuo, Matsumoto Tomoaki, Inutsuka Shu-ichiro, Machida Masahiro N., Tomida Kengo, Tachihara Kengo

FROM INTERSTELLAR CLOUDS TO STAR-FORMING GALAXIES: UNIVERSAL PROCESSES? ( 315 ) 2016

The Formation and Destruction of Molecular Clouds and Galactic Star Formation Reviewed

Inutsuka Shu-ichiro, Inoue Tsuyoshi, Iwasaki Kazunari, Hosokawa Takashi, Kobayashi Masato I. N.

FROM INTERSTELLAR CLOUDS TO STAR-FORMING GALAXIES: UNIVERSAL PROCESSES? ( 315 ) page： 61-68 2016

ON THE RADIUS ANOMALY OF HOT JUPITERS: REEXAMINATION OF THE POSSIBILITY AND IMPACT OF LAYERED CONVECTION Reviewed

Kurokawa Hiroyuki, Inutsuka Shu-ichiro

ASTROPHYSICAL JOURNAL Vol. 815 ( 1 ) 2015.12

Significant gas-to-dust ratio asymmetry and variation in the disk of HD 142527 and the indication of gas depletion Reviewed

Muto Takayuki, Tsukagoshi Takashi, Momose Munetake, Hanawa Tomoyuki, Nomura Hideko, Fukagawa Misato, Saigo Kazuya, Kataoka Akimasa, Kitamura Yoshimi, Takahashi Sanemichi Z., Inutsuka Shu-ichiro, Takeuchi Taku, Kobayashi Hiroshi, Akiyama Eiji, Honda Mitsuhiko, Fujiwara Hideaki, Shibai Hiroshi

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN Vol. 67 ( 6 ) 2015.12

ATMOSPHERIC ESCAPE BY MAGNETICALLY DRIVEN WIND FROM GASEOUS PLANETS. II. EFFECTS OF MAGNETIC DIFFUSION Reviewed

Tanaka Yuki A., Suzuki Takeru K., Inutsuka Shu-ichiro

ASTROPHYSICAL JOURNAL Vol. 809 ( 2 ) 2015.8

The formation and destruction of molecular clouds and galactic star formation An origin for the cloud mass function and star formation efficiency Reviewed

Inutsuka Shu-ichiro, Inoue Tsuyoshi, Iwasaki Kazunari, Hosokawa Takashi

ASTRONOMY & ASTROPHYSICS Vol. 580 2015.8

The formation and destruction of molecular clouds and galactic star formation. An origin for the cloud mass function and star formation efficiency Reviewed

Shu-ichiro Inutsuka, Tsuyoshi Inoue, Kazunari Iwasaki, Takashi Hosokawa

Astronomy & Astrophysics Vol. 580 ( A49 ) page： 7 2015.7

Authorship：Lead author Language：English Publishing type：Research paper (scientific journal)

We describe an overall picture of galactic-scale star formation. Recent high-resolution magneto-hydrodynamical simulations of two-fluid dynamics with cooling, heating, and thermal conduction have shown that the formation of molecular clouds requires multiple episodes of supersonic compression. This finding enables us to create a scenario in which molecular clouds form in interacting shells or bubbles on a galactic scale. First, we estimated the ensemble-averaged growth rate of molecular clouds on a timescale longer than a million years. Next, we performed radiation hydrodynamics simulations to evaluate the destruction rate of magnetized molecular clouds by the stellar far-ultraviolet radiation. We also investigated the resulting star formation efficiency within a cloud, which amounts to a low value (a few percent) if we adopt the power-law exponent ~2.5 for the mass distribution of stars in the cloud. We finally describe the time evolution of the mass function of molecular clouds on a long timescale (>1 Myr) and discuss the steady state exponent of the power-law slope in various environments.

DOI： 10.1051/0004-6361/201425584

Formation of terrestrial planets in disks evolving via disk winds and implications for the origin of the solar system's terrestrial planets Reviewed

Ogihara Masahiro, Kobayashi Hiroshi, Inutsuka Shu-ichiro, Suzuki Takeru K.

ASTRONOMY & ASTROPHYSICS Vol. 579 2015.7

An origin of arc structures deeply embedded in dense molecular cloud cores Reviewed

Matsumoto Tomoaki, Onishi Toshikazu, Tokuda Kazuki, Inutsuka Shu-ichiro

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY Vol. 449 ( 1 ) page： L123-L127 2015.5

THE NONLINEAR OHM'S LAW: PLASMA HEATING BY STRONG ELECTRIC FIELDS AND ITS EFFECTS ON THE IONIZATION BALANCE IN PROTOPLANETARY DISKS Reviewed

Okuzumi Satoshi, Inutsuka Shu-ichiro

ASTROPHYSICAL JOURNAL Vol. 800 ( 1 ) 2015.2

Effects of radiative transfer on the structure of self-gravitating discs, their fragmentation and the evolution of the fragments Reviewed

Tsukamoto, Y.; Takahashi, S. Z.; Machida, M. N.; Inutsuka, S.

Monthly Notices of the Royal Astronomical Society Vol. 446 ( 2 ) page： 1175-1190 2015.1

Language：English Publishing type：Research paper (scientific journal)

We investigate the structure of self-gravitating discs, their fragmentation and the evolution of the fragments (the clumps) using both an analytic approach and three-dimensional radiation hydrodynamics simulations starting from molecular cores. The simulations show that non-local radiative transfer determines the disc temperature. We find the disc structure is well described by an analytical model of a quasi-steady self-gravitating disc with radial radiative transfer. Because the radiative process is not local and radiation from the interstellar medium cannot be ignored, the local radiative cooling is not balanced with the viscous heating in a massive disc around a low-mass star. In our simulations, there are cases in which the disc does not fragment even though it satisfies the fragmentation criterion based on disc cooling time (Q~1 and Ωtcool~1). This indicates that, at least, the criterion is not a sufficient condition for fragmentation. We determine the parameter range for the host cloud core in which disc fragmentation occurs. In addition, we show that the temperature evolution of the centre of the clump is close to that of typical first cores, and that the minimum initial mass of clumps is about a few Jupiter masses.

DOI： 10.1093/mnras/stu2160

Two-component Secular Gravitational Instability in a Protoplanetary Disk: A Possible Mechanism for Creating Ring-like Structures Reviewed

Takahashi, Sanemichi Z.; Inutsuka, Shu-ichiro

The Astrophysical Journal Vol. 794 ( 1 ) page： 55 (7) 2014.10

Language：English Publishing type：Research paper (scientific journal)

The instability in protoplanetary disks due to gas-dust friction and self-gravity of gas and dust is investigated using linear analysis. In the case where the dust-to-gas ratio is enhanced and turbulence is weak, the instability grows, even in gravitationally stable disks, on a timescale of order 104-5 yr at a radius of order 100 AU. If we ignore the dynamical feedback from dust grains in the gas equation of motion, the instability reduces to the so-called "secular gravitational instability," which was investigated previously to be an instability of dust in a fixed background gas flow. In this work, we solve the equations of motion for both gas and dust consistently and find that long-wavelength perturbations are stable, in contrast to the secular gravitational instability in the simplified treatment. This may indicate that we should not neglect small terms in the equation of motion if the growth rate is small. The instability is expected to form ring structures in protoplanetary disks. The width of the ring formed at a radius of 100 AU is a few tens of AU. Therefore, the instability is a candidate for the formation mechanism of observed ring-like structures in disks. Another aspect of the instability is the accumulation of dust grains, and hence the instability may play an important role in the formation of planetesimals, rocky protoplanets, and cores of gas giants located at radii ~100 AU. If these objects survive the dispersal of the gaseous component of the disk, they may be the origin of debris disks.

DOI： 10.1088/0004-637X/794/1/55

A new scheme of causal viscous hydrodynamics for relativistic heavy-ion collisions: A Riemann solver for quark-gluon plasma Reviewed

Akamatsu, Yukinao; Inutsuka, Shu-ichiro; Nonaka, Chiho; Takamoto, Makoto

Journal of Computational Physics Vol. 256 ( 1 ) page： 34-54 2014.1

Authorship：Lead author Language：English Publishing type：Research paper (scientific journal)

In this article, we present a state-of-the-art algorithm for solving the relativistic viscous hydrodynamics equation with the QCD equation of state. The numerical method is based on the second-order Godunov method and has less numerical dissipation, which is crucial in describing of quark-gluon plasma in high-energy heavy-ion collisions. We apply the algorithm to several numerical test problems such as sound wave propagation, shock tube and blast wave problems. In sound wave propagation, the intrinsic numerical viscosity is measured and its explicit expression is shown, which is the second-order of spatial resolution both in the presence and absence of physical viscosity. The expression of the numerical viscosity can be used to determine the maximum cell size in order to accurately measure the effect of physical viscosity in the numerical simulation.

DOI： 10.1016/j.jcp.2013.08.047

Crowding-out of Giants by Dwarfs: An Origin for the Lack of Companion Planets in Hot Jupiter Systems Reviewed

Ogihara, Masahiro; Inutsuka, Shu-ichiro; Kobayashi, Hiroshi

The Astrophysical Journal Letters Vol. 778 ( 1 ) page： L9 2013.11

Language：English Publishing type：Research paper (scientific journal)

We investigate the formation of close-in terrestrial planets from planetary embryos under the influence of a hot Jupiter (HJ) using gravitational N-body simulations that include gravitational interactions between the gas disk and the terrestrial planet (e.g., type I migration). Our simulations show that several terrestrial planets efficiently form outside the orbit of the HJ, making a chain of planets, and all of them gravitationally interact directly or indirectly with the HJ through resonance, which leads to inward migration of the HJ. We call this mechanism of induced migration of the HJ "crowding-out." The HJ is eventually lost through collision with the central star, and only several terrestrial planets remain. We also find that the efficiency of the crowding-out effect depends on the model parameters; for example, the heavier the disk is, the more efficient the crowding-out is. When planet formation occurs in a massive disk, the HJ can be lost to the central star and is never observed. On the other hand, for a less massive disk, the HJ and terrestrial planets can coexist; however, the companion planets may be below the detection limit of current observations. In both cases, systems with a HJ and terrestrial planets have little chance of detection. Therefore, our model naturally explains the lack of companion planets in HJ systems regardless of the disk mass. In effect, our model provides a theoretical prediction for future observations; additional planets can be discovered just outside the HJ, and their masses should generally be small.

DOI： 10.1088/2041-8205/778/1/L9

Present-day star formation: From molecular cloud cores to protostars and protoplanetary disks Invited Reviewed

Shu-ichiro Inutsuka

Progress of Theoretical and Experimental Physics Vol. 2012 ( 1 ) page： id.01A307, 25 2012.10

Authorship：Lead author Language：English Publishing type：Research paper (scientific journal)

Essential physical processes in the formation of protostars and protoplanetary disks are described. Recent advances in non-ideal magnetohydrodynamics simulations, which cover a huge dynamic range from molecular cloud core density (10^4/cc) to stellar density (10^22/cc) in a self-consistent manner, enable us to study the realistic evolution of the magnetic field and rotation of protostars and the dynamics of outflows and jets.

DOI： 10.1093/ptep/pts024

Gravitational Fragmentation of Expanding Shells: I. Linear Analysis Reviewed

K. Iwasaki, S. Inutsuka, & T. Tsuribe

The Astrophysical Journal Vol. 733 ( 1 ) page： 16 (12pp) 2011.5

Language：English Publishing type：Research paper (scientific journal)

We perform a linear perturbation analysis of expanding shells driven by expansions of H II regions. The ambient gas is assumed to be uniform. As an unperturbed state, we develop a semi-analytic method for deriving the time evolution of the density profile across the thickness. It is found that the time evolution of the density profile can be divided into three evolutionary phases: deceleration-dominated, intermediate, and self-gravity-dominated phases. The density peak moves relatively from the shock front to the contact discontinuity as the shell expands. We perform a linear analysis taking into account the asymmetric density profile obtained by the semi-analytic method, and imposing the boundary conditions for the shock front and the contact discontinuity while the evolutionary effect of the shell is neglected. It is found that the growth rate is enhanced compared with previous studies based on the thin-shell approximation. This is due to the boundary effect of the contact discontinuity and asymmetric density profile that were not taken into account in previous works.

DOI： 10.1088/0004-637X/733/1/16

Gravitational Fragmentation of Expanding Shells. II. Three-dimensional Simulations Reviewed

K. Iwasaki, S. Inutsuka, & T. Tsuribe

The Astrophysical Journal Vol. 733 ( 1 ) page： 17 (11) 2011.5

Language：English Publishing type：Research paper (scientific journal)

We investigate the gravitational fragmentation of expanding shells driven by H II regions using the three-dimensional Lagrangian simulation codes based on the Riemann solver, called Godunov smoothed particle hydrodynamics. The ambient gas is assumed to be uniform. In order to attain high resolution to resolve the geometrically thin dense shell, we calculate not the whole but a part of the shell. We find that perturbations begin to grow earlier than predicted by linear analysis under the thin-shell approximation. The wavenumber of the most unstable mode is larger than that in the thin-shell linear analysis. The development of the gravitational instability is accompanied by the significant deformation of the contact discontinuity. These results are consistent with a linear analysis presented by Iwasaki et al. that have taken into account the density profile across the thickness and approximate shock and contact discontinuity boundary conditions. We derive useful analytic formulae for the fragment scale and the epoch when the gravitational instability begins to grow.

DOI： 10.1088/0004-637X/733/1/17

Recurrent Planet Formation and Intermittent Protostellar Outflows Induced by Episodic Mass Accretion Reviewed

Masahiro Machida, Shu-ichiro Inutsuka, & Tomoaki Matsumoto

The Astrophysical Journal Vol. in press 2011.1

Formation Process of the Circumstellar Disk: Long-term Simulations in the Main Accretion Phase of Star Formation Reviewed

Masahiro Machida, Shu-ichiro Inutsuka, & Tomoaki Matsumoto

The Astrophysical Journal Vol. 724 ( 2 ) page： 1006 2010.12

Language：English Publishing type：Research paper (scientific journal)

The formation and evolution of the circumstellar disk in unmagnetized molecular clouds is investigated using three-dimensional hydrodynamic simulations from the prestellar core until the end of the main accretion phase. In collapsing cloud cores, the first (adiabatic) core with a size of gsim3 AU forms prior to the formation of the protostar. At its formation, the first core has a thick disk-like structure and is mainly supported by the thermal pressure. After the protostar formation, it decreases the thickness gradually and becomes supported by the centrifugal force. We found that the first core is a precursor of the circumstellar disk with a size of >3 AU. This means that unmagnetized protoplanetary disk smaller than <3 AU does not exist. Reflecting the thermodynamics of the collapsing gas, at the protostar formation epoch, the first core (or the circumstellar disk) has a mass of ~0.005-0.1 M sun, while the protostar has a mass of ~10-3 M sun. Thus, just after the protostar formation, the circumstellar disk is about 10-100 times more massive than the protostar. In the main accretion phase that lasts for ~105 yr, the circumstellar disk mass initially tends to dominate the protostellar mass. Such a massive disk is unstable to gravitational instability and tends to show fragmentation. Our calculations indicate that the low-mass companions may form in the circumstellar disk in the main accretion phase. In addition, the mass accretion rate onto the protostar shows a strong time variability that is caused by the torque from the low-mass companions and/or the spiral arms in the circumstellar disk. Such variability provides an important signature for detecting the substellar mass companion in the circumstellar disk around very young protostars.

The relativistic kinetic dispersion relation: Comparison of the relativistic Bhatnagar-Gross-Krook model and Grad's 14-moment expansion Reviewed

Makoto Takamoto & Shu-ichiro Inutsuka

Physica Vol. 389 ( 21 ) page： 4580 2010.11

Language：English Publishing type：Research paper (scientific journal)

In this paper, we study the Cauchy problem of the linearized kinetic equations for the models of Marle and Anderson-Witting, and compare these dispersion relations with the 14-moment theory. First, we propose a modification of the Marle model to improve the resultant transport coefficients in accordance with those obtained by the full Boltzmann equation. Using the modified Marle model and Anderson-Witting model, we calculate dispersion relations that are kinetically correct within the validity of the BGK approximation. The 14-moment theory that includes the time derivative of dissipation currents has a causal structure, in contrast to the acausal first-order Chapman-Enskog approximation. However, the dispersion relation of the 14-moment theory does not accurately describe the result of the kinetic equation. Thus, our calculation indicates that keeping these second-order terms does not simply correspond to improving the physical description of the relativistic hydrodynamics.

Two-Step Acceleration Model of Cosmic Rays at Middle-Aged Supernova Remnants: Universality in Secondary Shocks Reviewed

Tsuyoshi Inoue, Ryo Yamazaki, & Shu-ichiro Inutsuka

The Astrophysical Journal Letters Vol. 723 ( 1 ) page： L108 2010.11

Language：English Publishing type：Research paper (scientific journal)

Recent gamma-ray observations of middle-aged supernova remnants revealed a mysterious broken power-law spectrum. Using three-dimensional magnetohydrodynamic simulations, we show that the interaction between a supernova blast wave and interstellar clouds formed by thermal instability generates multiple reflected shocks. The typical Mach numbers of the reflected shocks are shown to be Msime 2 depending on the density contrast between the diffuse intercloud gas and clouds. These secondary shocks can further energize cosmic-ray particles originally accelerated at the blast-wave shock. This "two-step" acceleration scenario reproduces the observed gamma-ray spectrum and predicts the high-energy spectral index ranging approximately from 3 to 4.

Two-Dimensional Study of the Propagation of Planetary Wake and the Indication to Gap Opening in an Inviscid Protoplanetary Disk Reviewed

Takayuki Muto, Takeru K. Suzuki, & Shu-ichiro Inutsuka

The Astrophysical Journal Vol. 724 page： 448 2010.11

Language：English Publishing type：Research paper (scientific journal)

We analyze the physical processes of gap formation in an inviscid protoplanetary disk with an embedded protoplanet using a two-dimensional local shearing-sheet model. The spiral density wave launched by the planet shocks and the angular momentum carried by the wave is transferred to the background flow. The exchange of the angular momentum can affect the mass flux in the vicinity of the planet to form an underdense region, or gap, around the planetary orbit. We first perform weakly nonlinear analyses to show that the specific vorticity formed by shock dissipation of the density wave can be a source of mass flux in the vicinity of the planet and that the gap can be opened even for low-mass planets unless the migration of the planet is substantial. We then perform high-resolution numerical simulations to check analytic consideration. By comparing the gap-opening timescale and type I migration timescale, we propose a criterion for the formation of underdense region around the planetary orbit that is qualitatively different from previous studies. The minimum mass required for the planet to form a dip is twice as small as previous studies if we incorporate the standard values of type I migration timescale, but it can be much smaller if there is a location in the disk where type I migration is halted.

Protoplanetary Disk Winds via Magnetorotational Instability: Formation of an Inner Hole and a Crucial Assist for Planet Formation Reviewed

Takeru K. Suzuki, Takayuki Muto, & Shu-ichiro Inutsuka

The Astrophysical Journal Vol. 718 ( 2 ) page： 1289-1304 2010.8

Language：English Publishing type：Research paper (scientific journal)

By constructing a global model based on three-dimensional local magnetohydrodynamical simulations, we show that the disk wind driven by magnetorotational instability (MRI) plays a significant role in the dispersal of the gas component of protoplanetary disks. Because the mass loss timescale of the MRI-driven disk winds is proportional to the local Keplerian rotation period, a gas disk dynamically evaporates from the inner region, possibly creating a gradually expanding inner hole, while a sizable amount of the gas remains in the outer region. The disk wind is highly time dependent with a quasi-periodicity of several times the Keplerian rotation period at each radius, which will be observed as the time variability of protostar-protoplanetary disk systems. These features persistently hold even if a dead zone exists because the disk winds are driven from the surface regions where ionizing cosmic rays and high energy photons can penetrate. Moreover, the predicted inside-out clearing significantly suppresses the infall of boulders to a central star and the type I migration of proto-planets, which are favorable for the formation and survival of planets.

Protoplanetary Disk Winds via Magnetorotational Instability: Formation of an Inner Hole and a Crucial Assist for Planet Formation Reviewed

Takeru K. Suzuki, Takayuki Muto, & Shu-ichiro Inutsuka

The Astrophysical Journal Vol. 718 ( 2 ) page： 1289 2010.8

Language：English Publishing type：Research paper (scientific journal)

N-Body Simulation of Planetesimal Formation through Gravitational Instability of a Dust Layer in Laminar Gas Disk Reviewed

Shugo Michikoshi, Eiichiro Kokubo, & Shu-ichiro Inutsuka

The Astrophysical Journal Vol. 719 page： 1021 2010.8

Language：English Publishing type：Research paper (scientific journal)

We investigate the formation process of planetesimals from the dust layer by the gravitational instability in the gas disk using local N-body simulations. The gas is modeled as a background laminar flow. We study the formation process of planetesimals and its dependence on the strength of the gas drag. Our simulation results show that the formation process is divided into three stages qualitatively: the formation of wake-like density structures, the creation of planetesimal seeds, and their collisional growth. The linear analysis of the dissipative gravitational instability shows that the dust layer is secularly unstable although Toomre's Q value is larger than unity. However, in the initial stage, the growth time of the gravitational instability is longer than that of the dust sedimentation and the decrease in the velocity dispersion. Thus, the velocity dispersion decreases and the disk shrinks vertically. As the velocity dispersion becomes sufficiently small, the gravitational instability finally becomes dominant. Then wake-like density structures are formed by the gravitational instability. These structures fragment into planetesimal seeds. The seeds grow rapidly owing to mutual collisions.

Emergence of Protoplanetary Disks and Successive Formation of Gaseous Planets by Gravitational Instability Reviewed

Shu-ichiro Inutsuka, Masahiro Machida, & Tomoaki Matsumoto

The Astrophysical Journal Letters Vol. 718 page： L58 2010.8

Language：English Publishing type：Research paper (scientific journal)

We use resistive magnetohydrodynamical (MHD) simulations with the nested grid technique to study the formation of protoplanetary disks around protostars from molecular cloud cores that provide the realistic environments for planet formation. We find that gaseous planetary-mass objects are formed in the early evolutionary phase by gravitational instability in regions that are decoupled from the magnetic field and surrounded by the injection points of the MHD outflows during the formation phase of protoplanetary disks. Magnetic decoupling enables massive disks to form and these are subject to gravitational instability, even at ~10 AU. The frequent formation of planetary-mass objects in the disk suggests the possibility of constructing a hybrid planet formation scenario, where the rocky planets form later under the influence of the giant planets in the protoplanetary disk.

Gas accretion onto a protoplanet and formation of a gas giant planet Reviewed

Masahiro Machida, Eiichiro Kokubo, Shu-ichiro Inutsuka, & Tomoaki Matsumoto

Monthly Notices of the Royal Astronomical Society Vol. 405 page： 1227 2010.6

Language：English Publishing type：Research paper (scientific journal)

We investigate gas accretion on to a protoplanet, by considering the thermal effect of gas in three-dimensional hydrodynamical simulations, in which the wide region from a protoplanetary gas disc to a Jovian radius planet is resolved using the nested grid method. We estimate the mass accretion rate and growth time-scale of gas giant planets. The mass accretion rate increases with protoplanet mass for Mp < Mcri, while it becomes saturated or decreases for Mp > Mcri, where Mcri ≡ 0.036MJup(ap/1 au)0.75, and MJup and ap are the Jovian mass and the orbital radius, respectively. This accretion rate is typically two orders of magnitude smaller than that in two-dimensional simulations. The growth time-scale of a gas giant planet or the time-scale of the gas accretion on to the protoplanet is about 105 yr, that is two orders of magnitude shorter than the growth time-scale of the solid core. The thermal effects barely affect the mass accretion rate because the gravitational energy dominates the thermal energy around the protoplanet. The mass accretion rate obtained in our local simulations agrees quantitatively well with those obtained in global simulations with coarser spatial resolution. The mass accretion rate is mainly determined by the protoplanet mass and the property of the protoplanetary disc. We find that the mass accretion rate is correctly calculated when the Hill or Bondi radius is sufficiently resolved. Using the oligarchic growth of protoplanets, we discuss the formation time-scale of gas giant planets.

Analysis of the Relaxation Process using Non-Relativistic Kinetic Equation Reviewed

Progress of Theoretical Physics

Progress of Theoretical Physics Vol. 123 page： 903 2010.5

Language：English Publishing type：Research paper (scientific journal)

We study the linearized kinetic equation of relaxation model proposed by Bhatnagar, Gross and Krook [P. L. Bhatnagar, E. P. Gross and M. Krook, Phys. Rev. 94 (1954), 511] (also called BGK model) and solve the dispersion relation. Using the solution of the dispersion relation, we analyze the relaxation of the macroscopic mode and kinetic mode. Since the BGK model is not based on the expansion in the mean free path in contrast to the Chapman-Enskog expansion, the solution can describe the accurate relaxation of initial disturbance with any wavelength. This nonrelativistic analysis gives suggestions for our next work on the relativistic analysis of relaxation.

Kelvin-Helmholtz instabilities with Godunov smoothed particle hydrodynamics Reviewed

Seung-Hoon Cha, Shu-ichiro Inutsuka, & Sergei Nayakshin

Monthly Notices of the Royal Astronomical Society Vol. 9999 page： 1-10 2010.1

Language：English Publishing type：Research paper (scientific journal)

Numerical simulations for the non-linear development of Kelvin-Helmholtz instability in two different density layers have been performed with the particle-based method (Godunov SPH) developed by Inutsuka. The Godunov SPH can describe the Kelvin-Helmholtz instability even with a high-density contrast, while the standard SPH shows the absence of the instability across a density gradient. The interaction of a dense blob with a hot ambient medium has been performed also. The Godunov SPH describes the formation and evolution of the fingers due to the combinations of Rayleigh-Taylor, Richtmyer-Meshkov and Kelvin-Helmholtz instabilities. The blob test result coincides well with the results of the grid-based codes.
An inaccurate handling of a density gradient in the standard SPH has been pointed out as the direct reason of the absence of the instabilities. An unphysical force happens at the density gradient even in a pressure equilibrium, and repulses particles from the initial density discontinuity. Therefore, the initial perturbation damps, and a gap form at the discontinuity. The unphysical force has been studied in terms of the consistency of a numerical scheme. Contrary to the standard SPH, the momentum equation of the Godunov SPH does not use the particle approximation, and has been derived from the kernel convolution or a new Lagrangian function. The new Lagrangian function used in the Godunov SPH is more analogous to the real Lagrangian function for continuum. The momentum equation of the Godunov SPH has much better linear consistency, so the unphysical force is greatly reduced compared to the standard SPH in a high density contrast.

Binary formation with different metallicities: dependence on initial conditions Reviewed

Masahiro N. Machida, Kazuyuki Omukai, Tomoaki Matsumoto, & Shu-ichiro Inutsuka

Monthly Notices of the Royal Astronomical Society Vol. 399 ( 3 ) page： 1255-1263 2009.11

Language：English Publishing type：Research paper (scientific journal)

The fragmentation process in collapsing clouds with various metallicities is studied using three-dimensional nested-grid hydrodynamics. Initial clouds are specified by three parameters: cloud metallicity, initial rotation energy and initial cloud shape. For different combinations of these parameters, we calculate 480 models in total and study cloud evolution, fragmentation conditions, orbital separation and binary frequency. For the cloud to fragment during collapse, the initial angular momentum must be higher than a threshold value, which decreases with decreasing metallicity. Although the exact fragmentation conditions depend also on the initial cloud shape, this dependence is only modest. Our results indicate a higher binary frequency in lower metallicity gas. In particular, with the same median rotation parameter as in the solar neighbourhood, a majority of stars are born as members of binary/multiple systems for <10-4Zsolar. With initial mass <0.1Msolar, if fragments are ejected in embryo from the host clouds by multibody interaction, they evolve to substellar-mass objects. This provides a formation channel for low-mass stars in zero- or low-metallicity environments.

N-body Simulation of Planetesimal Formation Through Gravitational Instability and Coagulation. II. Accretion Model Reviewed

Shugo Michikoshi, Eiichiro Kokubo, & Shu-ichiro Inutsuka

The Astrophysical Journal Vol. 703 ( 2 ) page： 1363-1373 2009.10

Language：English Publishing type：Research paper (scientific journal)

The gravitational instability of a dust layer is one of the scenarios for planetesimal formation. If the density of a dust layer becomes sufficiently high as a result of the sedimentation of dust grains toward the midplane of a protoplanetary disk, the layer becomes gravitationally unstable and spontaneously fragments into planetesimals. Using a shearing box method, we performed local N-body simulations of gravitational instability of a dust layer and subsequent coagulation without gas and investigated the basic formation process of planetesimals. In this paper, we adopted the accretion model as a collision model. A gravitationally bound pair of particles is replaced by a single particle with the total mass of the pair. This accretion model enables us to perform long-term and large-scale calculations. We confirmed that the formation process of planetesimals is the same as that in the previous paper with the rubble pile models. The formation process is divided into three stages: the formation of nonaxisymmetric structures; the creation of planetesimal seeds; and their collisional growth. We investigated the dependence of the planetesimal mass on the simulation domain size. We found that the mean mass of planetesimals formed in simulations is proportional to L 3/2 y , where Ly is the size of the computational domain in the direction of rotation. However, the mean mass of planetesimals is independent of Lx , where Lx is the size of the computational domain in the radial direction if Lx is sufficiently large. We presented the estimation formula of the planetesimal mass taking into account the simulation domain size.

Two-Fluid Magnetohydrodynamics Simulations of Converging H I Flows in the Interstellar Medium. II. Are Molecular Clouds Generated Directly from a Warm Neutral Medium? Reviewed

Tsuyoshi Inoue & Shu-ichiro Inutsuka

The Astrophysical Journal Vol. 704 ( 1 ) page： 161-169 2009.10

Language：English Publishing type：Research paper (scientific journal)

Formation of interstellar clouds as a consequence of thermal instability is studied using two-dimensional two-fluid magnetohydrodynamic simulations. We consider the situation of converging, supersonic flows of warm neutral medium in the interstellar medium that generate a shocked slab of thermally unstable gas in which clouds form. We find, as speculated in Paper I, that in the shocked slab magnetic pressure dominates thermal pressure and the thermal instability grows in the isochorically cooling, thermally unstable slab that leads to the formation of H I clouds whose number density is typically n lsim 100 cm-3, even if the angle between magnetic field and converging flows is small. We also find that even if there is a large dispersion of magnetic field, evolution of the shocked slab is essentially determined by the angle between the mean magnetic field and converging flows. Thus, the direct formation of molecular clouds by piling up warm neutral medium does not seem to be a typical molecular cloud formation process, unless the direction of supersonic converging flows is biased to the orientation of mean magnetic field by some mechanism. However, when the angle is small, the H I shell generated as a result of converging flows is massive and possibly evolves into molecular clouds, provided gas in the massive H I shell is piled up again along the magnetic field line. We expect that another subsequent shock wave can again pile up the gas of the massive shell and produce a larger cloud. We thus emphasize the importance of multiple episodes of converging flows, as a typical formation process of molecular clouds.

The Circumbinary Outflow: A Protostellar Outflow Driven by a Circumbinary Disk Reviewed

Masahiro N. Machida, Shu-ichiro Inutsuka, & Tomoaki Matsumoto

The Astrophysical Journal Vol. 704 ( 1 ) page： L10-L14 2009.10

Language：English Publishing type：Research paper (scientific journal)

Protostellar outflow is a star's first cry at the moment of birth. The outflows have an indispensable role in the formation of single stars because they carry off the excess angular momentum from the center of the shrinking gas cloud, and permit further collapse to form a star. On the other hand, a significant fraction of stars is supposedly born as binaries with circumbinary disks that are frequently observed. Here, we investigate the evolution of a magnetized rotating cloud using a three-dimensional resistive MHD nested-grid code, and show that the outflow is driven by the circumbinary disk and has an important role even in the binary formation. After the adiabatic core formation in the collapsing cloud core, the magnetic flux is significantly removed from the center of the cloud by the Ohmic dissipation. Since this removal makes the magnetic braking ineffective, the adiabatic core continuously acquires the angular momentum to induce fragmentation and subsequent binary formation. The magnetic field accumulates in the circumbinary disk where the removal and accretion of magnetic field are balanced, and finally drives the circumbinary outflow. This result explains the spectacular morphology of some specific young stellar objects such as L1551 IRS5. We can infer that most of the bipolar molecular outflows observed by low density tracers (i.e., CO) would correspond to circumbinary or circum-multiple outflows found in this Letter, since most of the young stellar objects are supposed to be binaries or multiples.

Emission from a Young Protostellar Object I. Signatures of Young Embedded Outflows Reviewed

Masako Yamada, Masahiro N. Machida, Shu-ichiro Inutsuka, & Kohji Tomisaka

The Astrophysical Journal Vol. 703 ( 1 ) page： 1141-1158 2009.9

Language：English Publishing type：Research paper (scientific journal)

We examine emission from a young protostellar object (YPO) with three-dimensional ideal magnetohydrodynamic (MHD) simulations and three-dimensional non-local thermodynamic equilibrium line transfer calculations, and show the first results. To calculate the emission field, we employed a snapshot result of an MHD simulation having young bipolar outflows and a dense protostellar disk (a young circumstellar disk) embedded in an infalling envelope. Synthesized line emission of two molecular species (CO and SiO) shows that subthermally excited SiO lines as a high-density tracer can provide a better probe of the complex velocity field of a YPO, compared to fully thermalized CO lines. In a YPO at the earliest stage when the outflows are still embedded in the collapsing envelope, infall, rotation, and outflow motions have similar speeds. We find that the combined velocity field of these components introduces a great complexity in the line emissions through varying optical thickness and emissivity, such as asymmetric double-horn profiles. We show that the rotation of the outflows, one of the features that characterizes an outflow driven by magneto-centrifugal forces, appears clearly in velocity channel maps and intensity-weighted mean velocity (first moment of velocity) maps. The somewhat irregular morphology of the line emission at this youngest stage is dissimilar to a more evolved object such as young Class 0. High angular resolution observation by, e.g., the Atacama Large Millimeter/submillimeter Array telescope can reveal these features. Our results demonstrate a powerful potential of the synthesized emission of the three-dimensional line transfer to probe the velocity field embedded in the envelope, and further analysis will be able to determine the precise velocity field to assess the dynamics in the YPO to gain a better understanding of star formation.

A Hybrid Scenario for Planet Formation

Shu-ichiro Inutsuka

AIP Conference Proceedings Vol. 1158 page： 31-34 2009.8

Authorship：Lead author Language：English Publishing type：Research paper (scientific journal)

The standard scenario for the formation of planets has two critical problems: (1) Turbulence in the disk stirs up dust particles and prevents the dust sedimentation onto the disk mid-plane that is required for the fragmentation of the dusty layer prior to planetesimal formation. (2) The gravitational interaction of (proto)planets and the disk tends to result in their migration onto the central star within a short timescale. These problems have stimulated extensive theoretical work but still remain to be solved. In contrast, the recent increase of our understanding of the star formation process enables us to depict the long-term evolution of protoplanetary disks: the resultant gravitational fragmentation and the formation of gaseous planetary-mass objects in the disks. We critically review recent progress in our understanding of these processes and propose a possible hybrid scenario for the formation of planetary-mass objects in variety.

Local Linear Analysis of Interaction between a Planet and Viscous Disk and an Implication on Type I Planetary Migration Reviewed

Takayuki Muto & Shu-ichiro Inutsuka

The Astrophysical Journal Vol. 701 ( 1 ) page： 18-31 2009.8

Language：English Publishing type：Research paper (scientific journal)

We investigate the effects of viscosity on disk-planet interaction and discuss how type I migration of planets is modified. We have performed a linear calculation using shearing-sheet approximation and obtained the detailed, high-resolution density structure around the planet embedded in a viscous disk with a wide range of viscous coefficients. We use a time-dependent formalism that is useful in investigating the effects of various physical processes on disk-planet interaction. We find that the density structure in the vicinity of the planet is modified and the main contribution to the torque comes from this region, in contrast to the inviscid case. Although it is not possible to derive total torque acting on the planet within the shearing-sheet approximation, the one-sided torque can be very different from the inviscid case, depending on the Reynolds number. This effect has been neglected so far but our results indicate that the interaction between a viscous disk and a planet can be qualitatively different from an inviscid case and the details of the density structure in the vicinity of the planet are critically important.

First Direct Simulation of Brown Dwarf Formation in a Compact Cloud Core Reviewed

Masahiro N. Machida, Shu-ichiro Inutsuka, & Tomoaki Matsumoto

The Astrophysical Journal Vol. 699 ( 2 ) page： L157 2009.7

Language：English Publishing type：Research paper (scientific journal)

Brown dwarf formation and star formation efficiency are studied using a nested grid simulation that covers 5 orders of magnitude in spatial scale (104-0.1 AU). Starting with a rotating magnetized compact cloud with a mass of 0.22 M sun(225 M Jup), we follow the cloud evolution until the end of the main accretion phase. An outflow of ~5 km s-1 emerges ~100 yr before the protostar formation and does not disappear until the end of the calculation. The mass accretion rate declines from ~10-6 M sun yr-1 to ~10-8-10-12 M sun yr-1 in a short time (~104 yr) after the protostar formation. This is because (1) a large fraction of mass is ejected from the host cloud by the protostellar outflow and (2) the gas escapes from the host cloud by the thermal pressure. At the end of the calculation, 74% (167 M Jup) of the total mass (225 M Jup) is outflowing from the protostar, in which 34% (77 M Jup) of the total mass is ejected by the protostellar outflow with supersonic velocity and 40% (90 M Jup) escapes with subsonic velocity. On the other hand, 20% (45 M Jup) is converted into the protostar and 6% (13 M Jup) remains as the circumstellar disk. Thus, the star formation efficiency is epsilon = 0.2. The resultant protostellar mass is in the mass range of brown dwarfs. Our results indicate that brown dwarfs can be formed in compact cores in the same manner as hydrogen-burning stars, and the magnetic field and protostellar outflow are essential in determining the star formation efficiency and stellar mass.

Turbulence and Magnetic Field Amplification in Supernova Remnants: Interactions Between a Strong Shock Wave and Multiphase Interstellar Medium Reviewed

Tsuyoshi Inoue, Ryo Yamazaki, & Shu-ichiro Inutsuka

The Astrophysical Journal Vol. 695 ( 2 ) page： 825-833 2009.4

Language：English Publishing type：Research paper (scientific journal)

We examine magnetohydrodynamic simulations of the propagation of a strong shock wave through the interstellar two-phase medium composed of small-scale cloudlets and diffuse warm neutral medium in two-dimensional geometry. The preshock two-phase medium is provided as a natural consequence of the thermal instability that is expected to be ubiquitous in the interstellar medium. We show that the shock-compressed shell becomes turbulent owing to the preshock density inhomogeneity, and magnetic field amplification takes place in the shell. The maximum field strength is determined by the condition that plasma β ~ 1, which gives the field strength on the order of 1 mG in the case of shock velocity ~103 km s-1. The strongly magnetized region shows filamentary and knotlike structures in two-dimensional simulations. The spatial scale of the regions with a magnetic field of ~1 mG in our simulation is roughly 0.05 pc, which is comparable to the spatial scale of the X-ray hot spots recently discovered in supernova remnants where the magnetic field strength is indicated to be amplified up to the order of 1 mG. This result may also suggest that the turbulent region with a locally strong magnetic field is expected to be spread out in the region with frequent supernova explosions, such as in the Galactic center and starburst galaxies.

Orbital Evolution of a Particle Interacting with a Single Planet in a Protoplanetary Disk Reviewed

Takayuki Muto & Shu-ichiro Inutsuka

The Astrophysical Journal Vol. 695 ( 2 ) page： 1132-1150 2009.4

Language：English Publishing type：Research paper (scientific journal)

We investigate the motion of a particle around a low-mass planet embedded in a nonturbulent gaseous disk. We take into account the effect of the gas structure that is modified by the gravitational interaction between the planets. We derive an analytic formula that describes the change of the semimajor axis of the particle due to the encounter with the planet using local approximation in a distant encounter regime. Our final formula includes the effects of steady, axisymmetric radial gas flow, the global gas pressure gradient in the disk, planet gravity, and the structure of the gas flow modified by the planet's gravity. We compare the analytic results with numerical calculations and indicate that our formula well describes the secular evolution of the dust particles' semimajor axes well, especially for small particles with large drag coefficients. We discuss the conditions for dust gap opening around a low-mass planet and radial distribution of dust particles. Our formula may provide a useful tool for calculating radial distribution of particles in a disk around the planet.

Supernova Propagation and Cloud Enrichment: A New Model for 60Fe Origin in Early Solar System Reviewed

Matthieu Gounelle, Anders Meibom, Patrick Hennebelle & Shu-ichiro Inutsuka

The Astrophysical Journal Vol. 694 ( 1 ) page： L1 2009.3

Language：English Publishing type：Research paper (scientific journal)

The radioactive isotope 60Fe (T 1/2 = 1.5 Myr) was present in the early solar system. It is unlikely that it was injected directly into the nascent solar system by a single, nearby supernova (SN). It is proposed instead that it was inherited during the molecular cloud (MC) stage from several SNe belonging to previous episodes of star formation. The expected abundance of 60Fe in star-forming regions is estimated taking into account the stochasticity of the star-forming process, and it is showed that many MCs are expected to contain 60Fe (and possibly 26Al [T 1/2 = 0.74 Myr]) at a level compatible with that of the nascent solar system. Therefore, no special explanation is needed to account for our solar system's formation.

*High- and Low-Velocity Magnetized Outflows in the Star Formation Process in a Gravitationally Collapsing Cloud Reviewed

Masahiro N. Machida, Shu-ichiro Inutsuka, Tomoaki Matsumoto

The Astrophysical Journal Vol. 676 ( 1 ) page： 1088-1108 2008.4

Language：English Publishing type：Research paper (scientific journal)

The driving mechanisms of low- and high-velocity outflows in star formation processes are studied using three-dimensional resistive MHD simulations. Starting with a Bonnor-Ebert isothermal cloud rotating in a uniform magnetic field, we calculate cloud evolution from the molecular cloud core (nc=104 cm-3) to the stellar core (nc=1022 cm-3), where nc denotes the central density. In the collapsing cloud core, we found two distinct flows: low-velocity flows (~5 km s-1) with a wide opening angle, driven from the adiabatic core when the central density exceeds nc>~1012 cm-3; and high-velocity flows (~30 km s-1) with good collimation, driven from the protostar when the central density exceeds nc>~1021 cm-3. High-velocity flows are enclosed by low-velocity flows after protostar formation. The difference in the degree of collimation between the two flows is caused by the strength of the magnetic field and configuration of the magnetic field lines. The magnetic field around an adiabatic core is strong and has an hourglass configuration; therefore, flows from the adiabatic core are driven mainly by the magnetocentrifugal mechanism and guided by the hourglass-like field lines. In contrast, the magnetic field around the protostar is weak and has a straight configuration owing to ohmic dissipation in the high-density gas region. Therefore, flows from the protostar are driven mainly by the magnetic pressure gradient force and guided by straight field lines. Differing depth of the gravitational potential between the adiabatic core and the protostar causes the difference of flow speed. Low-velocity flows may correspond to the observed molecular outflows, while high-velocity flows may correspond to the observed optical jets. We suggest that the protostellar outflow and the jet are driven by different cores, rather than the outflow being entrained by the jet.

*Angular Momentum Transport by Magnetohydrodynamic Turbulence in Accretion Disks: Gas Pressure Dependence of the Saturation Level of the Magnetorotational Instability Reviewed

Takayoshi Sano, Shu-ichiro Inutsuka, Neal J. Turner, James M. Stone

The Astronphysical Journal Vol. 605 ( 1 ) page： 321-339 2004.4

Language：English Publishing type：Research paper (scientific journal)

The saturation level of the magnetorotational instability (MRI) is investigated using three-dimensional MHD simulations. The shearing box approximation is adopted and the vertical component of gravity is ignored, so that the evolution of the MRI is followed in a small local part of the disk. We focus on the dependence of the saturation level of the stress on the gas pressure, which is a key assumption in the standard α disk model. From our numerical experiments we find that there is a weak power-law relation between the saturation level of the Maxwell stress and the gas pressure in the nonlinear regime; the higher the gas pressure, the larger the stress. Although the power-law index depends slightly on the initial field geometry, the relationship between stress and gas pressure is independent of the initial field strength and is unaffected by ohmic dissipation if the magnetic Reynolds number is at least 10. The relationship is the same in adiabatic calculations, where pressure increases over time, and nearly isothermal calculations, where pressure varies little with time. Over the entire region of parameter space explored, turbulence driven by the MRI has many characteristic ratios such as that of the Maxwell stress to the magnetic pressure. We also find that the amplitudes of the spatial fluctuations in density and the time variability in the stress are characterized by the ratio of magnetic pressure to gas pressure in the nonlinear regime. Our numerical results are qualitatively consistent with an idea that the saturation level of the MRI is determined by a balance between the growth of the MRI and the dissipation of the field through reconnection. The quantitative interpretation of the pressure-stress relation, however, may require advances in the theoretical understanding of nonsteady magnetic reconnection.

*Reformulation of Smoothed Particle Hydrodynamics with Riemann Solver Reviewed

Shu-ichiro Inutsuka

Journal of Computational Physics Vol. 179 ( 1 ) page： 238-267 2002.6

Authorship：Lead author Language：English Publishing type：Research paper (scientific journal)

Smoothed particle hydrodynamics is reformulated in terms of the convolution of the original hydrodynamics equations, and the new evolution equations for the particles are derived. The same evolution equation of motion is also derived using a new action principle. The force acting on each particle is determined by solving the Riemann problem. The use of the Riemann solver strengthens the method, making it accurate for the study of phenomena with strong shocks. The prescription for the variable smoothing length is shown. These techniques are implemented in strict conservation form. The results of a few test problems are also shown.

*An Origin of Supersonic Motions in Interstellar Clouds Reviewed

Hiroshi Koyama, Shu-ichiro Inutsuka

The Astronphysical Journal Vol. 564 ( 2 ) page： L97-L100 2002.1

Language：English Publishing type：Research paper (scientific journal)

The propagation of a shock wave into an interstellar medium is investigated by two-dimensional numerical hydrodynamic calculation with cooling, heating, and thermal conduction. We present results of the high-resolution, two-dimensional calculations to follow the fragmentation that results from thermal instability in a shock-compressed layer. We find that the geometrically thin cooling layer behind the shock front fragments into small cloudlets. The cloudlets have supersonic velocity dispersion in the warm neutral medium, in which the fragments are embedded as cold condensations. The fragments tend to coalesce and become larger clouds.

*A Radiation Hydrodynamic Model for Protostellar Collapse. II. The Second Collapse and the Birth of a Protostar Reviewed

Hirohiko Masunaga, Shu-ichiro Inutsuka

The Astrophysical Journal Vol. 351 ( 1 ) page： 350-365 2000.3

Authorship：Lead author Language：English Publishing type：Research paper (scientific journal)

We carry out radiation hydrodynamic calculations to study physical processes in the formation of a 1 Msolar protostar. Following our previous work, calculations pursue the whole evolution from the beginning of the first collapse to the end of the main accretion phase. The adiabatic core formed after the initial collapse (i.e., the first core) experiences further gravitational collapse triggered by dissociation of molecular hydrogen, which leads to the formation of the second core, i.e., the birth of a protostar. The protostar grows in mass as accreting the infalling material from the circumstellar envelope, while the protostar keeps its radius at ~4 Rsolar during the main accretion phase. These typical features in the evolution are in good agreement with previous studies. We consider two different initial conditions for the density distribution: homogeneous and hydrostatic cloud cores with the same central density of 1.415x10-19 g cm-3 . The homogeneous core has the total mass of 1 Msolar while the hydrostatic core has 3.852 Msolar. For the initially homogeneous model, the accretion luminosity rapidly rises to the maximum value of 25 Lsolar just after the birth of a protostar, and declines gradually as the mass accretion rate decreases. In contrast, the luminosity increases monotonically with time for the initially hydrostatic model. This difference arises because the mass accretion rate varies depending on the inward acceleration at the initial stage, which affects the luminosity curve. A less massive hydrostatic core would possess the similar properties in the luminosity curve to the 3.852 Msolar case, because a hydrostatic cloud core with mass lower than 3.852 Msolar can be shown to provide a smaller mass accretion rate after the birth of a protostar and a more gradual rise in the luminosity curve. Our numerical code is designed to provide the evolution of the spectral energy distribution (SED) along with the dynamical evolution in our spherically symmetric calcu

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