Faculty Profiles - SHINBORI Atsuki

Solar zenith angle dependence of plasma density and temperature in the polar cap ionosphere and low-altitude magnetosphere during geomagnetically quiet periods at solar maximum Reviewed

超高層物理学のための分野横断型メタデータ・データベースの構築

梅村宜生, 小山幸伸, 堀智昭, 阿部修司, 林寛生, 新堀淳樹, 田中良昌, 上野悟, 米田瑞生, 金田直樹, 元場哲郎

第4回データ工学と情報マネジメントに関するフォーラム論文集 page： A7-1 2012

N. Kitamura, Y. Ogawa, Y. Nishimura, N. Terada, T. Ono, A. Shinbori, A. Kumamoto, V. Truhlik, J. Smilauer

JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS Vol. 116 ( 8 ) 2011.8

Language：English Publishing type：Research paper (scientific journal) Publisher：AMER GEOPHYSICAL UNION

We constructed an empirical model of the electron density profile with solar zenith angle (SZA) dependence in the polar cap during geomagnetically quiet periods using 63 months of Akebono satellite observations at solar maximum. The electron density profile exhibits a transition at similar to 2000 km altitude only under dark conditions. The electron density and scale height at low altitudes change drastically, by factors of 25 (at 2300 km altitude) and 2.0, respectively, as the SZA increases from 90 degrees to 120 degrees. The SZA dependence of the ion and electron temperatures is also investigated statistically on the basis of data obtained by the Intercosmos satellites and European Incoherent Scatter (EISCAT) Svalbard radar (ESR). A drastic change in the electron temperature occurs near the terminator, similarly to that in the electron density profile obtained by the Akebono satellite. The sum of the ion and electron temperatures obtained by the ESR (similar to 6500 K at similar to 1050 km altitude under sunlit conditions and similar to 3000 K at similar to 750 km altitude under dark conditions) agrees well with the scale height at low altitudes obtained from the Akebono observations, assuming that the temperature is constant and that O(+) ions are dominant. Comparisons between the present statistical results (SZA dependence of the electron density and ion and electron temperatures) and modeling studies of the polar wind indicate that the plasma density profile (especially of the O(+) ion density) in the polar cap is strongly controlled by solar radiation onto the ionosphere by changing ion and electron temperatures in the ionosphere during geomagnetically quiet periods.

DOI： 10.1029/2011JA016631

Penetration of Magnetospheric Electric Fields to the Low Latitude Ionosphere During Storm/Substorms Reviewed

Penetration of Magnetospheric Electric Fields to the Low Latitude Ionosphere During Storm/Substorms Reviewed

Kikuchi, T, K. K. Hashimoto, A. Shinbori, Y. Tsuji, S. Watari

Aeronomy of the Earth's Atmosphere and Ionosphere IAGA Special Sopron Book Series 2, DOI: 10.1007/978-94-007-0326-1_34, Edit. M.A. Abdu, D.Pancheva, A. Bhattacharyya, Springer Science+Business Media B.V. Vol. 2 page： 443 - 453 2011.2

Kikuchi, T; Hashimoto, KK; Shinbori, A; Tsuji, Y; Watari, SI

AERONOMY OF THE EARTH'S ATMOSPHERE AND IONOSPHERE Vol. 2 page： 443 - 453 2011

IUGONET解析ソフトウェアの開発", 宇宙科学情報解析論文誌 Reviewed

新堀淳樹

宇宙科学情報解析論文誌 Vol. 1巻 2011

Direct measurements of the Poynting flux associated with convection electric fields in the magnetosphere Reviewed

Y. Nishimura, T. Kikuchi, A. Shinbori, J. Wygant, Y. Tsuji, T. Hori, T. Ono, S. Fujita, T. Tanaka

JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS Vol. 115 ( 12 ) 2010.12

Language：English Publishing type：Research paper (scientific journal) Publisher：AMER GEOPHYSICAL UNION

Observations of Poynting fluxes associated with onset of convection electric fields are essential for understanding of electromagnetic energy transport from the solar wind toward the magnetosphere leading to changes in the convection electric field, which is one of the most fundamental parameters in the magnetosphere-ionosphere coupled system. We present Cluster multispacecraft observations of Poynting fluxes associated with abrupt changes in large-scale electric fields during sudden commencements and southward turning of the interplanetary magnetic field (IMF). The Cluster spacecraft detected Poynting fluxes dominated by the field-aligned upward component during the preliminary impulse of sudden commencements and in the initial period after southward turning of the IMF. The upward Poynting flux indicates existence of Alfven waves transporting electromagnetic energy from the ionosphere toward the magnetosphere leading to magnetospheric convection changes. The waveguide model and global magnetohydrodynamic (MHD) simulation calculating evolution of the Poynting flux following solar wind pressure enhancements also show upward Poynting fluxes propagating from the ionosphere toward the magnetosphere faster than the propagation of compressional waves. We conclude that the ionosphere acts as a channel to transmit electromagnetic energy supplied as field-aligned currents toward a wide region in the magnetosphere-ionosphere system instantaneously, leading to changes in magnetospheric convection electric fields.

DOI： 10.1029/2010JA015491

Observations of very-low-energy (< 10 eV) ion outflows dominated by O+ ions in the region of enhanced electron density in the polar cap magnetosphere during geomagnetic storms Reviewed Open Access

N. Kitamura, Y. Nishimura, T. Ono, Y. Ebihara, N. Terada, A. Shinbori, A. Kumamoto, T. Abe, M. Yamada, S. Watanabe, A. Matsuoka, A. W. Yau

JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS Vol. 115 ( 11 ) 2010.11

Language：English Publishing type：Research paper (scientific journal) Publisher：AMER GEOPHYSICAL UNION

Velocity distributions of upflowing ions in the polar ionosphere are crucial to understand their destinations. Natural plasma wave observations by the plasma wave and sounder experiments and thermal ion observations by the suprathermal ion mass spectrometer onboard the Akebono satellite at similar to 9000 km altitude in the polar magnetosphere during the geomagnetic storms showed that ions in the region of enhanced electron density in the polar cap were dominated by very-low-energy O+ ions (similar to 85%) with upward velocities of 4-10 km s(-1), corresponding to streaming energies of 1.3-8.4 eV. The fluxes of very-low-energy upflowing O+ ions exceeded 1 x 10(9) cm(-2) s(-1) (mapped to 1000 km altitude) across wide regions. These signatures are consistent with high-density plasma supplied by the cleft ion fountain mechanism. Trajectory calculations of O+ ions based on the Akebono observations as the initial condition showed the transport paths and accelerations of the O+ ions and indicated that the velocities of the very-low-energy upflowing O+ ions through the dayside polar cap are enough to reach the magnetosphere under strong convection. The calculations suggest the importance of the very-low-energy upflowing O+ ions with large fluxes in the total O+ ion supply toward the magnetosphere, especially the near-Earth tail region and inner magnetosphere. The initially very-low-energy O+ ions can contribute significantly to the ring current formation during geomagnetic storms since some of the O+ ions were transported into the ring current region with typical energies of ring current ions (several tens of keV) in the trajectory calculations.

DOI： 10.1029/2010JA015601

Anomalous occurrence features of the preliminary impulse of geomagnetic sudden commencement in the South Atlantic Anomaly region Reviewed Open Access

Atsuki Shinbori, Yukitoshi Nishimura, Yuji Tsuji, Takashi Kikuchi, Tohru Araki, Akihiro Ikeda, Teiji Uozumi, Roland E. S. Otadoy, Hisashi Utada, Jose Ishitsuka, Nalin Baual Trivedi, Severino L. G. Dutra, Nelson Jorge Schuch, Shinichi Watari, Tsutomu Nagatsuma, Kiyohumi Yumoto

JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS Vol. 115 ( 8 ) 2010.8

Language：English Publishing type：Research paper (scientific journal) Publisher：AMER GEOPHYSICAL UNION

Occurrence features of the preliminary impulse (PI) of geomagnetic sudden commencement (SC) both in the Pacific Ocean and South Atlantic Anomaly (SAA) regions were investigated using the long-term magnetic field data obtained from the Circum-pan Pacific Magnetometer Network (CPMN) and NICT Space Weather Monitoring (NSWM) magnetometer networks. The low-latitude preliminary reverse impulse (PRI) at Okinawa (OKI: dip latitude = 37.97 degrees) in the Pacific Ocean region appeared in all the magnetic local time (MLT) sectors with the peak occurrence rate of 40% around noon. On the other hand, the PRI occurrence rate at Santa Maria (SMA: dip latitude = -34.35 degrees) near the center of the SAA region showed a significant enhancement in the daytime sector (0800-1600 h, MLT) with the peak value of 80%, which resembles the occurrence feature of the equatorial PRI. Moreover, the PRI amplitude around noon at SMA was about 3.0 times larger than that at OKI. From the calculation of the ionospheric conductivity derived from the IRI-2007 and NRLMSISE-00 models, it is shown that the height-integrated conductivity was more enhanced in the SAA region (SMA), where the ambient magnetic field intensity is weak, compared with that in the Pacific Ocean region (OKI). Therefore, the anomalous increase of the PRI occurrence and amplitude is caused by the significant enhancement of the ionospheric conductivity due to the weakness of the ambient magnetic field intensity in the SAA region.

DOI： 10.1029/2009JA015035

Temporal variations and spatial extent of the electron density enhancements in the polar magnetosphere during geomagnetic storms Reviewed

Anomalous Enhancement of Occurrence of the Preliminary Impulse of Geomagnetic Sudden Commencement (SC) at Low Latitude in the South Atlantic Anomaly (SAA) region Reviewed

Shinbori A, Y. Nishimura, Y. Tsuji, T. Kikuchi, T. Araki, A. Ikeda, T. Uozumi, R. Otadoy, H. Utada, J. Ishitsuka, N. Trivedi, S. Dutra, N. Schuch, S. Watari, T. Nagatsuma, K. Yumoto

Journal of Geophysical Research: Space Physics, Volume 115, Issue A8, CiteID: A08309, doi: 10.1029/2009JA015035 Vol. 115 ( A8 ) 2010.8

Kitamura, N, Y. Nishimura, T. Ono, A. Kumamoto, A. Shinbori, M. Iizima, A. Matsuoka, M. R. Hairston

J. Geophys. Res. Vol. 115 ( A7 ) 2010.7

Penetration of magnetospheric electric fields to the equator and their effects on the low-latitude ionosphere during intense geomagnetic storms Reviewed

B. Veenadhari, S. Alex, T. Kikuchi, A. Shinbori, Rajesh Singh, E. Chandrasekhar

JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS Vol. 115 ( A3 ) 2010.3

Language：English Publishing type：Research paper (scientific journal) Publisher：AMER GEOPHYSICAL UNION

The penetration of magnetospheric electric fields to the magnetic equator has been investigated for two intense magnetic storms that occurred on 31 March 2001 and 6 November 2001. The digital ground magnetic data from equatorial station Tirunelveli (TIR, 0.17 degrees S geomagnetic latitude (GML)) and low-latitude station Alibag (ABG, 10.17 degrees N GML) have been used to identify the storm time electrojet index, EEJ(Dis), which is the difference of the magnetic field variations between TIR and ABG after removing the quiet day variations. The appearance of enhanced DP 2 currents and counterelectrojets (CEJ) during the main and recovery phases of the magnetic storms is possibly due to prompt penetration of electric fields from the high latitudes. These signatures can be interpreted as a clear indicator of the eastward and westward electric fields at the equator. The observed results suggest that the magnitude of the equatorial ionospheric currents driven by the penetrating electric fields is very sensitive to ionospheric conductivity (which depends on local time). Moreover, the intensity of the DP 2 currents started decreasing during the end of the main phase of the storm despite the large negative southward IMF Bz, indicating the dominance of a well-developed shielding electric field for 1 h. As an effect of penetrating electric fields at the equator, the equatorial ionization anomaly is enhanced during the main phase (because of strong eastward electric field) and is inhibited or reduced due to the strong CEJ (because of westward electric field) during the recovery phase.

DOI： 10.1029/2009JA014562

Development metadata database for upper atmosphere

Koyama, Y, Y.-M. Tanaka, T. Kouno, H. Hayashi, T. Hori, M. Kagitani, D. Yoshida, S. UeNo, S. Abe, A. Shinbori, N. Kaneda

Proceedings of CAWSES-II Kickoff Symposium in Japan page： 135-136 2010

Scientific perspectives powered by IUGONET metadata database and integrated analysis tool

Hori, T, Y. Koyama, Y.-M. Tanaka, M. Kagitani, H. Hayashi, A. Shinbori, S. UeNo, D. Yoshida, S. Abe, T. Kouno, N. Kaneda, H. Tadokoro, IUGONET project members

Proceedings of CAWSES-II Kickoff Symposium in Japan page： 71-74 2010

Response of convection electric fields in the magnetosphere to IMF orientation change Reviewed Open Access

Y. Nishimura, T. Kikuchi, J. Wygant, A. Shinbori, T. Ono, A. Matsuoka, T. Nagatsuma, D. Brautigam

JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS Vol. 114 ( 9 ) 2009.9

Language：English Publishing type：Research paper (scientific journal) Publisher：AMER GEOPHYSICAL UNION

The transient response of convection electric fields in the inner magnetosphere to southward turning of the interplanetary magnetic field (IMF) is investigated using in-situ electric field observations by the CRRES and Akebono spacecraft. Electric fields earthward of the inner edge of the electron plasma sheet show quick responses simultaneously with change in ionospheric electric fields, which indicates the arrival of the first signal related to southward turning. A coordinated observation of the electric field by the CRRES and Akebono spacecraft separated by 5 RE reveals a simultaneous increase in the dawn-dusk electric field in a wide region of the inner magnetosphere. A quick response associated with the southward turning of the IMF is also identified in in-situ magnetic fields. It indicates that the southward turning of the IMF initiates simultaneous (less than 1 min) enhancements of ionospheric electric fields, convection electric fields in the inner magnetosphere, and the ring or tail current and region 2 FACs. In contrast, a quick response of convection electric fields is not identified in the electron plasma sheet. A statistical study using 161 events of IMF orientation change in 1991 confirms a prompt response within 5 min for 80% of events earthward of the electron plasma sheet, while a large time lag of more than 30 min is identified in electric fields in the electron plasma sheet. The remarkable difference in the response of electric fields indicates that electric fields in the electron plasma sheet are weakened by high conductance in the magnetically conjugated auroral ionosphere.

DOI： 10.1029/2009JA014277

Magnetic latitude and local time dependence of the amplitude of geomagnetic sudden commencements Reviewed

Magnetic latitude and local time dependence of the amplitude of geomagnetic sudden commencements Reviewed

Shinbori Atsuki, Tsuji Yuji, Kikuchi Takashi, Araki Tohru, Watari Shinichi

JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS Vol. 114 2009.4

Shinbori A., Tsuji Y., Kikuchi T., Araki T., Watari S.

Journal of Geophysical Research: Space Physics Vol. 114 ( 4 ) 2009.4

Language：Japanese Publishing type：Research paper (scientific journal) Publisher：Journal of Geophysical Research: Space Physics

Statistical analysis of the main impulse (MI) amplitude of geomagnetic sudden commencements (SCs) in a region from the middle latitudes to equator has been made using the long-term geomagnetic field data obtained from the Yap (geomagnetic latitude, θ = 0.38°), Guam (θ = 5.22°), Okinawa (θ = 16.54°), Kakioka (θ = 27.18°), Memanbetsu (θ = 35.16°), and St. Paratunka (θ = 45.58°) stations. The magnetic local time (MLT) dependence of SC amplitude in the middle latitudes showed magnetic field variations produced by two-cell ionospheric currents (DP 2-type currents) which are driven by the dawn-to-dusk electric field accompanying a pair of field-aligned currents (FACs). The effect of the DP 2-type currents at least expands to the low latitude (θ = 16.54°). In this region, the DL part of SC produced by the enhanced Chapman-Ferraro currents can be dominant, but the DP part of SC contaminated 7% of the DL one. On the other hand, at the daytime equator between 8:00 and 16:00 (MLT), the SC amplitude is considerably enhanced with its peak amplitude of 3.24 (normalized SYM-H value) around 11:00 (MLT) due to the Cowling effect. Another interesting point is that the SC amplitude in the nighttime sector was enhanced at all the stations again, and its peak value increases with increasing magnetic latitude. This result suggests that the effect of the FACs associated with the MI phase of SC expands to the equator. Copyright 2009 by the American Geophysical Union.

DOI： 10.1029/2008JA013871

Seasonal variations of the electron density distribution in the polar region during geomagnetically quiet periods near solar maximum Reviewed Open Access

N. Kitamura, A. Shinbori, Y. Nishimura, T. Ono, M. Iizima, A. Kumamoto

Journal of Geophysical Research: Space Physics Vol. 114 ( A1 ) page： n/a - n/a 2009.1

Language：English Publishing type：Research paper (scientific journal) Publisher：American Geophysical Union (AGU)

Meridional electron density distributions above 45 degrees invariant latitude (ILAT) during geomagnetically quiet periods are statistically studied. Electron density data were obtained from plasma waves observed by the Akebono satellite from March 1989 to February 1991 (near solar maximum) in an altitude range of 274-10,500 km. Field-aligned electron density profiles were fitted by the sum of exponential and power law functions. The transition height, where the power law term equals the exponential term, is highest in the summer (at low solar zenith angle (SZA)) at similar to 4000 km and lowest in the winter (at high SZA) at similar to 1800 km in a region of ILAT >= 70 degrees; this is caused by the larger scale height in the summer (similar to 550 km) than that in the winter (similar to 250 km). The largest seasonal variation and SZA dependence of the electron density are found at an altitude of similar to 2000 km with a factor of similar to 50 (similar to 10(4) /cc in the summer, similar to 10(3) /cc in the winter) in the trough, auroral, and polar cap regions. The seasonal variation and SZA dependence are smaller, about a factor of 5-10, above similar to 5000 km. Day-night asymmetries in each season (within a factor of 5) are smaller than the seasonal variation. The scale height is larger in the dayside than in the nightside in each season. These results indicate that photoionization processes in the ionosphere strongly control electron density distributions up to at least similar to 5000 km in the trough, auroral, and polar cap regions.

DOI： 10.1029/2008JA013288