Japan Geoscience Union Meeting 2019

Presentation information

[E] Oral

P (Space and Planetary Sciences ) » P-EM Solar-Terrestrial Sciences, Space Electromagnetism & Space Environment

[P-EM15] Study of coupling processes in solar-terrestrial system

Thu. May 30, 2019 10:45 AM - 12:15 PM A01 (TOKYO BAY MAKUHARI HALL)

convener:Mamoru Yamamoto(Research Institute for Sustainable Humanosphere, Kyoto University), Yasunobu Ogawa(National Institute of Polar Research), Satonori Nozawa(Institute for Space-Earth Environment Research), Akimasa Yoshikawa(Department of Earth and Planetary Sciences, Kyushu University), Chairperson:Satonori Nozawa

11:30 AM - 11:45 AM

[PEM15-09] Characteristics of CME- and CIR-driven ion upflows in the polar ionosphere

*Yasunobu Ogawa1, Kanako Seki2, Kunihiro Keika2, Yusuke Ebihara3 (1.National Institute of Polar Research, 2.School of Science, the University of Tokyo, 3.Research Institute for Sustainable Humanosphere, Kyoto University)

Keywords:polar ionosphere, M-I coupling, EISCAT

We investigated how velocity and flux of ionospheric ion upflows vary during magnetic storms driven by corotating interaction regions (CIRs) and coronal mass ejections (CMEs), using data from the European Incoherent Scatter (EISCAT) Tromsø UHF and Svalbard radars between 1996 and 2015. The characteristics of ion upflows were compared with ion and electron temperature variations measured with the EISCAT radars, and also joule heating rate, electric field, and field-aligned current (FAC) distribution derived from the Weimer model. Upward ion velocity increases in the nighttime at Tromsø (66.2 o N geomagnetic latitude) just after the CIR- and CME-driven storms, corresponding to electron temperature enhancements due to soft particle precipitation and also ion temperature enhancements in the strong westward electric field region. The CME-driven storms have larger upward ion flux (~1.7×1013 m-2s-1) than those under the CIR-driven storms (~0.3×1013 m-2s-1). In the daytime, ion upflows are seen at Longyearbyen, Svalbard (75.2 o N geomagnetic latitude), with an upward flux of typically 1013 m-2s-1 for small CIR and CME storm cases. Substantial ion upflows last for a few days after the storm onsets under small CIR storms, whereas they last for only a day under small CME storms. Under both the cases, the substantial ion upflows are associated with an enhancement of the Region 1 FAC, eastward electric field and Joule heating rate. For large CME storms, substantial ion upflows are absent in the daytime probably due to equatorward expansion of the auroral oval.