JpGU-AGU Joint Meeting 2017

Presentation information

[EE] Oral

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

[P-EM14] [EE] Dynamics in magnetosphere and ionosphere

Sun. May 21, 2017 9:00 AM - 10:30 AM 105 (International Conference Hall 1F)

convener:Tomoaki Hori(Graduate school of Science, University of Tokyo), Yoshimasa Tanaka(National Institute of Polar Research), Aoi Nakamizo(Applied Electromagnetic Research Institute, National Institute of Information and Communications Technology), Mitsunori Ozaki(Faculty of Electrical and Computer Engineering, Institute of Science and Engineering, Kanazawa University), Chairperson:Atsuki Shinbori(ISEE, Nagoya Univ.), Chairperson:Shin'ya Nakano(The Institute of Statistical Mathematics), Chairperson:Shin-ichiro Oyama(ISEE, Nagoya Univ.)

9:45 AM - 10:00 AM

[PEM14-15] Response of the Earth’s magnetosphere and ionosphere to the small-scale magnetic flux rope in solar wind by the MHD simulation

*Kyung Sun Park1, Myeong Joon Kim1, Dae-Young Lee1, Kyungsuk Cho2, Rok Soon Kim2, Tatsuki Ogino3 (1.Chungbuk National University, Korea, 2.Korea Astronomy and Space Science Institute, Korea, 3.ISEE, Nagoya University, Japan)

Keywords:small-scale magnetic flux rope, magnetosphere and ionosphere , cross polar cap potential

We have studied the response of the Earth’s magnetosphere and ionosphere to two cases of small-scale magnetic flux ropes in solar wind by using a three-dimensional global MHD simulation. (1) the case of +Z axis of magnetic flux rope, the IMF is northward with a dawn to dusk BY components as right-handed, (2) the case of +Y axis of magnetic flux rope, the IMF is north to southward with a duskward BY as right-handed and solar wind dynamic pressure is normal (1.3 nPa).
The simulation results show that the bow shock is located at about 14.6 RE and the magnetopause is located at about 10.24 RE in both cases. However, ionospheric phenomena show the different feature for two cases. The cross polar cap potential becomes small during the northward even though magnitude of magnetic field becomes large for +Z axis of magnetic flux rope. And the cross polar cap potential increase that is governed by magnitude of magnetic field as well as southward BZ for +Y axis of magnetic flux rope.