Japan Geoscience Union Meeting 2014

Presentation information

Oral

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

[P-EM34_1PM1] Plasma Astrophysics: interstellar/interplanetary space, magnetosphere

Thu. May 1, 2014 2:15 PM - 4:00 PM 503 (5F)

Convener:*Shuichi Matsukiyo(Department of Earth System Science and Technology, Kyushu University), Yasuhiro Nariyuki(Faculty of Human Development, University of Toyama), Chair:Yasuhiro Nariyuki(Faculty of Human Development, University of Toyama)

2:15 PM - 2:30 PM

[PEM34-05] Dependence of Jovian Magnetopause Location on Solar Wind Dynamic Pressure

*Hirotaka KITAGAWA1, Satoshi KASAHARA2, Chihiro TAO3, Tomoki KIMURA2, Masaki FUJIMOTO2 (1.Earth and Planetary Science, School of Science, University of Tokyo, 2.Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3.Research Institute in Astrophysics and Planetology)

Keywords:Jovian Magnetopause, Solar Wind Dynamic Pressure

Past observations revealed that the probability density distribution of Jovian magnetopause stand-off distance has double-peak. The probability between two peaks is very low. Thus the stand-off distance of Jovian magnetopause changes from the peak distance to the other peak by solar wind dynamic pressure. However, the scatter plot of stand-off distance versus solar wind dynamic pressure was nearly on one line. But the solar wind dynamic pressure was considered by magnetic pressure in the Jovian magnetosphere, due to the absence of the solar wind monitor at the Jovian orbit. We approached the double-peaked distribution by using the calculated solar wind parameters via MHD equations whose input parameters are based on the observation at Earth's orbit. Referring the propagated solar wind parameters, we investigated the location of Jovian magnetopause observed by the Galileo spacecraft. We found that the peaks of the distribution seem to be a result of probability density distribution of solar wind dynamic pressure. The very low probability stand-off distance between the peaks seemed to be caused by unusual distribution of solar wind dynamic pressure.