Japan Geoscience Union Meeting 2016

Presentation information


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

[P-EM19] Heliosphere and Interplanetary Space

Wed. May 25, 2016 1:45 PM - 3:15 PM 302 (3F)

Convener:*Ken Tsubouchi(Tokyo Institute of Technology), Masaki N Nishino(Institute for Space-Earth Environmental Research, Nagoya University), Yasuhiro Nariyuki(Faculty of Human Development, University of Toyama), Chair:Fumiko Otsuka(Interdisciplinary Graduate School of Engineering Sciences Kyushu University)

2:15 PM - 2:30 PM

[PEM19-09] A Statistical Study of the Radial and North-South Component Values of Heliospheric Magnetic Field

*Nishiki Nozaki1, Nobuhiko Nishimura1, Bernard Jackson2, Hsiu-Shan Yu2, Munetoshi Tokumaru1, Ken'ichi Fujiki1, keiji hayashi1, Kazuyuki Hakamada3 (1.Institute for Space-Earth Environmental Research, 2.University of California, San Diego, 3.Chubu University)

Keywords:solar wind, interplanetary magnetic field, space weather, heliosphere

Determination of interplanetary magnetic field (IMF) north-south component of magnetic field (Bz) is important from the space weather perspective because this field interacts with Earth’s magnetic field causing geomagnetic storms. Lyatsky et al. (2003) and Youssef et al. (2011) show that there is a correlation between IMF Bz (south is positive) and the absolute value of the radial field Bx (|Bx|) during solar minima. They find a positive correlation when the dominant solar field has a positive polarity and negative for a dominant negative field polarity. The negative and positive polarities correspond to whether the Sun’s magnetic field in the northern hemisphere is directed toward or away from the Sun, respectively. We calculate the correlation between IMF Bz and |Bx| using the OMNI dataset from 1965 - 2015, and Helios in-situ measurement data from 1975 - 1977. In a similar study, we find that the correlation between Bz and |Bx| shows a sinusoidal variation associated with ~11 year solar cycle, and also that an even more significant correlation between Bz and |Bx| exists for solar distances between 0.3 and 0.4 AU in the Helios measurements. In an ongoing study, we extrapolate the Potential Field Source Surface (PFSS) model [Hakamada, 1998] to the Earth’s location by using the UCSD 3D tomography model [Jackson et al. 2010] and compare the radial component (Br) of modeled magnetic field with the normal (north-south) component (Bn) observed by ACE spacecraft. This study finds a significant positive correlation between Br and Bn (north is positive). Thus, this study strongly suggests that the IMF Bz is generated, not in interplanetary space, but at the corona. In the future, we will study why this correlation between Bz and |Bx| exists.