TY - JOUR
T1 - Type-II entry of solar wind protons into the lunar wake
T2 - Effects of magnetic connection to the night-side surface
AU - Nishino, Masaki N.
AU - Fujimoto, Masaki
AU - Saito, Yoshifumi
AU - Tsunakawa, Hideo
AU - Kasahara, Yoshiya
AU - Kawamura, Mariko
AU - Matsushima, Masaki
AU - Takahashi, Futoshi
AU - Shibuya, Hidetoshi
AU - Shimizu, Hisayoshi
AU - Goto, Yoshitaka
AU - Hashimoto, Kozo
AU - Omura, Yoshiharu
AU - Kumamoto, Atsushi
AU - Ono, Takayuki
AU - Yokota, Shoichiro
PY - 2013/10
Y1 - 2013/10
N2 - Our recent observations around the Moon revealed that so-called type-II (T2) entry of the solar wind protons into the near-Moon wake occurs when the IMF is dominated by the non-radial components (i.e. BY and/or B z). Under this condition a part of the solar wind protons scattered/reflected at the lunar dayside surface subsequently enters the central region of the near-Moon wake after a large-scale cycloid motion, which accelerates electrons along the filed line into the wake. The situation handled in the previous studies is that the relevant magnetic field line is detached from the lunar surface, leaving a possibility of the T2 entry under magnetic connection left open. Here we report that the protons can access the central wake region that is magnetically connected to the lunar nightsicle surface, which we categorize into the T2 entry with magnetic connection to the lunar surface (T2MC). Furthermore we show that the energy of the electron beams induced by the proton entry into the wake depends on the magnetic connectivity. Strong electron acceleration (up to several hundred eV to 1 keV) along the magnetic field associated with the T2 entry is prominent when the field line has its both ends in the solar wind, that is, when the magnetic field is detached from the lunar surface (i.e. the previously reported T2 entry that we rename toT2MD). On the other hand, no significant electron acceleration is found in the T2MC cases, although an enhancement of the electron flux associated with the T2 proton entry is evident. We also report that the T2 entry process takes place even under radial (Bx-dominated) IMF condition. Our results indicate that, while the T2 entry of solar wind protons into the wake itself does not require a special IMF condition but is a rather general phenomenon, the characteristic energy of associated electrons does show a strong dependence on the magnetic connectivity to the lunar surface.
AB - Our recent observations around the Moon revealed that so-called type-II (T2) entry of the solar wind protons into the near-Moon wake occurs when the IMF is dominated by the non-radial components (i.e. BY and/or B z). Under this condition a part of the solar wind protons scattered/reflected at the lunar dayside surface subsequently enters the central region of the near-Moon wake after a large-scale cycloid motion, which accelerates electrons along the filed line into the wake. The situation handled in the previous studies is that the relevant magnetic field line is detached from the lunar surface, leaving a possibility of the T2 entry under magnetic connection left open. Here we report that the protons can access the central wake region that is magnetically connected to the lunar nightsicle surface, which we categorize into the T2 entry with magnetic connection to the lunar surface (T2MC). Furthermore we show that the energy of the electron beams induced by the proton entry into the wake depends on the magnetic connectivity. Strong electron acceleration (up to several hundred eV to 1 keV) along the magnetic field associated with the T2 entry is prominent when the field line has its both ends in the solar wind, that is, when the magnetic field is detached from the lunar surface (i.e. the previously reported T2 entry that we rename toT2MD). On the other hand, no significant electron acceleration is found in the T2MC cases, although an enhancement of the electron flux associated with the T2 proton entry is evident. We also report that the T2 entry process takes place even under radial (Bx-dominated) IMF condition. Our results indicate that, while the T2 entry of solar wind protons into the wake itself does not require a special IMF condition but is a rather general phenomenon, the characteristic energy of associated electrons does show a strong dependence on the magnetic connectivity to the lunar surface.
KW - Lunar plasma environment
KW - Lunar wake
KW - Selene (kaguya)
KW - Solar wind-moon interaction
KW - Wave particle interaction
UR - http://www.scopus.com/inward/record.url?scp=84888356707&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=84888356707&partnerID=8YFLogxK
U2 - 10.1016/j.pss.2013.08.017
DO - 10.1016/j.pss.2013.08.017
M3 - Article
AN - SCOPUS:84888356707
SN - 0032-0633
VL - 87
SP - 106
EP - 114
JO - Planetary and Space Science
JF - Planetary and Space Science
ER -