TY - JOUR
T1 - Substorm-associated shrinkage of the mid-tail magnetosphere
T2 - IACG campaign #2
AU - Kawano, H.
AU - Nakamura, R.
AU - Kokubun, S.
AU - Mukai, T.
AU - Yamamoto, T.
AU - Yumoto, K.
AU - Slavin, J. A.
N1 - Funding Information:
We thank G. Rostoker and G. Reevesf or useful discussions. We also thank the WIND/SWE team for their data,a nd R. Belian and G. Reevesf or LANL energetice lectrond ata. The CANOPUS instrumenta rray was constructeda nd is maintaineda nd operatedb y the Canadian Space Agency for the Canadian scientific community. We also thank the 210” magneticm eridian observationg roup for the groundd ata.
PY - 2000
Y1 - 2000
N2 - In the framework of IACG Campaign #2, we study a case in which the GEOTAIL spacecraft was close to the mid-tail magnetopause when three substorms took place. GEOTAIL was mainly located within the dawnside plasmasheet, and its average speed normal to the nominal magnetopause was very small (∼0.2 R E /hr) because it was near its apogee. It exited to the LLBL∼magnetosheath during the expansion to recovery phases of each substorm, stayed there for a while, and then returned to the plasmasheet near the end of the recovery phase. This pattern suggests a shrinkage of the mid-tail magnetosphere after the expansion onset so that the tail radius becomes smaller than that in the quiet time. We interpret it as a result of strong tailward flows from the near-Earth neutral line which transports plasma in the mid-tail region to the distant tail and causes a rarefaction in the mid-tail region.
AB - In the framework of IACG Campaign #2, we study a case in which the GEOTAIL spacecraft was close to the mid-tail magnetopause when three substorms took place. GEOTAIL was mainly located within the dawnside plasmasheet, and its average speed normal to the nominal magnetopause was very small (∼0.2 R E /hr) because it was near its apogee. It exited to the LLBL∼magnetosheath during the expansion to recovery phases of each substorm, stayed there for a while, and then returned to the plasmasheet near the end of the recovery phase. This pattern suggests a shrinkage of the mid-tail magnetosphere after the expansion onset so that the tail radius becomes smaller than that in the quiet time. We interpret it as a result of strong tailward flows from the near-Earth neutral line which transports plasma in the mid-tail region to the distant tail and causes a rarefaction in the mid-tail region.
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U2 - 10.1016/S0273-1177(99)00685-7
DO - 10.1016/S0273-1177(99)00685-7
M3 - Article
AN - SCOPUS:0040195808
SN - 0273-1177
VL - 25
SP - 1689
EP - 1696
JO - Advances in Space Research
JF - Advances in Space Research
IS - 7-8
ER -