Open AccessPlasma sheet and (nonstorm) ring current formation from solar and polar wind sources
Author(s) -
Moore T. E.,
Fok M.C.,
Chandler M. O.,
Chappell C. R.,
Christon S. P.,
Delcourt D. C.,
Fedder J.,
Huddleston M.,
Liemohn M.,
Peterson W. K.,
Slinker S.
Publication year - 2005
Publication title -
journal of geophysical research: space physics
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 1.67
H-Index - 298
eISSN - 2156-2202
pISSN - 0148-0227
DOI - 10.1029/2004ja010563
Subject(s) - solar wind , ring current , physics , plasma sheet , magnetosphere , polar wind , current sheet , magnetopause , interplanetary magnetic field , heliospheric current sheet , geophysics , polar , proton , computational physics , atmospheric sciences , plasma , atomic physics , magnetohydrodynamics , astronomy , nuclear physics
We consider the formation of the plasma sheet and geosynchronous region (nonstorm) ring current in the framework of collisionless test particle motions in three‐dimensional magnetospheric fields obtained from self‐consistent MHD simulations. Simulation results are compared with observations of the near‐Earth plasma sheet from the Polar spacecraft during 2001 and 2002. Many particles were initiated in two regions representative of the solar wind source upstream of the bow shock and the polar wind source outside the plasmasphere, both of which are dominated by protons (H + ). Proton trajectories are run until they precipitate into the atmosphere, escape from the simulation space, or become stably trapped. These calculations produce a database of proton characteristics in each 1 R E 3 volume element of the magnetosphere and yield velocity distributions as well as bulk plasma properties. We report results reflecting steady growth phase conditions after 45 min of southward interplanetary field, B Z = −5 nT ( B Y = 0), and for conditions resulting after 2 hours of northward B Z = +5 nT. The results for simulated velocity distributions are consistent with the Polar soundings of the current sheet from lobe to lobe and with AMPTE/CCE observations of (nonstorm) ring current region protons. The simulations help us identify the differentiation between solar and polar wind H + ions in observations. The weak NB Z ring current‐like pressure is primarily polar wind protons, while the moderately active SB Z ring current‐like pressure is primarily solar wind protons. The solar and polar wind contributions to the SB Z ring current are comparable in density, but the solar protons have a higher average energy. For SB Z , solar wind protons enter the nonstorm ring current region primarily via the dawn flank and to a lesser degree via the midnight plasma sheet. For NB Z , solar wind protons enter the ring current‐like region via the cusp and flanks. Polar wind protons enter the nonstorm ring current through the midnight plasma sheet in both cases. Solar and ionospheric plasmas thus take different transport paths to the geosynchronous (nonstorm) ring current region and may thus be expected to respond differently to substorm dynamics of the magnetotail.