P. Song1(1-734-764-8327; firstname.lastname@example.org); M. 0. Chandler2;
Moore3; C. T. Russell4; S. S. Stahara5;
J. R. Spreiter5; J.-H. Shue6
1Space Physics Research Lab, University of Michigan, 2455 Hayward, Ann Arbor, MI 48109-2143, United States
2Space Sciences Laboratory, NASA Mail Code ES83, NASA MarshO Space Flight Center, Huntsville, AL 35812, United States
3Interplanetary Physics, Code 692, Bldg.2-Rm 138, NASA Goddard Space Flight Center, Greenbelt, MD 20771, United States
4Institute of Geophysics and Planetary Physics, University of California, 405 Hilgard Ave., Los Angeles, CA 90095, United States
5RMA Aerospace Inc., Mountain View, CA, United States
6Solar-Terrestrial Environment Laboratory, Nagoya University, Toyokawa, Japan
The unusually high solar wind pressure and strongly southward IMF
on May 4, 1998 pushed the magnetopause well into the geosynchronous
orbit, which exposed the POLAR satellite to the magnetosheath and
solar wind. We use a gasdynamic convected field model to predict the
magnetosheath quantities and then compare them with the in situ observations.
The model prediction helps to reduce the uncertainty in
the timing of the solar wind arrival time and provides a reference value
for each physical parameter. It also helps to resolve the location of the
satellite during strong magnetic fluctuations near the magnetopause.
The plasma measurements from the TIDE instrument, in conjunction
with the magnetometer measurements, indicate that there is
a magnetospheric boundary layer during the event. There are also transient
signatures near the magnetopause which may be caused by magnetospheric
flux transfer events.