To C. T. Russell's page
The importance of the magnetosheath is only now being gradually recognized. Terrestrial researchers often relate the properties of the solar wind to processes occurring within the magnetosphere. Seldom do they take into account that these properties are modified crossing the shock and flowing through the magnetosheath to the magnetopause. In particular, the Mach number of the solar wind affects the temperature of the magnetosheath and hence the plasma beta there. Beta in turn is known to control the rate of reconnection as measured by the strength of accelerated flows at the magnetopause. The shock and magnetosheath can also affect waves connected to the magnetosheath through mode coupling and damping. Unfortunately, few researchers have attempted detailed studies of the high beta, non-linear plasma processes of the magnetosheath. It was hoped that this workshop could encourage such activity.
In closing I would like to thank the session chairmen and referees who worked hard at the meeting and afterwards, reviewing these manuscripts, and whose efforts permitted the timely production of this volume: N. U. Crooker, C. Farrugia, D. G. Sibeck and P. Song.
I would like to thank Z. Niemirowicz and his COSPAR staff for once again providing excellent support for the symposium and to thank the local organizers, especially R. Hart, for arranging such an excellent meeting. Finally, I am extremely grateful for the efforts of my own staff at UCLA in particular Lynda Kim and Angela McKnight who assisted with correspondence prior to the meeting and afterward. All this assistance made my job much easier.
Christopher T. Russell
Institute of Geophysics and Planetary Physics
Department of Earth and Space Sciences
University of California, Los Angeles
March, 1993
Page 1: preface
Page 5: Gasdynamic and Magnetohydrodynamic Modeling of the Magnetosheath: A Tutorial; J. R. Spreiter and S. S. Stahara
Page 21: MHD Simulations of the Magnetosheath; J. G. Lyon
Page 31: Ion Distribution Function in the Magnetosheath: Fine Structure; J. Safrankova, Z. Nemecek and O. Santolik
Page 35: Simulation of Shell Like Heavy Ion Distributions Downstream of the Bow Shock; U. Motschmann and K. H. Glassmeier
Page 39: Medium Energy Particle Perspective From Magnetopause to Upstream Region: Prognoz-10 Data; K. Kudela, D. G. Sibeck M. Slivka, D. Venkatesan, S. Fischer and V. N. Lutsenko
Page 45: Sources of Magnetosheath Waves and Turbulence; N. Omidi, A. O'Farrell and D. Krauss-Varban
Page 55: Nature and Origin of Wave Modes in the Dayside Earth Magnetosheath; D. Hubert
Page 65: Mirror Instability in the Magnetosheath; A. N. Fazakerley and D. J. Southwood
Page 71: ISEE Observations of the Dayside Magnetosheath; P. Song
Page 81: The Solar Wind Flow Along the Subsolar Line in the Magnetic Barrier and Reconnection at the Magnetopause; N. V. Erkaev, A. V. Mezentsev, H. K Biernat, B. P. Besser, G. A. Bachmaier, V. S. Semenov, R. P. Rijnbeek and C. J. Farrugia
Page 87: Depletion as a Signature of Interconnection; N. U. Crooker
Page 91: Magnetosheath Magnetic Field Variability; D. G. Sibeck
Page 95: Consequences of Magnetohydrodynamic Processes for Large Scale Flow in the Magnetosheath; M. C. Kivelson, S.H. Chen and D. J. Southwood
Page 105: Observations in the Sheath Region Ahead of a Magnetic Cloud and in the Dayside Magnetosheath During Magnetic Cloud Passage; C. J. Farrugia, R. J. Fitzenreiter, L. F. Burlaga, N. V. Erkaev, V. A. Osherovich, H. K Biernat and A. Fazakerley
Page 113: Chaotic Phenomenon in the Magnetopause Plasma; N.Q. Wang and X.-X. Zhang
Page 123: Fractal Clusters in the Solar Wind; A. V. Milovanov and L. M. Zelenyi
Page 135: Author Index