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Kinetic instabilities in Mercury's magnetosphere: Three‐dimensional simulation results
Author(s) -
Trávníček Pavel M.,
Hellinger Petr,
Schriver David,
Herčík David,
Slavin James A.,
Anderson Brian J.
Publication year - 2009
Publication title -
geophysical research letters
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.007
H-Index - 273
eISSN - 1944-8007
pISSN - 0094-8276
DOI - 10.1029/2008gl036630
Subject(s) - magnetosheath , magnetopause , physics , magnetosphere , mercury's magnetic field , geophysics , bow wave , bow shock (aerodynamics) , solar wind , plasma , equator , shock wave , computational physics , mechanics , interplanetary magnetic field , astronomy , quantum mechanics , latitude
A self‐consistent global three‐dimensional kinetic study of Mercury's magnetosphere is carried out examining waves and instabilities generated by ion temperature anisotropy and plasma flow. The overall structure of Mercury's upstream bow shock and magnetosheath are qualitatively very similar to those of Earth. Beam‐generated long‐wavelength oscillations are present upstream of Mercury's quasi‐parallel bow shock, whereas large‐amplitude mirror waves develop downstream of the quasi‐parallel bow shock in the magnetosheath. A train of mirror waves forms also downstream of the quasi‐perpendicular bow shock. A velocity shear near the magnetopause can lead to formation of vortex‐like structures. The magnetospheric cavity close to the planet's equatorial plane is filled with ions much hotter than the solar wind protons. A drift‐driven plasma belt close to the equator is present in the model and contains plasma with high‐temperature anisotropy, and the loss cone for charged particles in this region is large. The belt may cause diamagnetic effects superimposed on the planet's internal magnetic field and can interact with Mercury's magnetopause.