Open AccessSolar wind interaction with the ionosphere/atmosphere and crustal magnetic fields at Mars: Mars Global Surveyor Magnetometer/Electron Reflectometer, radio science, and accelerometer data
Author(s) -
Krymskii A. M.,
Ness N. F.,
Crider D. H.,
Breus T. K.,
Acuña M. H.,
Hinson D. P.
Publication year - 2004
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 - 10.1029/2004ja010420
Subject(s) - ionosphere , geophysics , atmosphere (unit) , solar wind , atmospheric sciences , mars exploration program , atmosphere of mars , geology , interplanetary magnetic field , martian , northern hemisphere , physics , magnetic field , meteorology , astrobiology , quantum mechanics
The solar wind (SW) mainly interacts with the Martian ionosphere/atmosphere. However, the intense crustal magnetization creates localized minimagnetospheres above the surface. The interplanetary magnetic field (IMF) can reconnect with these crustal fields and this allows SW and more energetic particles to precipitate into and heat the neutral atmosphere in localized regions, especially in the southern hemisphere. A study of 907 electron density profiles obtained by the MGS Radio Science (RS) experiment at latitudes from +63° to +77° and 219 profiles at latitudes −69° to −64.5° has been conducted. The role of the magnetic field as a driving force of the cross‐terminator convection is discussed. Longitudinal variations of neutral atmosphere scale height H peak derived from the MGS RS data have been analyzed. Ionospheric parameters are found to be more variable in the southern than in the northern hemisphere. This correlates well with the variability of the magnetic field direction from local zenith. The scale height of neutral atmosphere density H ACC derived from the MGS accelerometer data is also found to be more variable in the southern than in the northern hemisphere.