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Electric and magnetic variations in the near-Mars environment

Fowler, C. M. (author)
University of Colorado Boulder, Laboratory for Atmospheric and Space Physics
Andersson, L. (author)
University of Colorado Boulder, Laboratory for Atmospheric and Space Physics
Halekas, J. (author)
University Of Iowa, Department of Physics And Astronomy
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Espley, J. R. (author)
NASA, Goddard Space Flight Center
Mazelle, C. (author)
University of Toulouse, CNRS, UPS, IRAP,CNES
Coughlin, E. R. (author)
University of California Berkeley, Department Astronomy; University of California Berkeley, Theoretical Astrophysics Center; Einstein Fellow
Ergun, R. E. (author)
University of Colorado Boulder, Laboratory for Atmospheric and Space Physics
Andrews, David J. (author)
Uppsala universitet,Institutet för rymdfysik, Uppsalaavdelningen
Connerney, J. E. P. (author)
NASA, Goddard Space Flight Center
Jakosky, B. (author)
University of Colorado Boulder, Laboratory for Atmospheric and Space Physics
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 (creator_code:org_t)
2017
2017
English.
In: Journal of Geophysical Research - Space Physics. - 2169-9380 .- 2169-9402. ; 122:8, s. 8536-8559
Related links:
https://urn.kb.se/re...
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https://doi.org/10.1...
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  • Journal article (peer-reviewed)
Abstract Subject headings
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  • For the first time at Mars the statistical distribution of (1-D) electric field wave power in the magnetosphere is presented, along with the distribution of magnetic field wave power, as observed by the Mars Atmosphere and Volatile EvolutioN spacecraft from the first 14.5months of the mission. Wave power in several different frequency bands was investigated, and the strongest wave powers were observed at the lowest frequencies. The presented statistical studies suggest that the full thermalization of ions within the magnetosheath does not appear to occur, as has been predicted by previous studies. Manual inspection of 140 periapsis passes on the dayside shows that Poynting fluxes (at 2-16 Hz) between similar to 10(-11) and 10(-8) Wm(-2) reach the upper ionosphere for all 140 cases. Wave power is not observed in the ionosphere for integrated electron densities greater than 10(10.8)cm(-2), corresponding to typical depths of 100-200 km. The observations presented support previous suggestions that energy from the Mars-solar wind interaction can propagate into the upper ionosphere and may provide an ionospheric heating source. Upstream of the shock, the orientation of the solar wind interplanetary magnetic field was shown to significantly affect the statistical distribution of wave power, based on whether the spacecraft was likely magnetically connected to the shock or not-something that is predicted but has not been quantitatively shown at Mars before. In flight performance and caveats of the Langmuir Probe and Waves electric field power spectra are also discussed.

Subject headings

NATURVETENSKAP  -- Fysik -- Astronomi, astrofysik och kosmologi (hsv//swe)
NATURAL SCIENCES  -- Physical Sciences -- Astronomy, Astrophysics and Cosmology (hsv//eng)

Keyword

magnetic
electric
wave
power
Mars
MAVEN

Publication and Content Type

ref (subject category)
art (subject category)

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