Abstract
AbstractSince Mars lacks a global intrinsic magnetic field, the solar wind interacts directly with the Martian upper atmosphere and ionosphere. The presence of localized intense remnant crustal magnetic fields adds to this interaction, making the Martian plasma system a unique environment within the solar system. Rapid reductions in the electron flux, referred to as “electron holes,” occur within the Martian induced magnetosphere (IM). We present a statistical analysis of this phenomenon identified from proxy measurements of the electron flux derived from measurements by the Analyser of Space Plasmas and Energetic Neutral Atoms Electron Spectrometer experiment on board the Mars Express (MEX) spacecraft. The study is completed for the period of 9 February 2004 to 9 May 2014. Electron holes are observed within the IM in more than 56% of MEX orbits during this study period, occurring predominantly at altitudes less than 1300 km, with the majority in the negative X Mars‐Centric Solar Orbital direction. The spatial distribution above the surface of Mars is observed to bear close resemblance to that of the crustal magnetic fields as predicted by the Cain et al. [] magnetic field model, suggesting that they play an important role in the formation of these phenomena.
Highlights
Mars lacks an intrinsic global magnetic field, so it is the Martian upper atmosphere and ionosphere that interact directly with the solar wind and interplanetary magnetic field (IMF)
We present a statistical analysis of this phenomenon identified from proxy measurements of the electron flux derived from measurements by the Analyser of Space Plasmas and Energetic Neutral Atoms Electron Spectrometer experiment on board the Mars Express (MEX) spacecraft
The objective of this paper is to present a study of rapid reductions in electron flux within the Martian induced magnetosphere (IM) by doing a more exhaustive analysis of the occurrence of such reductions using the MEX Analyser of Space Plasmas and Energetic Neutrals Electron Spectrometer (ASPERA-3 ELS) instrument [Barabash et al, 2006]
Summary
Mars lacks an intrinsic global magnetic field, so it is the Martian upper atmosphere and ionosphere that interact directly with the solar wind and interplanetary magnetic field (IMF). Missions such as the NASA Mars Global Surveyor (MGS, 1996–2006) spacecraft and the European Space Agency (ESA) Mars Express (MEX, 2003 up to present) spacecraft have been used for almost two decades to characterize the intricacies of the Martian plasma system During this time, variations have been observed in measurements of quantities such as the electron flux and derived plasma moments [e.g., Mitchell et al, 2001; Soobiah et al, 2006; Brain et al, 2007; Duru et al, 2011], as well as apparent large-scale changes in the structure of the ionosphere associated with the crustal magnetic fields [e.g., Lundin et al, 2011; Nilsson et al, 2011; Andrews et al, 2013, 2014; Dubinin et al, 2012]. The description of the phenomenon is highly influenced by the nature of the measuring instrument
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