Estimation of the escape of photoelectrons from Mars in 2004 liberated by the ionization of carbon dioxide and atomic oxygen

Frahm, R. A.; Sharber, J. R.; Winningham, J. D.; Link, R.; Liemohn, Michael W.; Kozyra, J. U.; Coates, A. J.; Linder, Dietmar; Barabash, S.; Lundin, R.; Fedorov, A.

doi:10.1016/j.icarus.2009.03.024

Cited by 40 publications

(45 citation statements)

References 26 publications

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“…Open field lines provide pathways on which planetary ions can be accelerated and escape into space (Dubinin et al, 2012;Ergun et al, 2006;Frahm et al, 2010;Lillis et al, 2015Lillis et al, , 2017, whereas closed field lines can trap ionospheric plasma (Andrews et al, 2015;Brain et al, 2007;Flynn et al, 2017;. Open field lines provide pathways on which planetary ions can be accelerated and escape into space (Dubinin et al, 2012;Ergun et al, 2006;Frahm et al, 2010;Lillis et al, 2015Lillis et al, , 2017, whereas closed field lines can trap ionospheric plasma (Andrews et al, 2015;Brain et al, 2007;Flynn et al, 2017;.…”

Section: Discussionmentioning

confidence: 99%

Magnetic Reconnection on Dayside Crustal Magnetic Fields at Mars: MAVEN Observations

Harada

Halekas

DiBraccio

et al. 2018

Geophysical Research Letters

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The identification of magnetic reconnection on the dayside of Mars has been elusive owing to the lack of comprehensive plasma and field measurements. Here we present direct measurements of dayside in situ reconnection signatures by the comprehensive particles and fields package on board the Mars Atmosphere and Volatile EvolutioN (MAVEN) spacecraft over strong crustal magnetic fields in the southern hemisphere of Mars. During a crossing of a bifurcated current sheet consisting of northward and southward magnetic fields, MAVEN recorded (i) ionospheric photoelectrons trapped on closed magnetic field lines, (ii) Hall magnetic fields and a nonzero normal field with polarity consistent with a crossing northward of the X line, and (iii) northward Alfvénic ion jets. Dayside magnetic reconnection on crustal magnetic fields could control the global configuration and topology of the Martian magnetosphere and alter the ion escape pattern from the dayside ionosphere.

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Section: Discussionmentioning

confidence: 99%

Magnetic Reconnection on Dayside Crustal Magnetic Fields at Mars: MAVEN Observations

Harada

Halekas

DiBraccio

et al. 2018

Geophysical Research Letters

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“…Photoelectrons occupy a large region which approximately coincides with the magnetic pile-up region (MPR) adjacent to the induced magnetospheric boundary. Frahm et al (2010) have estimated the escape fluxes of these photoelectrons as ∼4 × 10 6 cm −2 s −1 and the total losses to match the escape of the suprathermal electrons to be 3 × 10 23 s −1 . Since only 'peaked' electrons could be traced and referred to polar wind, this value should be regarded only as the lower limit of polar wind losses.…”

Section: Polar Windmentioning

confidence: 99%

Ion Energization and Escape on Mars and Venus

Dubinin

Fräenz

Fedorov³

et al. 2011

Space Sci Rev

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167

174

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Mars and Venus do not have a global magnetic field and as a result solar wind interacts directly with their ionospheres and upper atmospheres. Neutral atoms ionized by solar UV, charge exchange and electron impact, are extracted and scavenged by solar wind providing a significant loss of planetary volatiles. There are different channels and routes through which the ionized planetary matter escapes from the planets. Processes of ion energization driven by direct solar wind forcing and their escape are intimately related. Forces responsible for ion energization in different channels are different and, correspondingly, the effectiveness of escape is also different. Classification of the energization processes and escape channels on Mars and Venus and also their variability with solar wind parameters is the main topic of our review. We will distinguish between classical pickup and 'massloaded' pickup processes, energization in boundary layer and plasma sheet, polar winds on unmagnetized planets with magnetized ionospheres and enhanced escape flows from localized auroral regions in the regions filled by strong crustal magnetic fields.

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“…However, photoelectrons observed close to Mars on the dayside might be locally produced whereas those in the downstream sector, far from Mars might likely photoelectrons travelling along draped field lines connected to the ionosphere (Frahm et al 2006). Unfortunately ASPERA-3 ELS cannot discriminate between locally produced and transported photoelectrons (Frahm et al 2010).…”

Section: The Photoelectron Boundary (Peb)mentioning

confidence: 99%

The Induced Magnetospheres of Mars, Venus, and Titan

et al. 2011

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This article summarizes and aims at comparing the main features of the induced magnetospheres of Mars, Venus and Titan. All three objects form a well-defined induced magnetosphere (IM) and magnetotail as a consequence of the interaction of an external wind of plasma with the ionosphere and the exosphere of these objects. In all three, photoionization seems to be the most important ionization process. In all three, the IM displays a clear outer boundary characterized by an enhancement of magnetic field draping and massloading, along with a change in the plasma composition, a decrease in the plasma temperature, a deflection of the external flow, and, at least for Mars and Titan, an increase of the total density. Also, their magnetotail geometries follow the orientation of the upstream magnetic field and flow velocity under quasi-steady conditions. Exceptions to this are fossil fields observed at Titan and the near Mars regions where crustal fields dominate the magnetic topology. Magnetotails also concentrate the escaping plasma flux from these three objects and similar acceleration mechanisms are thought to be at work. In the case of Mars and Titan, global reconfiguration of the magnetic field topology (reconnection with the crustal sources and exits into Saturn's magnetosheath, respectively) may lead to important losses of C. Bertucci ( )

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Estimation of the escape of photoelectrons from Mars in 2004 liberated by the ionization of carbon dioxide and atomic oxygen

Cited by 40 publications

References 26 publications

Magnetic Reconnection on Dayside Crustal Magnetic Fields at Mars: MAVEN Observations

Magnetic Reconnection on Dayside Crustal Magnetic Fields at Mars: MAVEN Observations

Ion Energization and Escape on Mars and Venus

The Induced Magnetospheres of Mars, Venus, and Titan

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