2006
DOI: 10.1016/j.icarus.2005.10.036
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Numerical interpretation of high-altitude photoelectron observations

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Cited by 56 publications
(61 citation statements)
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“…Since this pilot study uses only one ELS sector (sector 3), it is possible that the difference in aspect resulting from different spacecraft observational modes might affect our statistics. It has been demonstrated that the measurement of flows can be very aspect sensitive at large distances from the planet [Frahm et al, 2006;Liemohn et al, 2006a]. The slightly reduced occurrence percentages in the region near -0.75 R M < X < -0.25 R M of Figure 5 could be an indication of this, as this is the region where MEX often maneuvers into the ELS radial measurement configuration.…”
Section: Instrumentmentioning
confidence: 94%
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“…Since this pilot study uses only one ELS sector (sector 3), it is possible that the difference in aspect resulting from different spacecraft observational modes might affect our statistics. It has been demonstrated that the measurement of flows can be very aspect sensitive at large distances from the planet [Frahm et al, 2006;Liemohn et al, 2006a]. The slightly reduced occurrence percentages in the region near -0.75 R M < X < -0.25 R M of Figure 5 could be an indication of this, as this is the region where MEX often maneuvers into the ELS radial measurement configuration.…”
Section: Instrumentmentioning
confidence: 94%
“…(During 2004 the MEX apoapsis changed from an altitude of ~11,600 km to ~10,100 km and periapsis changed from ~270 km to ~260 km in mid year to ~300 km at the end of the year.) In an effort to understand how these photoelectrons reach the large distances, Liemohn et al (2006a) used ELS photoelectron observations and simulations with a global MHD code [Ma et al, 2002; to study the likely paths of the electrons detected by the spacecraft. Two of the three cases studied indicated that the photoelectrons were produced on open field lines connecting to the planet in the afternoon/evening sector, while the third suggested that the photoelectrons were observed on interplanetary field lines draping the planet.…”
Section: Locations Of Atmospheric Photoelectron Energy Peaks Within Tmentioning
confidence: 99%
“…Above 200 km photoelectrons can be transported and contribute to an electron escape flux. Note that for closed crustal magnetic field lines the upward electrons would reenter the ionosphere as a down flux [Liemohn et al, 2006], but we do not consider this case in our paper. Figure 3a shows a comparison of our model fluxes with SWEA fluxes for case 1 (1 April 2015).…”
Section: Resultsmentioning
confidence: 99%
“…Photoelectrons were first measured in the Martian ionosphere by the Viking Retarding Potential Analyzer [Mantas and Hanson, 1979]. The magnetotail can also act as a source of suprathermal electrons for the ionosphere if the magnetic topology is favorable [Liemohn et al, 2006]. Ions and electrons from the solar wind that make it past the magnetic pileup region can also deposit energy in the upper atmosphere [Crider et al, 2004].…”
Section: Introductionmentioning
confidence: 99%
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