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Locations of Atmospheric Photoelectron Energy Peaks Within the Mars Environment

By identifying peaks in the photoelectron spectrum produced by photoionization of CO2 in the Martian atmosphere, we have conducted a pilot study to determine the locations of these photoelectrons in the space around Mars. The significant result of this study is that these photoelectrons populate a r... Full description

Journal Title: Space science reviews 2007-03-20, Vol.126 (1-4), p.389-402
Main Author: Frahm, R A
Other Authors: Sharber, J R , Winningham, J D , Wurz, P , Liemohn, M W , Kallio, E , Yamauchi, M , Lundin, R , Barabash, S , Coates, A J , Linder, D R , Kozyra, J U , Holmstrom, M , Jeffers, S J , Andersson, H , McKenna-Lawler, S
Format: Electronic Article Electronic Article
Language: English
Subjects:
Publisher: Springer
ID: ISSN: 0038-6308
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recordid: cdi_proquest_miscellaneous_29318903
title: Locations of Atmospheric Photoelectron Energy Peaks Within the Mars Environment
format: Article
creator:
  • Frahm, R A
  • Sharber, J R
  • Winningham, J D
  • Wurz, P
  • Liemohn, M W
  • Kallio, E
  • Yamauchi, M
  • Lundin, R
  • Barabash, S
  • Coates, A J
  • Linder, D R
  • Kozyra, J U
  • Holmstrom, M
  • Jeffers, S J
  • Andersson, H
  • McKenna-Lawler, S
subjects:
  • Mars (Planet)
ispartof: Space science reviews, 2007-03-20, Vol.126 (1-4), p.389-402
description: By identifying peaks in the photoelectron spectrum produced by photoionization of CO2 in the Martian atmosphere, we have conducted a pilot study to determine the locations of these photoelectrons in the space around Mars. The significant result of this study is that these photoelectrons populate a region around Mars bounded externally by the magnetic pileup boundary, and internally by the lowest altitude of our measurements (-250 km) on the dayside and by a cylinder of approximately the planetary radius on the nightside. It is particularly noteworthy that the photoelectrons on the nightside are observed from the terminator plane tailward to a distance of - 3 RM, the Mars Express apoapsis. The presence of the atmospherically generated photoelectrons on the nightside of Mars may be explained by direct magnetic field line connection between the nightside observation locations and the Martian dayside ionosphere. Thus the characteristic photoelectron peaks may be used as tracers of magnetic field lines for the study of the magnetic field configuration and particle transport in the Martian environment.
language: eng
source:
identifier: ISSN: 0038-6308
fulltext: no_fulltext
issn:
  • 0038-6308
  • 1572-9672
url: Link


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titleLocations of Atmospheric Photoelectron Energy Peaks Within the Mars Environment
creatorFrahm, R A ; Sharber, J R ; Winningham, J D ; Wurz, P ; Liemohn, M W ; Kallio, E ; Yamauchi, M ; Lundin, R ; Barabash, S ; Coates, A J ; Linder, D R ; Kozyra, J U ; Holmstrom, M ; Jeffers, S J ; Andersson, H ; McKenna-Lawler, S
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descriptionBy identifying peaks in the photoelectron spectrum produced by photoionization of CO2 in the Martian atmosphere, we have conducted a pilot study to determine the locations of these photoelectrons in the space around Mars. The significant result of this study is that these photoelectrons populate a region around Mars bounded externally by the magnetic pileup boundary, and internally by the lowest altitude of our measurements (-250 km) on the dayside and by a cylinder of approximately the planetary radius on the nightside. It is particularly noteworthy that the photoelectrons on the nightside are observed from the terminator plane tailward to a distance of - 3 RM, the Mars Express apoapsis. The presence of the atmospherically generated photoelectrons on the nightside of Mars may be explained by direct magnetic field line connection between the nightside observation locations and the Martian dayside ionosphere. Thus the characteristic photoelectron peaks may be used as tracers of magnetic field lines for the study of the magnetic field configuration and particle transport in the Martian environment.
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descriptionBy identifying peaks in the photoelectron spectrum produced by photoionization of CO2 in the Martian atmosphere, we have conducted a pilot study to determine the locations of these photoelectrons in the space around Mars. The significant result of this study is that these photoelectrons populate a region around Mars bounded externally by the magnetic pileup boundary, and internally by the lowest altitude of our measurements (-250 km) on the dayside and by a cylinder of approximately the planetary radius on the nightside. It is particularly noteworthy that the photoelectrons on the nightside are observed from the terminator plane tailward to a distance of - 3 RM, the Mars Express apoapsis. The presence of the atmospherically generated photoelectrons on the nightside of Mars may be explained by direct magnetic field line connection between the nightside observation locations and the Martian dayside ionosphere. Thus the characteristic photoelectron peaks may be used as tracers of magnetic field lines for the study of the magnetic field configuration and particle transport in the Martian environment.
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abstractBy identifying peaks in the photoelectron spectrum produced by photoionization of CO2 in the Martian atmosphere, we have conducted a pilot study to determine the locations of these photoelectrons in the space around Mars. The significant result of this study is that these photoelectrons populate a region around Mars bounded externally by the magnetic pileup boundary, and internally by the lowest altitude of our measurements (-250 km) on the dayside and by a cylinder of approximately the planetary radius on the nightside. It is particularly noteworthy that the photoelectrons on the nightside are observed from the terminator plane tailward to a distance of - 3 RM, the Mars Express apoapsis. The presence of the atmospherically generated photoelectrons on the nightside of Mars may be explained by direct magnetic field line connection between the nightside observation locations and the Martian dayside ionosphere. Thus the characteristic photoelectron peaks may be used as tracers of magnetic field lines for the study of the magnetic field configuration and particle transport in the Martian environment.
pubSpringer
doi10.1007/s11214-006-9119-5