Numerical interpretation of high-altitude photoelectron observations

Michael W. Liemohn; R. A. Frahm; J. D. Winningham; Y. Ma; S. Barabash; R. Lundin; J. U. Kozyra; A. F. Nagy; S. M. Bougher; J. Bell; D. Brain; D. Mitchell; J. Luhmann; M. Holmström; H. Andersson; M. Yamauchi; A. Grigoriev; S. McKenna-Lawler; J. R. Sharber; J. R. Scherrer; S. J. Jeffers; A. J. Coates; D. R. Linder; D. O. Kataria; E. Kallio; H. Koskinen; T. Säles; P. Riihelä; W. Schmidt; E. Roelof; D. Williams; S. Livi; C. C. Curtis; K. C. Hsieh; B. R. Sandel; M. Grande; M. Carter; J. A. Sauvaud; A. Fedorov; J. J. Thocaven; S. Orsini; R. Cerulli-Irelli; M. Maggi; P. Wurz; P. Bochsler; N. Krupp; J. Woch; M. Fränz; K. Asamura; C. Dierker

doi:10.1016/j.icarus.2005.10.036

Numerical interpretation of high-altitude photoelectron observations

Michael W. Liemohn, R. A. Frahm, J. D. Winningham, Y. Ma, S. Barabash, R. Lundin, J. U. Kozyra, A. F. Nagy, S. M. Bougher, J. Bell, D. Brain, D. Mitchell, J. Luhmann, M. Holmström, H. Andersson, M. Yamauchi, A. Grigoriev, S. McKenna-Lawler, J. R. Sharber, J. R. ScherrerS. J. Jeffers, A. J. Coates, D. R. Linder, D. O. Kataria, E. Kallio, H. Koskinen, T. Säles, P. Riihelä, W. Schmidt, E. Roelof, D. Williams, S. Livi, C. C. Curtis, K. C. Hsieh, B. R. Sandel, M. Grande, M. Carter, J. A. Sauvaud, A. Fedorov, J. J. Thocaven, S. Orsini, R. Cerulli-Irelli, M. Maggi, P. Wurz, P. Bochsler, N. Krupp, J. Woch, M. Fränz, K. Asamura, C. Dierker

Research output: Contribution to journal › Article › peer-review

52 Scopus citations

Abstract

The Electron Spectrometer (ELS) instrument of the ASPERA-3 package on the Mars Express satellite has recorded photoelectron energy spectra up to apoapsis ( ∼ 10, 000 km altitude). The characteristic photoelectron shape of the spectrum is sometimes seen well above the ionosphere in the evening sector across a wide range of near-equatorial latitudes. Two numerical models are used to analyze the characteristics of these high-altitude photoelectrons. The first is a global, multi-species MHD code that produces a 3-D representation of the magnetic field and bulk plasma parameters around Mars. It is used here to examine the possibility of magnetic connectivity between the high-altitude flanks of the martian ionosheath and the subsolar ionosphere. It is shown that some field lines in this region are draped interplanetary magnetic lines while others are open field lines (connected to both the IMF and the crustal magnetic field sources). The second model is a kinetic electron transport model that calculates the electron velocity space distribution along a selected, non-uniform, magnetic field line. It is used here to simulate the high-altitude ELS measurements. It is shown that the photoelectrons are essentially confined to the source cone, as governed by magnetic field inhomogeneity along the field line. Reasonable agreement is shown between the data and the model results, and a method is demonstrated for inferring properties of the local and photoelectron source region magnetic field from the ELS measurements. Specifically, the number of sectors in which photoelectrons are measured is a function of the magnetic field intensity ratio and the field's angle with respect to the detector plane. In addition, the sector of the photoelectron flux peak is a function of the magnetic field azimuthal angle in the detector plane.

Original language	English (US)
Pages (from-to)	383-395
Number of pages	13
Journal	Icarus
Volume	182
Issue number	2
DOIs	https://doi.org/10.1016/j.icarus.2005.10.036
State	Published - Jun 2006
Externally published	Yes

Keywords

Ionospheres
Magnetic fields
Magnetospheres
Mars

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

Access to Document

10.1016/j.icarus.2005.10.036

Cite this

Liemohn, M. W., Frahm, R. A., Winningham, J. D., Ma, Y., Barabash, S., Lundin, R., Kozyra, J. U., Nagy, A. F., Bougher, S. M., Bell, J., Brain, D., Mitchell, D., Luhmann, J., Holmström, M., Andersson, H., Yamauchi, M., Grigoriev, A., McKenna-Lawler, S., Sharber, J. R., ... Dierker, C. (2006). Numerical interpretation of high-altitude photoelectron observations. Icarus, 182(2), 383-395. https://doi.org/10.1016/j.icarus.2005.10.036

Liemohn, MW, Frahm, RA, Winningham, JD, Ma, Y, Barabash, S, Lundin, R, Kozyra, JU, Nagy, AF, Bougher, SM, Bell, J, Brain, D, Mitchell, D, Luhmann, J, Holmström, M, Andersson, H, Yamauchi, M, Grigoriev, A, McKenna-Lawler, S, Sharber, JR, Scherrer, JR, Jeffers, SJ, Coates, AJ, Linder, DR, Kataria, DO, Kallio, E, Koskinen, H, Säles, T, Riihelä, P, Schmidt, W, Roelof, E, Williams, D, Livi, S, Curtis, CC, Hsieh, KC, Sandel, BR, Grande, M, Carter, M, Sauvaud, JA, Fedorov, A, Thocaven, JJ, Orsini, S, Cerulli-Irelli, R, Maggi, M, Wurz, P, Bochsler, P, Krupp, N, Woch, J, Fränz, M, Asamura, K & Dierker, C 2006, 'Numerical interpretation of high-altitude photoelectron observations', Icarus, vol. 182, no. 2, pp. 383-395. https://doi.org/10.1016/j.icarus.2005.10.036

@article{8019a4f43c7843018168eb12ab4ed5bf,

title = "Numerical interpretation of high-altitude photoelectron observations",

abstract = "The Electron Spectrometer (ELS) instrument of the ASPERA-3 package on the Mars Express satellite has recorded photoelectron energy spectra up to apoapsis ( ∼ 10, 000 km altitude). The characteristic photoelectron shape of the spectrum is sometimes seen well above the ionosphere in the evening sector across a wide range of near-equatorial latitudes. Two numerical models are used to analyze the characteristics of these high-altitude photoelectrons. The first is a global, multi-species MHD code that produces a 3-D representation of the magnetic field and bulk plasma parameters around Mars. It is used here to examine the possibility of magnetic connectivity between the high-altitude flanks of the martian ionosheath and the subsolar ionosphere. It is shown that some field lines in this region are draped interplanetary magnetic lines while others are open field lines (connected to both the IMF and the crustal magnetic field sources). The second model is a kinetic electron transport model that calculates the electron velocity space distribution along a selected, non-uniform, magnetic field line. It is used here to simulate the high-altitude ELS measurements. It is shown that the photoelectrons are essentially confined to the source cone, as governed by magnetic field inhomogeneity along the field line. Reasonable agreement is shown between the data and the model results, and a method is demonstrated for inferring properties of the local and photoelectron source region magnetic field from the ELS measurements. Specifically, the number of sectors in which photoelectrons are measured is a function of the magnetic field intensity ratio and the field's angle with respect to the detector plane. In addition, the sector of the photoelectron flux peak is a function of the magnetic field azimuthal angle in the detector plane.",

keywords = "Ionospheres, Magnetic fields, Magnetospheres, Mars",

author = "Liemohn, {Michael W.} and Frahm, {R. A.} and Winningham, {J. D.} and Y. Ma and S. Barabash and R. Lundin and Kozyra, {J. U.} and Nagy, {A. F.} and Bougher, {S. M.} and J. Bell and D. Brain and D. Mitchell and J. Luhmann and M. Holmstr{\"o}m and H. Andersson and M. Yamauchi and A. Grigoriev and S. McKenna-Lawler and Sharber, {J. R.} and Scherrer, {J. R.} and Jeffers, {S. J.} and Coates, {A. J.} and Linder, {D. R.} and Kataria, {D. O.} and E. Kallio and H. Koskinen and T. S{\"a}les and P. Riihel{\"a} and W. Schmidt and E. Roelof and D. Williams and S. Livi and Curtis, {C. C.} and Hsieh, {K. C.} and Sandel, {B. R.} and M. Grande and M. Carter and Sauvaud, {J. A.} and A. Fedorov and Thocaven, {J. J.} and S. Orsini and R. Cerulli-Irelli and M. Maggi and P. Wurz and P. Bochsler and N. Krupp and J. Woch and M. Fr{\"a}nz and K. Asamura and C. Dierker",

note = "Funding Information: The Michigan authors would like to thank support for this research by NASA under Grants NAG5-10887, NNG04G055G, and NAG5-13332, by the NSF under Grant ATM-0455729, and by subcontract from Southwest Research Institute under NASW-00003. The ASPERA-3 experiment on the European Space Agency (ESA) Mars Express mission is a joint effort between 15 laboratories in 10 countries, all sponsored by their national agencies. We thank all these agencies as well as the various departments/institutes hosting these efforts. We also wish to acknowledge the Swedish National Space Board for their support of the main PI-institute and we are indebted to ESA for their courage in embarking on the Mars Express program, the first ESA mission to the Red Planet.",

year = "2006",

month = jun,

doi = "10.1016/j.icarus.2005.10.036",

language = "English (US)",

volume = "182",

pages = "383--395",

journal = "Icarus",

issn = "0019-1035",

publisher = "Academic Press Inc.",

number = "2",

}

TY - JOUR

T1 - Numerical interpretation of high-altitude photoelectron observations

AU - Liemohn, Michael W.

AU - Frahm, R. A.

AU - Winningham, J. D.

AU - Ma, Y.

AU - Barabash, S.

AU - Lundin, R.

AU - Kozyra, J. U.

AU - Nagy, A. F.

AU - Bougher, S. M.

AU - Bell, J.

AU - Brain, D.

AU - Mitchell, D.

AU - Luhmann, J.

AU - Holmström, M.

AU - Andersson, H.

AU - Yamauchi, M.

AU - Grigoriev, A.

AU - McKenna-Lawler, S.

AU - Sharber, J. R.

AU - Scherrer, J. R.

AU - Jeffers, S. J.

AU - Coates, A. J.

AU - Linder, D. R.

AU - Kataria, D. O.

AU - Kallio, E.

AU - Koskinen, H.

AU - Säles, T.

AU - Riihelä, P.

AU - Schmidt, W.

AU - Roelof, E.

AU - Williams, D.

AU - Livi, S.

AU - Curtis, C. C.

AU - Hsieh, K. C.

AU - Sandel, B. R.

AU - Grande, M.

AU - Carter, M.

AU - Sauvaud, J. A.

AU - Fedorov, A.

AU - Thocaven, J. J.

AU - Orsini, S.

AU - Cerulli-Irelli, R.

AU - Maggi, M.

AU - Wurz, P.

AU - Bochsler, P.

AU - Krupp, N.

AU - Woch, J.

AU - Fränz, M.

AU - Asamura, K.

AU - Dierker, C.

N1 - Funding Information: The Michigan authors would like to thank support for this research by NASA under Grants NAG5-10887, NNG04G055G, and NAG5-13332, by the NSF under Grant ATM-0455729, and by subcontract from Southwest Research Institute under NASW-00003. The ASPERA-3 experiment on the European Space Agency (ESA) Mars Express mission is a joint effort between 15 laboratories in 10 countries, all sponsored by their national agencies. We thank all these agencies as well as the various departments/institutes hosting these efforts. We also wish to acknowledge the Swedish National Space Board for their support of the main PI-institute and we are indebted to ESA for their courage in embarking on the Mars Express program, the first ESA mission to the Red Planet.

PY - 2006/6

Y1 - 2006/6

N2 - The Electron Spectrometer (ELS) instrument of the ASPERA-3 package on the Mars Express satellite has recorded photoelectron energy spectra up to apoapsis ( ∼ 10, 000 km altitude). The characteristic photoelectron shape of the spectrum is sometimes seen well above the ionosphere in the evening sector across a wide range of near-equatorial latitudes. Two numerical models are used to analyze the characteristics of these high-altitude photoelectrons. The first is a global, multi-species MHD code that produces a 3-D representation of the magnetic field and bulk plasma parameters around Mars. It is used here to examine the possibility of magnetic connectivity between the high-altitude flanks of the martian ionosheath and the subsolar ionosphere. It is shown that some field lines in this region are draped interplanetary magnetic lines while others are open field lines (connected to both the IMF and the crustal magnetic field sources). The second model is a kinetic electron transport model that calculates the electron velocity space distribution along a selected, non-uniform, magnetic field line. It is used here to simulate the high-altitude ELS measurements. It is shown that the photoelectrons are essentially confined to the source cone, as governed by magnetic field inhomogeneity along the field line. Reasonable agreement is shown between the data and the model results, and a method is demonstrated for inferring properties of the local and photoelectron source region magnetic field from the ELS measurements. Specifically, the number of sectors in which photoelectrons are measured is a function of the magnetic field intensity ratio and the field's angle with respect to the detector plane. In addition, the sector of the photoelectron flux peak is a function of the magnetic field azimuthal angle in the detector plane.

AB - The Electron Spectrometer (ELS) instrument of the ASPERA-3 package on the Mars Express satellite has recorded photoelectron energy spectra up to apoapsis ( ∼ 10, 000 km altitude). The characteristic photoelectron shape of the spectrum is sometimes seen well above the ionosphere in the evening sector across a wide range of near-equatorial latitudes. Two numerical models are used to analyze the characteristics of these high-altitude photoelectrons. The first is a global, multi-species MHD code that produces a 3-D representation of the magnetic field and bulk plasma parameters around Mars. It is used here to examine the possibility of magnetic connectivity between the high-altitude flanks of the martian ionosheath and the subsolar ionosphere. It is shown that some field lines in this region are draped interplanetary magnetic lines while others are open field lines (connected to both the IMF and the crustal magnetic field sources). The second model is a kinetic electron transport model that calculates the electron velocity space distribution along a selected, non-uniform, magnetic field line. It is used here to simulate the high-altitude ELS measurements. It is shown that the photoelectrons are essentially confined to the source cone, as governed by magnetic field inhomogeneity along the field line. Reasonable agreement is shown between the data and the model results, and a method is demonstrated for inferring properties of the local and photoelectron source region magnetic field from the ELS measurements. Specifically, the number of sectors in which photoelectrons are measured is a function of the magnetic field intensity ratio and the field's angle with respect to the detector plane. In addition, the sector of the photoelectron flux peak is a function of the magnetic field azimuthal angle in the detector plane.

KW - Ionospheres

KW - Magnetic fields

KW - Magnetospheres

KW - Mars

UR - http://www.scopus.com/inward/record.url?scp=33747354124&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=33747354124&partnerID=8YFLogxK

U2 - 10.1016/j.icarus.2005.10.036

DO - 10.1016/j.icarus.2005.10.036

M3 - Article

AN - SCOPUS:33747354124

SN - 0019-1035

VL - 182

SP - 383

EP - 395

JO - Icarus

JF - Icarus

IS - 2

ER -

Numerical interpretation of high-altitude photoelectron observations

Abstract

Keywords

ASJC Scopus subject areas

Access to Document

Other files and links

Fingerprint

Cite this