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IMF Direction Derived from Cycloid-Like Ion Distributions Observed by Mars Express

Although the Mars Express (MEX) does not carry a magnetometer, it is in principle possible to derive the interplanetary magnetic field (IMF) orientation from the three dimensional velocity distribution of pick-up ions measured by the Ion Mass Analyser (IMA) on board MEX because pick-up ions' orbits,... Full description

Journal Title: Space science reviews 2007-03-20, Vol.126 (1-4), p.239-266
Main Author: Yamauchi, M.
Other Authors: Futaana, Y. , Fedorov, A. , Dubinin, E. , Lundin, R. , Sauvaud, J.-A. , Winningham, D. , Frahm, R. , Barabash, S. , Holmstrom, M. , Woch, J. , Fraenz, M. , Budnik, E. , Borg, H. , Sharber, J. R. , Coates, A. J. , Soobiah, Y. , Koskinen, H. , Kallio, E. , Asamura, K. , Hayakawa, H. , Curtis, C. , Hsieh, K. C. , Sandel, B. R. , Grande, M. , Grigoriev, A. , Wurz, P. , Orsini, S. , Brandt, P. , Mckenna-Lawler, S. , Kozyra, J. , Luhmann, J.
Format: Electronic Article Electronic Article
Language: English
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Publisher: Springer
ID: ISSN: 0038-6308
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recordid: cdi_proquest_miscellaneous_29341273
title: IMF Direction Derived from Cycloid-Like Ion Distributions Observed by Mars Express
format: Article
creator:
  • Yamauchi, M.
  • Futaana, Y.
  • Fedorov, A.
  • Dubinin, E.
  • Lundin, R.
  • Sauvaud, J.-A.
  • Winningham, D.
  • Frahm, R.
  • Barabash, S.
  • Holmstrom, M.
  • Woch, J.
  • Fraenz, M.
  • Budnik, E.
  • Borg, H.
  • Sharber, J. R.
  • Coates, A. J.
  • Soobiah, Y.
  • Koskinen, H.
  • Kallio, E.
  • Asamura, K.
  • Hayakawa, H.
  • Curtis, C.
  • Hsieh, K. C.
  • Sandel, B. R.
  • Grande, M.
  • Grigoriev, A.
  • Wurz, P.
  • Orsini, S.
  • Brandt, P.
  • Mckenna-Lawler, S.
  • Kozyra, J.
  • Luhmann, J.
subjects:
  • Astronomy
  • Mars (Planet)
ispartof: Space science reviews, 2007-03-20, Vol.126 (1-4), p.239-266
description: Although the Mars Express (MEX) does not carry a magnetometer, it is in principle possible to derive the interplanetary magnetic field (IMF) orientation from the three dimensional velocity distribution of pick-up ions measured by the Ion Mass Analyser (IMA) on board MEX because pick-up ions' orbits, in velocity phase space, are expected to gyrate around the IMF when the IMF is relatively uniform on a scale larger than the proton gyroradius. Upstream of bow shock, MEX often observed cycloid distributions (two dimensional partial ring distributions in velocity phase space) of protons in a narrow channel of the IMA detector (only one azimuth for many polar angles). We show two such examples. Three different methods are used to derive the IMF orientation from the observed cycloid distributions. One method is intuitive (intuitive method), while the others derive the minimum variance direction of the velocity vectors for the observed ring ions. These velocity vectors are selected either manually (manual method) or automatically using simple filters (automatic method). While the intuitive method and the manual method provide similar IMF orientations by which the observed cycloid distribution is well arranged into a partial circle (representing gyration) and constant parallel velocity, the automatic method failed to arrange the data to the degree of the manual method, yielding about a 30 deg offset in the estimated IMF direction. The uncertainty of the derived IMF orientation is strongly affected by the instrument resolution. The source population for these ring distributions is most likely newly ionized hydrogen atoms, which are picked up by the solar wind.
language: eng
source:
identifier: ISSN: 0038-6308
fulltext: no_fulltext
issn:
  • 0038-6308
  • 1572-9672
url: Link


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titleIMF Direction Derived from Cycloid-Like Ion Distributions Observed by Mars Express
creatorYamauchi, M. ; Futaana, Y. ; Fedorov, A. ; Dubinin, E. ; Lundin, R. ; Sauvaud, J.-A. ; Winningham, D. ; Frahm, R. ; Barabash, S. ; Holmstrom, M. ; Woch, J. ; Fraenz, M. ; Budnik, E. ; Borg, H. ; Sharber, J. R. ; Coates, A. J. ; Soobiah, Y. ; Koskinen, H. ; Kallio, E. ; Asamura, K. ; Hayakawa, H. ; Curtis, C. ; Hsieh, K. C. ; Sandel, B. R. ; Grande, M. ; Grigoriev, A. ; Wurz, P. ; Orsini, S. ; Brandt, P. ; Mckenna-Lawler, S. ; Kozyra, J. ; Luhmann, J.
creatorcontribYamauchi, M. ; Futaana, Y. ; Fedorov, A. ; Dubinin, E. ; Lundin, R. ; Sauvaud, J.-A. ; Winningham, D. ; Frahm, R. ; Barabash, S. ; Holmstrom, M. ; Woch, J. ; Fraenz, M. ; Budnik, E. ; Borg, H. ; Sharber, J. R. ; Coates, A. J. ; Soobiah, Y. ; Koskinen, H. ; Kallio, E. ; Asamura, K. ; Hayakawa, H. ; Curtis, C. ; Hsieh, K. C. ; Sandel, B. R. ; Grande, M. ; Grigoriev, A. ; Wurz, P. ; Orsini, S. ; Brandt, P. ; Mckenna-Lawler, S. ; Kozyra, J. ; Luhmann, J.
descriptionAlthough the Mars Express (MEX) does not carry a magnetometer, it is in principle possible to derive the interplanetary magnetic field (IMF) orientation from the three dimensional velocity distribution of pick-up ions measured by the Ion Mass Analyser (IMA) on board MEX because pick-up ions' orbits, in velocity phase space, are expected to gyrate around the IMF when the IMF is relatively uniform on a scale larger than the proton gyroradius. Upstream of bow shock, MEX often observed cycloid distributions (two dimensional partial ring distributions in velocity phase space) of protons in a narrow channel of the IMA detector (only one azimuth for many polar angles). We show two such examples. Three different methods are used to derive the IMF orientation from the observed cycloid distributions. One method is intuitive (intuitive method), while the others derive the minimum variance direction of the velocity vectors for the observed ring ions. These velocity vectors are selected either manually (manual method) or automatically using simple filters (automatic method). While the intuitive method and the manual method provide similar IMF orientations by which the observed cycloid distribution is well arranged into a partial circle (representing gyration) and constant parallel velocity, the automatic method failed to arrange the data to the degree of the manual method, yielding about a 30 deg offset in the estimated IMF direction. The uncertainty of the derived IMF orientation is strongly affected by the instrument resolution. The source population for these ring distributions is most likely newly ionized hydrogen atoms, which are picked up by the solar wind.
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descriptionAlthough the Mars Express (MEX) does not carry a magnetometer, it is in principle possible to derive the interplanetary magnetic field (IMF) orientation from the three dimensional velocity distribution of pick-up ions measured by the Ion Mass Analyser (IMA) on board MEX because pick-up ions' orbits, in velocity phase space, are expected to gyrate around the IMF when the IMF is relatively uniform on a scale larger than the proton gyroradius. Upstream of bow shock, MEX often observed cycloid distributions (two dimensional partial ring distributions in velocity phase space) of protons in a narrow channel of the IMA detector (only one azimuth for many polar angles). We show two such examples. Three different methods are used to derive the IMF orientation from the observed cycloid distributions. One method is intuitive (intuitive method), while the others derive the minimum variance direction of the velocity vectors for the observed ring ions. These velocity vectors are selected either manually (manual method) or automatically using simple filters (automatic method). While the intuitive method and the manual method provide similar IMF orientations by which the observed cycloid distribution is well arranged into a partial circle (representing gyration) and constant parallel velocity, the automatic method failed to arrange the data to the degree of the manual method, yielding about a 30 deg offset in the estimated IMF direction. The uncertainty of the derived IMF orientation is strongly affected by the instrument resolution. The source population for these ring distributions is most likely newly ionized hydrogen atoms, which are picked up by the solar wind.
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abstractAlthough the Mars Express (MEX) does not carry a magnetometer, it is in principle possible to derive the interplanetary magnetic field (IMF) orientation from the three dimensional velocity distribution of pick-up ions measured by the Ion Mass Analyser (IMA) on board MEX because pick-up ions' orbits, in velocity phase space, are expected to gyrate around the IMF when the IMF is relatively uniform on a scale larger than the proton gyroradius. Upstream of bow shock, MEX often observed cycloid distributions (two dimensional partial ring distributions in velocity phase space) of protons in a narrow channel of the IMA detector (only one azimuth for many polar angles). We show two such examples. Three different methods are used to derive the IMF orientation from the observed cycloid distributions. One method is intuitive (intuitive method), while the others derive the minimum variance direction of the velocity vectors for the observed ring ions. These velocity vectors are selected either manually (manual method) or automatically using simple filters (automatic method). While the intuitive method and the manual method provide similar IMF orientations by which the observed cycloid distribution is well arranged into a partial circle (representing gyration) and constant parallel velocity, the automatic method failed to arrange the data to the degree of the manual method, yielding about a 30 deg offset in the estimated IMF direction. The uncertainty of the derived IMF orientation is strongly affected by the instrument resolution. The source population for these ring distributions is most likely newly ionized hydrogen atoms, which are picked up by the solar wind.
pubSpringer
doi10.1007/s11214-006-9090-1