Structure of the martian wake

A. Fedorov; E. Budnik; J. A. Sauvaud; C. Mazelle; S. Barabash; R. Lundin; M. Acuña; M. Holmström; A. Grigoriev; M. Yamauchi; H. Andersson; J. J. Thocaven; D. Winningham; R. Frahm; J. R. Sharber; J. Scherrer; A. J. Coates; D. R. Linder; D. O. Kataria; E. Kallio; H. Koskinen; T. Säles; P. Riihelä; W. Schmidt; J. Kozyra; J. Luhmann; E. Roelof; D. Williams; S. Livi; C. C. Curtis; K. C. Hsieh; B. R. Sandel; M. Grande; M. Carter; S. McKenna-Lawler; 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.2005.09.021

Structure of the martian wake

A. Fedorov^*, E. Budnik, J. A. Sauvaud, C. Mazelle, S. Barabash, R. Lundin, M. Acuña, M. Holmström, A. Grigoriev, M. Yamauchi, H. Andersson, J. J. Thocaven, D. Winningham, R. Frahm, J. R. Sharber, J. Scherrer, A. J. Coates, D. R. Linder, D. O. Kataria, E. KallioH. Koskinen, T. Säles, P. Riihelä, W. Schmidt, J. Kozyra, J. Luhmann, E. Roelof, D. Williams, S. Livi, C. C. Curtis, K. C. Hsieh, B. R. Sandel, M. Grande, M. Carter, S. McKenna-Lawler, S. Orsini, R. Cerulli-Irelli, M. Maggi, P. Wurz, P. Bochsler, N. Krupp, J. Woch, M. Fränz, K. Asamura, C. Dierker

^*Corresponding author for this work

Department of Physics

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

76 Citations (Scopus)

Abstract

We present the first results from the ion mass analyzer IMA of the ASPERA-3 instrument on-board of Mars Express. More than 200 orbits for May 2004-September 2004 time interval have been selected for the statistical study of the distribution of the atmospheric origin ions in the planetary wake. This study shows that the martian magnetotail consists of two different ion regimes. Planetary origin ions of the first regime form the layer adjacent to the magnetic pile-up boundary. These ions are accelerated to energy greater than 2000 eV and exhibit a gradual decreasing of energy down to the planetary tail. The second plasma regime is observed in the planetary shadow. The heavy ions (considered as planetary ones) are accelerated to the energy of the solar wind protons. Obviously the acceleration mechanism is different for the different plasma regimes. Study of two plasma regimes in the frame referred to the interplanetary magnetic field (IMF) direction (we used MGS magnetometer data to obtain the IMF clock angle) clearly shows their spatial anisotropy. The monoenergetic plasma in the planetary shadow is observed only in the narrow angular sector around the positive direction of the interplanetary electric field.

Original language	English
Pages (from-to)	329-336
Number of pages	8
Journal	Icarus
Volume	182
Issue number	2
DOIs	https://doi.org/10.1016/j.icarus.2005.09.021
Publication status	Published - Jun 2006

Keywords

Magnetospheres
Mars

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Fedorov, A., Budnik, E., Sauvaud, J. A., Mazelle, C., Barabash, S., Lundin, R., Acuña, M., Holmström, M., Grigoriev, A., Yamauchi, M., Andersson, H., Thocaven, J. J., Winningham, D., Frahm, R., Sharber, J. R., Scherrer, J., Coates, A. J., Linder, D. R., Kataria, D. O., ... Dierker, C. (2006). Structure of the martian wake. Icarus, 182(2), 329-336. https://doi.org/10.1016/j.icarus.2005.09.021

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title = "Structure of the martian wake",

abstract = "We present the first results from the ion mass analyzer IMA of the ASPERA-3 instrument on-board of Mars Express. More than 200 orbits for May 2004-September 2004 time interval have been selected for the statistical study of the distribution of the atmospheric origin ions in the planetary wake. This study shows that the martian magnetotail consists of two different ion regimes. Planetary origin ions of the first regime form the layer adjacent to the magnetic pile-up boundary. These ions are accelerated to energy greater than 2000 eV and exhibit a gradual decreasing of energy down to the planetary tail. The second plasma regime is observed in the planetary shadow. The heavy ions (considered as planetary ones) are accelerated to the energy of the solar wind protons. Obviously the acceleration mechanism is different for the different plasma regimes. Study of two plasma regimes in the frame referred to the interplanetary magnetic field (IMF) direction (we used MGS magnetometer data to obtain the IMF clock angle) clearly shows their spatial anisotropy. The monoenergetic plasma in the planetary shadow is observed only in the narrow angular sector around the positive direction of the interplanetary electric field.",

keywords = "Magnetospheres, Mars",

author = "A. Fedorov and E. Budnik and Sauvaud, {J. A.} and C. Mazelle and S. Barabash and R. Lundin and M. Acu{\~n}a and M. Holmstr{\"o}m and A. Grigoriev and M. Yamauchi and H. Andersson and Thocaven, {J. J.} and D. Winningham and R. Frahm and Sharber, {J. R.} and J. Scherrer 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 J. Kozyra and J. Luhmann 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 S. McKenna-Lawler 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",

year = "2006",

month = jun,

doi = "10.1016/j.icarus.2005.09.021",

language = "English",

volume = "182",

pages = "329--336",

journal = "Icarus",

issn = "0019-1035",

publisher = "Elsevier",

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Fedorov, A, Budnik, E, Sauvaud, JA, Mazelle, C, Barabash, S, Lundin, R, Acuña, M, Holmström, M, Grigoriev, A, Yamauchi, M, Andersson, H, Thocaven, JJ, Winningham, D, Frahm, R, Sharber, JR, Scherrer, J, Coates, AJ, Linder, DR, Kataria, DO, Kallio, E, Koskinen, H, Säles, T, Riihelä, P, Schmidt, W, Kozyra, J, Luhmann, J, Roelof, E, Williams, D, Livi, S, Curtis, CC, Hsieh, KC, Sandel, BR, Grande, M, Carter, M, McKenna-Lawler, S, Orsini, S, Cerulli-Irelli, R, Maggi, M, Wurz, P, Bochsler, P, Krupp, N, Woch, J, Fränz, M, Asamura, K & Dierker, C 2006, 'Structure of the martian wake', Icarus, vol. 182, no. 2, pp. 329-336. https://doi.org/10.1016/j.icarus.2005.09.021

TY - JOUR

T1 - Structure of the martian wake

AU - Fedorov, A.

AU - Budnik, E.

AU - Sauvaud, J. A.

AU - Mazelle, C.

AU - Barabash, S.

AU - Lundin, R.

AU - Acuña, M.

AU - Holmström, M.

AU - Grigoriev, A.

AU - Yamauchi, M.

AU - Andersson, H.

AU - Thocaven, J. J.

AU - Winningham, D.

AU - Frahm, R.

AU - Sharber, J. R.

AU - Scherrer, 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 - Kozyra, J.

AU - Luhmann, J.

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 - McKenna-Lawler, S.

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.

PY - 2006/6

Y1 - 2006/6

N2 - We present the first results from the ion mass analyzer IMA of the ASPERA-3 instrument on-board of Mars Express. More than 200 orbits for May 2004-September 2004 time interval have been selected for the statistical study of the distribution of the atmospheric origin ions in the planetary wake. This study shows that the martian magnetotail consists of two different ion regimes. Planetary origin ions of the first regime form the layer adjacent to the magnetic pile-up boundary. These ions are accelerated to energy greater than 2000 eV and exhibit a gradual decreasing of energy down to the planetary tail. The second plasma regime is observed in the planetary shadow. The heavy ions (considered as planetary ones) are accelerated to the energy of the solar wind protons. Obviously the acceleration mechanism is different for the different plasma regimes. Study of two plasma regimes in the frame referred to the interplanetary magnetic field (IMF) direction (we used MGS magnetometer data to obtain the IMF clock angle) clearly shows their spatial anisotropy. The monoenergetic plasma in the planetary shadow is observed only in the narrow angular sector around the positive direction of the interplanetary electric field.

AB - We present the first results from the ion mass analyzer IMA of the ASPERA-3 instrument on-board of Mars Express. More than 200 orbits for May 2004-September 2004 time interval have been selected for the statistical study of the distribution of the atmospheric origin ions in the planetary wake. This study shows that the martian magnetotail consists of two different ion regimes. Planetary origin ions of the first regime form the layer adjacent to the magnetic pile-up boundary. These ions are accelerated to energy greater than 2000 eV and exhibit a gradual decreasing of energy down to the planetary tail. The second plasma regime is observed in the planetary shadow. The heavy ions (considered as planetary ones) are accelerated to the energy of the solar wind protons. Obviously the acceleration mechanism is different for the different plasma regimes. Study of two plasma regimes in the frame referred to the interplanetary magnetic field (IMF) direction (we used MGS magnetometer data to obtain the IMF clock angle) clearly shows their spatial anisotropy. The monoenergetic plasma in the planetary shadow is observed only in the narrow angular sector around the positive direction of the interplanetary electric field.

KW - Magnetospheres

KW - Mars

UR - http://www.scopus.com/inward/record.url?scp=33747335947&partnerID=8YFLogxK

U2 - 10.1016/j.icarus.2005.09.021

DO - 10.1016/j.icarus.2005.09.021

M3 - Article

AN - SCOPUS:33747335947

SN - 0019-1035

VL - 182

SP - 329

EP - 336

JO - Icarus

JF - Icarus

IS - 2

ER -

Structure of the martian wake

Abstract

Keywords

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