Comparative analysis of Venus and Mars magnetotails

A. Fedorov; C. Ferrier; J. A. Sauvaud; S. Barabash; T. L. Zhang; C. Mazelle; R. Lundin; H. Gunell; H. Andersson; K. Brinkfeldt; Y. Futaana; A. Grigoriev; M. Holmström; M. Yamauchi; K. Asamura; W. Baumjohann; H. Lammer; A. J. Coates; D. O. Kataria; D. R. Linder; C. C. Curtis; K. C. Hsieh; B. R. Sandel; J. -J. Thocaven; M. Grande; H. Koskinen; E. Kallio; T. Sales; W. Schmidt; P. Riihela; J. Kozyra; N. Krupp; J. Woch; J. Luhmann; S. McKenna-Lawlor; S. Orsini; R. Cerulli-Irelli; A. Mura; A. Milillo; M. Maggi; E. Roelof; P. Brandt; C. T. Russell; K. Szego; J. D. Winningham; R. A. Frahm; J. Scherrer; J. R. Sharber; P. Wurz; P. Bochsler

doi:10.1016/j.pss.2007.12.012

Comparative analysis of Venus and Mars magnetotails

A. Fedorov, C. Ferrier, J. A. Sauvaud, S. Barabash, T. L. Zhang, C. Mazelle, R. Lundin, H. Gunell, H. Andersson, K. Brinkfeldt, Y. Futaana, A. Grigoriev, M. Holmström, M. Yamauchi, K. Asamura, W. Baumjohann, H. Lammer, A. J. Coates, D. O. Kataria, D. R. LinderC. C. Curtis, K. C. Hsieh, B. R. Sandel, J. -J. Thocaven, M. Grande, H. Koskinen, E. Kallio, T. Sales, W. Schmidt, P. Riihela, J. Kozyra, N. Krupp, J. Woch, J. Luhmann, S. McKenna-Lawlor, S. Orsini, R. Cerulli-Irelli, A. Mura, A. Milillo, M. Maggi, E. Roelof, P. Brandt, C. T. Russell, K. Szego, J. D. Winningham, R. A. Frahm, J. Scherrer, J. R. Sharber, P. Wurz, P. Bochsler

Department of Physics

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41 Citations (Scopus)

Abstract

We have an unique opportunity to compare the magnetospheres of two non-magnetic planets as Mars and Venus with identical instrument sets Aspera-3 and Aspera-4 on board of the Mars Express and Venus Express missions. We have performed both statistical and case studies of properties of the magnetosheath ion flows and the flows of planetary ions behind both planets. We have shown that the general morphology of both magnetotails is generally identical. In both cases the energy of the light (H+) and the heavy (O+, etc.) ions decreases from the tail periphery (several keV) down to few eV in the tail center. At the same time the wake center of both planets is occupied by plasma sheet coincident with the current sheet of the tail. Both plasma sheets are filled by accelerated (500–1000 eV) heavy planetary ions. We report also the discovery of a new feature never observed before in the tails of non-magnetic planets: the plasma sheet is enveloped by consecutive layers of He+ and H+ with decreasing energies.

Original language	English
Pages (from-to)	812-817
Number of pages	6
Journal	Planetary and Space Science
Volume	56
Issue number	6
DOIs	https://doi.org/10.1016/j.pss.2007.12.012
Publication status	Published - 01 May 2008

Keywords

Mars
Venus
Magnetotail
Magnetosphere

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Fedorov, A., Ferrier, C., Sauvaud, J. A., Barabash, S., Zhang, T. L., Mazelle, C., Lundin, R., Gunell, H., Andersson, H., Brinkfeldt, K., Futaana, Y., Grigoriev, A., Holmström, M., Yamauchi, M., Asamura, K., Baumjohann, W., Lammer, H., Coates, A. J., Kataria, D. O., ... Bochsler, P. (2008). Comparative analysis of Venus and Mars magnetotails. Planetary and Space Science, 56(6), 812-817. https://doi.org/10.1016/j.pss.2007.12.012

@article{0740a3f587e34d118b3307efd735ab2d,

title = "Comparative analysis of Venus and Mars magnetotails",

abstract = "We have an unique opportunity to compare the magnetospheres of two non-magnetic planets as Mars and Venus with identical instrument sets Aspera-3 and Aspera-4 on board of the Mars Express and Venus Express missions. We have performed both statistical and case studies of properties of the magnetosheath ion flows and the flows of planetary ions behind both planets. We have shown that the general morphology of both magnetotails is generally identical. In both cases the energy of the light (H+) and the heavy (O+, etc.) ions decreases from the tail periphery (several keV) down to few eV in the tail center. At the same time the wake center of both planets is occupied by plasma sheet coincident with the current sheet of the tail. Both plasma sheets are filled by accelerated (500–1000 eV) heavy planetary ions. We report also the discovery of a new feature never observed before in the tails of non-magnetic planets: the plasma sheet is enveloped by consecutive layers of He+ and H+ with decreasing energies.",

keywords = "Mars, Venus, Magnetotail, Magnetosphere",

author = "A. Fedorov and C. Ferrier and Sauvaud, {J. A.} and S. Barabash and Zhang, {T. L.} and C. Mazelle and R. Lundin and H. Gunell and H. Andersson and K. Brinkfeldt and Y. Futaana and A. Grigoriev and M. Holmstr{\"o}m and M. Yamauchi and K. Asamura and W. Baumjohann and H. Lammer and Coates, {A. J.} and Kataria, {D. O.} and Linder, {D. R.} and Curtis, {C. C.} and Hsieh, {K. C.} and Sandel, {B. R.} and Thocaven, {J. -J.} and M. Grande and H. Koskinen and E. Kallio and T. Sales and W. Schmidt and P. Riihela and J. Kozyra and N. Krupp and J. Woch and J. Luhmann and S. McKenna-Lawlor and S. Orsini and R. Cerulli-Irelli and A. Mura and A. Milillo and M. Maggi and E. Roelof and P. Brandt and Russell, {C. T.} and K. Szego and Winningham, {J. D.} and Frahm, {R. A.} and J. Scherrer and Sharber, {J. R.} and P. Wurz and P. Bochsler",

year = "2008",

month = may,

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doi = "10.1016/j.pss.2007.12.012",

language = "English",

volume = "56",

pages = "812--817",

journal = "Planetary and Space Science",

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publisher = "Elsevier",

number = "6",

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Fedorov, A, Ferrier, C, Sauvaud, JA, Barabash, S, Zhang, TL, Mazelle, C, Lundin, R, Gunell, H, Andersson, H, Brinkfeldt, K, Futaana, Y, Grigoriev, A, Holmström, M, Yamauchi, M, Asamura, K, Baumjohann, W, Lammer, H, Coates, AJ, Kataria, DO, Linder, DR, Curtis, CC, Hsieh, KC, Sandel, BR, Thocaven, J-J, Grande, M, Koskinen, H, Kallio, E, Sales, T, Schmidt, W, Riihela, P, Kozyra, J, Krupp, N, Woch, J, Luhmann, J, McKenna-Lawlor, S, Orsini, S, Cerulli-Irelli, R, Mura, A, Milillo, A, Maggi, M, Roelof, E, Brandt, P, Russell, CT, Szego, K, Winningham, JD, Frahm, RA, Scherrer, J, Sharber, JR, Wurz, P & Bochsler, P 2008, 'Comparative analysis of Venus and Mars magnetotails', Planetary and Space Science, vol. 56, no. 6, pp. 812-817. https://doi.org/10.1016/j.pss.2007.12.012

TY - JOUR

T1 - Comparative analysis of Venus and Mars magnetotails

AU - Fedorov, A.

AU - Ferrier, C.

AU - Sauvaud, J. A.

AU - Barabash, S.

AU - Zhang, T. L.

AU - Mazelle, C.

AU - Lundin, R.

AU - Gunell, H.

AU - Andersson, H.

AU - Brinkfeldt, K.

AU - Futaana, Y.

AU - Grigoriev, A.

AU - Holmström, M.

AU - Yamauchi, M.

AU - Asamura, K.

AU - Baumjohann, W.

AU - Lammer, H.

AU - Coates, A. J.

AU - Kataria, D. O.

AU - Linder, D. R.

AU - Curtis, C. C.

AU - Hsieh, K. C.

AU - Sandel, B. R.

AU - Thocaven, J. -J.

AU - Grande, M.

AU - Koskinen, H.

AU - Kallio, E.

AU - Sales, T.

AU - Schmidt, W.

AU - Riihela, P.

AU - Kozyra, J.

AU - Krupp, N.

AU - Woch, J.

AU - Luhmann, J.

AU - McKenna-Lawlor, S.

AU - Orsini, S.

AU - Cerulli-Irelli, R.

AU - Mura, A.

AU - Milillo, A.

AU - Maggi, M.

AU - Roelof, E.

AU - Brandt, P.

AU - Russell, C. T.

AU - Szego, K.

AU - Winningham, J. D.

AU - Frahm, R. A.

AU - Scherrer, J.

AU - Sharber, J. R.

AU - Wurz, P.

AU - Bochsler, P.

PY - 2008/5/1

Y1 - 2008/5/1

N2 - We have an unique opportunity to compare the magnetospheres of two non-magnetic planets as Mars and Venus with identical instrument sets Aspera-3 and Aspera-4 on board of the Mars Express and Venus Express missions. We have performed both statistical and case studies of properties of the magnetosheath ion flows and the flows of planetary ions behind both planets. We have shown that the general morphology of both magnetotails is generally identical. In both cases the energy of the light (H+) and the heavy (O+, etc.) ions decreases from the tail periphery (several keV) down to few eV in the tail center. At the same time the wake center of both planets is occupied by plasma sheet coincident with the current sheet of the tail. Both plasma sheets are filled by accelerated (500–1000 eV) heavy planetary ions. We report also the discovery of a new feature never observed before in the tails of non-magnetic planets: the plasma sheet is enveloped by consecutive layers of He+ and H+ with decreasing energies.

AB - We have an unique opportunity to compare the magnetospheres of two non-magnetic planets as Mars and Venus with identical instrument sets Aspera-3 and Aspera-4 on board of the Mars Express and Venus Express missions. We have performed both statistical and case studies of properties of the magnetosheath ion flows and the flows of planetary ions behind both planets. We have shown that the general morphology of both magnetotails is generally identical. In both cases the energy of the light (H+) and the heavy (O+, etc.) ions decreases from the tail periphery (several keV) down to few eV in the tail center. At the same time the wake center of both planets is occupied by plasma sheet coincident with the current sheet of the tail. Both plasma sheets are filled by accelerated (500–1000 eV) heavy planetary ions. We report also the discovery of a new feature never observed before in the tails of non-magnetic planets: the plasma sheet is enveloped by consecutive layers of He+ and H+ with decreasing energies.

KW - Mars

KW - Venus

KW - Magnetotail

KW - Magnetosphere

UR - http://hdl.handle.net/2160/8315

U2 - 10.1016/j.pss.2007.12.012

DO - 10.1016/j.pss.2007.12.012

M3 - Article

SN - 0032-0633

VL - 56

SP - 812

EP - 817

JO - Planetary and Space Science

JF - Planetary and Space Science

IS - 6

ER -

Comparative analysis of Venus and Mars magnetotails

Abstract

Keywords

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