Mars Express and Venus Express multi-point observation's of geoeffective solar flare events in December 2006

被引：105

作者：

Futaana, Y. ^{[1
]}

Barabash, S. ^{[1
]}

Yamauchi, M. ^{[1
]}

McKenna-Lawlor, S. ^{[2
]}

Lundin, R. ^{[1
]}

Luhmann, J. G. ^{[3
]}

Brain, D. ^{[3
]}

Carlsson, E. ^{[1
]}

Sauvaud, J. -A. ^{[4
]}

Winningham, J. D. ^{[5
]}

Frahm, R. A. ^{[5
]}

Wurz, P. ^{[6
]}

Holmstrom, M. ^{[1
]}

Gunell, H. ^{[7
]}

Kallo, E. ^{[8
]}

Baumjohann, W. ^{[9
]}

Lammer, H. ^{[9
]}

Sharber, J. R. ^{[5
]}

Hsieh, K. C. ^{[10
]}

Andersson, H. ^{[1
]}

Grigoriev, A. ^{[1
]}

Brinkfeldt, K. ^{[1
]}

Nilsson, H. ^{[1
]}

Asamura, K. ^{[11
]}

Zhang, T. L. ^{[9
]}

Coates, A. J. ^{[12
]}

Linder, D. R. ^{[12
]}

Kataria, D. O. ^{[12
]}

Curtis, C. C. ^{[10
]}

Sandel, B. R. ^{[10
]}

Fedorov, A. ^{[4
]}

Mazelle, C. ^{[4
]}

Thocaven, J. -J. ^{[4
]}

Grande, M. ^{[13
]}

Koskinen, Hannu E. J. ^{[14
]}

Sales, T. ^{[8
]}

Schmidt, W. ^{[8
]}

Riihela, P. ^{[8
]}

Kozyra, J. ^{[15
]}

Krupp, N. ^{[16
]}

Woch, J. ^{[16
]}

Fraenz, M. ^{[16
]}

Dubinin, E. ^{[16
]}

Orsini, S. ^{[17
]}

Cerulli-Irelli, R. ^{[17
]}

Mura, A. ^{[17
]}

Milillo, A. ^{[17
]}

Maggi, M. ^{[17
]}

Roelof, E. ^{[18
]}

Brandt, P. ^{[18
]}

机构：

[1] Swedish Inst Space Phys, SE-98128 Kiruna, Sweden

[2] Natl Univ Ireland, Maynooth, Kildare, Ireland

[3] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA

[4] Ctr Etud Spatiale Rayonnements, F-31028 Toulouse, France

[5] SW Res Inst, San Antonio, TX USA

[6] Univ Bern, Inst Phys, CH-3012 Bern, Switzerland

[7] W Virginia Univ, Dept Phys, Morgantown, WV 26506 USA

[8] Finnish Meteorol Inst, FIN-00101 Helsinki, Finland

[9] Austrian Acad Sci, Space Res Inst, A-8042 Graz, Austria

[10] Univ Arizona, Tucson, AZ 85721 USA

[11] Inst Space & Astronaut Sci, Sagamihara, Kanagawa 229, Japan

[12] UCL, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England

[13] Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England

[14] Univ Helsinki, Dept Phys Sci, FIN-00014 Helsinki, Finland

[15] Univ Michigan, Space Phys Res Lab, Ann Arbor, MI 48109 USA

[16] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany

[17] Inst Fis Spazio Interplanetari, I-00133 Rome, Italy

[18] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA

[19] KFKI Res Inst Particle & Nucl Phys, H-1525 Budapest, Hungary

来源：

PLANETARY AND SPACE SCIENCE | 2008年 / 56卷 / 06期

基金：

英国科学技术设施理事会;

关键词：

solar flare; space weather; ion escape; Mars; Venus; SEP;

D O I：

10.1016/j.pss.2007.10.014

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

In December 2006, a single active region produced a series of proton solar flares, with X-ray class up to the X9.0 level, starting on 5 December 2006 at 10:35 UT. A feature of this X9.0 flare is that associated MeV particles were observed at Venus and Mars by Venus Express (VEX) and Mars Express (MEX), which were similar to 80 degrees and similar to 125 degrees east of the flare site, respectively, in addition to the Earth, which was similar to 79 degrees west of the flare site. On December 5, 2006, the plasma instruments ASPERA-3 and ASPERA-4 on board MEX and VEX detected a large enhancement in their respective background count levels. This is a typical signature of solar energetic particle (SEP) events, i.e., intensive MeV particle fluxes. The timings of these enhancements were consistent with the estimated field-aligned travel time of particles associated with the X9.0 flare that followed the Parker spiral to reach Venus and Mars. Coronal mass ejection (CME) signatures that might be related to the proton flare were twice identified at Venus within < 43 and < 67 h after the flare. Although these CMEs did not necessarily originate from the X9.0 flare on December 5, 2006, they most likely originated from the same active region because these characteristics are very similar to flare-associated CMEs observed on the Earth. These observations indicate that CME and flare activities on the invisible side of the Sun may affect terrestrial space weather as a result of traveling more than 90 degrees in both azimuthal directions in the heliosphere. We would also like to emphasize that during the SEP activity, MEX data indicate an approximately one-order of magnitude enhancement in the heavy ion outflow flux from the Martian atmosphere. This is the first observation of the increase of escaping ion flux from Martian atmosphere during an intensive SEP event. This suggests that the solar EUV flux levels significantly affect the atmopheric loss from unmagnetized planets. (c) 2008 Elsevier Ltd. All rights reserved.

引用

页码：873 / 880

页数：8

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