NDLI: Observation of a Complex Solar Wind Reconnection Exhaust from Spacecraft Separated by over 1800 R $

Content Provider	Springer Nature Link
Author	Lavraud, B. Gosling, J. T. Rouillard, A. P. Fedorov, A. Opitz, A. Sauvaud, J. A. Foullon, C. Dandouras, I. Gét, V. Jacquey, C. Louarn, P. Mazelle, C. Peu, E. Phan, T. D. Larson, D. E. Luhmann, J. G. Schroeder, P. Skoug, R. M. Steinberg, J. T. Russell, C. T.
Copyright Year	2009
Abstract	We analyze Wind, ACE, and STEREO (ST-A and ST-B) plasma and magnetic field data in the vicinity of the heliospheric current sheet (HCS) crossed by all spacecraft between 22:15 UT on 31 March and 01:25 UT on 1 April 2007 corresponding to its observation at ST-A and ST-B, which were separated by over 1800 R $_{E}$ (or over 1200 R $_{E}$ across the Sun – Earth line). Although only Wind and ACE provided good ion flow data in accord with a solar wind magnetic reconnection exhaust at the HCS, the magnetic field bifurcation typical of such exhausts was clearly observed at all spacecraft. They also all observed unambiguous strahl mixing within the exhaust, consistent with the sunward flow deflection observed at Wind and ACE and thus with the formation of closed magnetic field lines within the exhaust with both ends attached to the Sun. The strong dawnward flow deflection in the exhaust is consistent with the exhaust and X-line orientations obtained from minimum variance analysis at each spacecraft so that the X-line is almost along the GSE Z-axis and duskward of all the spacecraft. The observation of strahl mixing in extended and intermittent layers outside the exhaust by ST-A and ST-B is consistent with the formation of electron separatrix layers surrounding the exhaust. This event also provides further evidence that balanced parallel and antiparallel suprathermal electron fluxes are not a necessary condition for identification of closed field lines in the solar wind. In the present case the origin of the imbalance simply is the mixing of strahls of substantially different strengths from a different solar source each side of the HCS. The inferred exhaust orientations and distances of each spacecraft relative to the X-line show that the exhaust was likely nonplanar, following the Parker spiral orientation. Finally, the separatrix layers and exhausts properties at each spacecraft suggest that the magnetic reconnection X-line location and/or reconnection rate were variable in both space and time at such large scales.
Starting Page	379
Ending Page	392
Page Count	14
File Format	PDF
ISSN	00380938
Journal	Solar Physics
Volume Number	256
Issue Number	1-2
e-ISSN	1573093X
Language	English
Publisher	Springer Netherlands
Publisher Date	2009-04-07
Publisher Place	Dordrecht
Access Restriction	One Nation One Subscription (ONOS)
Subject Keyword	Magnetic reconnection Solar wind Suprathermal electrons Strahl Halo Heliospheric current sheet Magnetic topology Extraterrestrial Physics, Space Sciences Meteorology/Climatology Astrophysics
Content Type	Text
Resource Type	Article
Subject	Astronomy and Astrophysics Space and Planetary Science

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1	Ministry of Education (GoI), Department of Higher Education	Sanctioning Authority	https://www.education.gov.in/ict-initiatives
2	Indian Institute of Technology Kharagpur	Host Institute of the Project: The host institute of the project is responsible for providing infrastructure support and hosting the project	https://www.iitkgp.ac.in
3	National Digital Library of India Office, Indian Institute of Technology Kharagpur	The administrative and infrastructural headquarters of the project	Dr. B. Sutradhar bsutra@ndl.gov.in
4	Project PI / Joint PI	Principal Investigator and Joint Principal Investigators of the project	Dr. B. Sutradhar bsutra@ndl.gov.in Prof. Saswat Chakrabarti will be added soon
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Observation of a Complex Solar Wind Reconnection Exhaust from Spacecraft Separated by over 1800 R E

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