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Structure of the interplanetary magnetic field during the interval spanning the first Cassini fly-through of Saturn's magnetosphere and its implications for Saturn's magnetospheric dynamics

Structure of the interplanetary magnetic field during the interval spanning the first Cassini fly-through of Saturn's magnetosphere and its implications for Saturn's magnetospheric dynamics
Structure of the interplanetary magnetic field during the interval spanning the first Cassini fly-through of Saturn's magnetosphere and its implications for Saturn's magnetospheric dynamics

We examine the interplanetary magnetic field (IMF) data obtained by the Cassini spacecraft during a 5 month period spanning the first fly-through of Saturn's magnetosphere, this interval corresponding to six solar rotations at the spacecraft. It is shown that the structure of the interplanetary medium was consistent with expectations for the declining phase of the solar cycle, generally consisting of two IMF sectors and two corotating interaction region compressions during each solar rotation. Field strengths and consequent estimated reconnection voltages at Saturn's magnetopause were overall weaker by a factor of about two compared with those observed during the immediately preceding interval investigated by Jackman et al. (J. Geophys. Res., 109, A11203, doi:10.1029/2004JA010614, 2004). Specifically, during the four solar rotations immediately preceding the fly-through, it is estimated that the total open flux produced at Saturn's magnetopause was ∼60 GWb per solar rotation, compared with ∼100 GWb per solar rotation estimated similarly for the earlier interval. These values compare with estimates of ∼35 GWb of open magnetic flux typically present in Saturn's tail lobes and polar cap. However, in the solar rotation immediately following the fly-through, it is found that field and voltage values recovered to former overall values.

Cassini, Declining phase of solar cycle, IMF, Saturn's magnetospheric dynamics
0273-1177
2120-2126
Jackman, C.M.
9bc3456c-b254-48f1-ade0-912c5b8b4529
Achilleos, N.
620cd146-20a4-4a84-8fd9-2a3e5d95aa2a
Bunce, E.J.
208e1177-a92f-47a6-878d-ef27ed03f811
Cowley, S.W.H.
e8174910-ddcd-4a23-9d7c-0e1117def06c
Milan, S.E.
b6dd5367-b0c4-4f30-953a-f2d13078d656
Jackman, C.M.
9bc3456c-b254-48f1-ade0-912c5b8b4529
Achilleos, N.
620cd146-20a4-4a84-8fd9-2a3e5d95aa2a
Bunce, E.J.
208e1177-a92f-47a6-878d-ef27ed03f811
Cowley, S.W.H.
e8174910-ddcd-4a23-9d7c-0e1117def06c
Milan, S.E.
b6dd5367-b0c4-4f30-953a-f2d13078d656

Jackman, C.M., Achilleos, N., Bunce, E.J., Cowley, S.W.H. and Milan, S.E. (2005) Structure of the interplanetary magnetic field during the interval spanning the first Cassini fly-through of Saturn's magnetosphere and its implications for Saturn's magnetospheric dynamics. Advances in Space Research, 36 (11), 2120-2126. (doi:10.1016/j.asr.2004.12.023).

Record type: Article

Abstract

We examine the interplanetary magnetic field (IMF) data obtained by the Cassini spacecraft during a 5 month period spanning the first fly-through of Saturn's magnetosphere, this interval corresponding to six solar rotations at the spacecraft. It is shown that the structure of the interplanetary medium was consistent with expectations for the declining phase of the solar cycle, generally consisting of two IMF sectors and two corotating interaction region compressions during each solar rotation. Field strengths and consequent estimated reconnection voltages at Saturn's magnetopause were overall weaker by a factor of about two compared with those observed during the immediately preceding interval investigated by Jackman et al. (J. Geophys. Res., 109, A11203, doi:10.1029/2004JA010614, 2004). Specifically, during the four solar rotations immediately preceding the fly-through, it is estimated that the total open flux produced at Saturn's magnetopause was ∼60 GWb per solar rotation, compared with ∼100 GWb per solar rotation estimated similarly for the earlier interval. These values compare with estimates of ∼35 GWb of open magnetic flux typically present in Saturn's tail lobes and polar cap. However, in the solar rotation immediately following the fly-through, it is found that field and voltage values recovered to former overall values.

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More information

e-pub ahead of print date: 5 February 2005
Published date: 2005
Keywords: Cassini, Declining phase of solar cycle, IMF, Saturn's magnetospheric dynamics

Identifiers

Local EPrints ID: 437118
URI: http://eprints.soton.ac.uk/id/eprint/437118
ISSN: 0273-1177
PURE UUID: cd1c2ee3-3d29-40a8-96e6-3d7374c936f1
ORCID for C.M. Jackman: ORCID iD orcid.org/0000-0003-0635-7361

Catalogue record

Date deposited: 17 Jan 2020 17:34
Last modified: 10 Nov 2021 03:35

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Contributors

Author: C.M. Jackman ORCID iD
Author: N. Achilleos
Author: E.J. Bunce
Author: S.W.H. Cowley
Author: S.E. Milan

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