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Comparison of Magnetic Properties in a Magnetic Cloud and Its Solar Source on 2013 April 11-14

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dc.contributor.author Vemareddy, P
dc.contributor.author Mostl, C
dc.contributor.author Amerstorfer, T
dc.contributor.author Mishra, W
dc.contributor.author Farrugia, C
dc.contributor.author Leitner, M
dc.date.accessioned 2020-11-27T12:52:18Z
dc.date.available 2020-11-27T12:52:18Z
dc.date.issued 2016-06
dc.identifier.citation The Astrophysical Journal, Vol. 828, No. 1, 12 en_US
dc.identifier.issn 0004-637X
dc.identifier.uri http://prints.iiap.res.in/handle/2248/7495
dc.description Restricted Access © The American Astronomical Society http://dx.doi.org/10.3847/0004-637X/828/1/12 en_US
dc.description.abstract In the context of the Sun–Earth connection of coronal mass ejections and magnetic flux ropes (MFRs), we studied the solar active region (AR) and the magnetic properties of magnetic cloud (MC) event during 2013 April 14–15. We use in situ observations from the Advanced Composition Explorer and source AR measurements from the Solar Dynamics Observatory. The MCs magnetic structure is reconstructed from the Grad–Shafranov method, which reveals a northern component of the axial field with left handed helicity. The MC invariant axis is highly inclined to the ecliptic plane pointing northward and is rotated by 117° with respect to the source region PIL. The net axial flux and current in the MC are comparatively higher than from the source region. Linear force-free alpha distribution (10−7–10−6 m−1) at the sigmoid leg matches the range of twist number in the MC of 1–2 au MFR. The MFR is nonlinear force-free with decreasing twist from the axis (9 turns/au) toward the edge. Therefore, a Gold– Hoyle (GH) configuration, assuming a constant twist, is more consistent with the MC structure than the Lundquist configuration of increasing twist from the axis to boundary. As an indication of that, the GH configuration yields a better fitting to the global trend of in situ magnetic field components, in terms of rms, than the Lundquist model. These cylindrical configurations improved the MC fitting results when the effect of self-similar expansion of MFR was considered. For such twisting behavior, this study suggests an alternative fitting procedure to better characterize the MC magnetic structure and its source region links. en_US
dc.language.iso en en_US
dc.publisher IOP Publishing en_US
dc.subject Sun: coronal mass ejections (CMEs) en_US
dc.subject Sun: fi laments, prominences en_US
dc.subject Sun: flares en_US
dc.subject Sun: heliosphere en_US
dc.title Comparison of Magnetic Properties in a Magnetic Cloud and Its Solar Source on 2013 April 11-14 en_US
dc.type Article en_US


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