ON THE INTERNAL STRUCTURE OF THE MAGNETIC FIELD IN MAGNETIC CLOUDS AND INTERPLANETARY CORONAL MASS EJECTIONS: WRITHE VERSUS TWIST

被引：40

作者：

Al-Haddad, N. ^{[1
,2
]}

Roussev, I. I. ^{[1
]}

Moestl, C. ^{[3
,4
]}

Jacobs, C. ^{[2
]}

Lugaz, N. ^{[1
]}

Poedts, S. ^{[2
]}

Farrugia, C. J. ^{[5
,6
]}

机构：

[1] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA

[2] Katholieke Univ Leuven, Ctr Plasma Astrofys, B-3001 Louvain, Belgium

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

[4] Graz Univ, Inst Phys, A-8010 Graz, Austria

[5] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA

[6] Univ New Hampshire, Dept Phys, Durham, NH 03824 USA

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2011年 / 738卷 / 02期

基金：

奥地利科学基金会;

关键词：

Sun: corona; Sun: coronal mass ejections (CMEs); FLUX ROPES; RECONSTRUCTION; PROPAGATION; TOPOLOGY; WIND; CME;

D O I：

10.1088/2041-8205/738/2/L18

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

In this study, we test the flux rope paradigm by performing a "blind" reconstruction of the magnetic field structure of a simulated interplanetary coronal mass ejection (ICME). The ICME is the result of a magnetohydrodynamic numerical simulation and does not exhibit much magnetic twist, but appears to have some characteristics of a magnetic cloud, due to a writhe in the magnetic field lines. We use the Grad-Shafranov technique with simulated spacecraft measurements at two different distances and compare the reconstructed magnetic field with that of the ICME in the simulation. While the reconstructed magnetic field is similar to the simulated one as seen in two dimensions, it yields a helically twisted magnetic field in three dimensions. To further verify the results, we perform the reconstruction at three different position angles at every distance point, and all results are found to be in agreement. This work demonstrates that the current paradigm of associating magnetic clouds with flux ropes may have to be revised.

引用

页数：6

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