Astronomy & Astrophysics

Issue		A&A Volume 464, Number 2, March III 2007
Page(s)		753 - 760
Section		The Sun
DOI		10.1051/0004-6361:20065866

A&A 464, 753-760 (2007)
DOI: 10.1051/0004-6361:20065866

MHD evolution of a fragment of a CME core in the outer solar corona

P. Pagano^{1, 2}, F. Reale^{1, 2}, S. Orlando², and G. Peres^{1, 2}

¹ Dipartimento di Scienze Fisiche ed Astronomiche, Sezione di Astronomia, Università di Palermo, Piazza del Parlamento 1, 90134 Palermo, Italy
e-mail: pagano@astropa.unipa.it
² INAF - Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, 90134 Palermo, Italy

(Received 20 June 2006 / Accepted 9 December 2006)

Abstract
Context.Detailed hydrodynamic modeling explained several features of a fragment of the core of a Coronal Mass Ejection observed with SoHO/UVCS at 1.7 $R_{\odot}$ on 12 December 1997, but some questions remained unsolved.
Aims.We investigate the role of the magnetic fields in the thermal insulation and the expansion of an ejected fragment (cloud) traveling upwards in the outer corona.
Methods.We perform MHD simulations including the effects of thermal conduction and radiative losses of a dense spherical or cylindrical cloud launched upwards in the outer corona, with various assumptions on the strength and topology of the ambient magnetic field; we also consider the case of a cylindrical cloud with an internal magnetic field component along its axis.
Results.We find that a weak ambient magnetic field ( $\beta \sim 20$ ) with open topology provides both significant thermal insulation and large expansion. The cylindrical cloud expands more than the spherical one.

Key words: Sun: coronal mass ejections (CMEs) -- magnetohydrodynamics (MHD) -- Sun: corona

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