Seismological demonstration of perpendicular density structuring in the solar corona

Free access article

Issue		A&A Volume 491, Number 2, November IV 2008


Page(s)		L9 - L12
Section		Letters
DOI		http://dx.doi.org/10.1051/0004-6361:200810659
Published online		15 October 2008

A&A 491, L9-L12 (2008)
DOI: 10.1051/0004-6361:200810659

Letter

Seismological demonstration of perpendicular density structuring in the solar corona

T. Van Doorsselaere, C. S. Brady, E. Verwichte, and V. M. Nakariakov

Centre for Fusion, Space and Astrophysics, Physics Department, University of Warwick, Coventry CV4 7AL, UK
e-mail: [t.van-doorsselaere;c.s.brady;v.nakariakov;erwin.verwichte]@warwick.ac.uk

Received 23 July 2008 / Accepted 18 September 2008

Abstract
The peculiarities of the propagating transverse waves observed in the solar corona with the Coronal Multi-channel Polarimeter (CoMP) indicate the existence of fine field structuring in the coronal density. We present results of numerical simulations studying the evolution of a localised transverse magneto-hydrodynamic wave in a uniform magnetic field. We consider two initial low plasma-beta equilibria: one with a homogeneous density, and one with a field-aligned dense structure (such as a loop or a plume). The perpendicular localisation of the wave strongly determines the angular distribution of the energy propagation. If the perpendicular scale of the wave is significantly smaller than the parallel scale (e.g. wavelength), as established by CoMP, the wave develops as an oblique fast magneto-acoustic wave. In an unstructured medium, the energy of such a wave is transferred mainly across the magnetic field. However, it is possible to channel the energy of the transverse wave along the magnetic field in the presence of a field-aligned density enhancement. We conclude that the CoMP results provide an independent seismological proof that the corona is structured in density in the perpendicular direction.

Key words: Sun: corona -- Sun: oscillations -- Sun: magnetic fields

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