Rotational splitting of helioseismic modes influenced by a magnetic atmosphere

Free access article

Issue		A&A Volume 378, Number 1, October IV 2001


Page(s)		L1 - L4
Section		Letters
DOI		http://dx.doi.org/10.1051/0004-6361:20011061

A&A 378, L1-L4 (2001)
DOI: 10.1051/0004-6361:20011061

Rotational splitting of helioseismic modes influenced by a magnetic atmosphere

B. Pintér¹, R. New¹ and R. Erdélyi²

¹ School of Science and Mathematics, Sheffield Hallam University, Howard Street, Sheffield, S1 1WB, UK
e-mail: r.new@shu.ac.uk
² Space & Atmosphere Research Center, Dept. of Applied Mathematics, University of Sheffield, Hicks Building, Hounsfield Road, Sheffield, S3 7RH, UK
e-mail: Robertus@sheffield.ac.uk

(Received 18 July 2001 / Accepted 25 July 2001 )

Abstract
In the present paper the splitting of sectoral ( $m=\pm l$ ) helioseismic eigenmodes (f- and p-modes) is studied in the presence of a magnetic atmosphere. The solar interior is in a steady state, with sub-photospheric plasma flow along the equator representing solar rotation. The Cartesian geometry employed restricts the present study to sectoral modes, $m=\pm l$ . We work with $l \ge 50$ , which guarantees that the modes do not deeply penetrate into the solar interior and therefore experience an approximately uniform rotation. Potentially observable effects are predicted and developments of the model to aid detections are discussed.

Key words: Sun: helioseismology -- Sun: oscillations -- Sun: interior -- Sun: atmosphere -- Sun: magnetic fields -- Sun: rotation

Offprint request: B. Pintér, b. pinter@shu.ac.uk

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