EDP Sciences
Free access
Issue
A&A
Volume 413, Number 3, January III 2004
Page(s) 1135 - 1142
Section Diffuse matter in space
DOI http://dx.doi.org/10.1051/0004-6361:20031541


A&A 413, 1135-1142 (2004)
DOI: 10.1051/0004-6361:20031541

Solar p modes in 10 years of the IRIS network

D. Salabert1, 2, E. Fossat1, B. Gelly1, S. Kholikov3, 4, G. Grec5, M. Lazrek5, 6 and F. X. Schmider1

1  Laboratoire Universitaire d'Astrophysique de Nice, Université de Nice-Sophia Antipolis, 06108 Nice Cedex 2, France
2  School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham B15 2TT, UK
3  Astronomical Institute of the Uzbek Academy of Sciences, 33, Astronomicheskaya, Tashkent 700052, Uzbekistan
4  National Solar Observatory, 950 North Cherry Avenue, Tucson, AZ 85719, USA
5  Observatoire de la Côte d'Azur, Lab. Cassini CNRS UMR 6529, 06304 Nice Cedex 4, France
6  Laboratoire d'Astronomie du CNCPRST, BP 1346, Rabat, Morocco

(Received 20 January 2003 / Accepted 3 September 2003)

Abstract
IRIS data (the low degree $\ell\leq 3$ helioseismology network) have been analysed for the study of p-mode parameters variability over the falling phase of the solar activity cycle 22 and the rising phase of the solar activity cycle 23. The IRIS duty cycle has been improved by the so-called "repetitive music method", a method of partial gap filling. We present in this paper an analysis of the dependence of p-mode frequencies and linewidths with frequency and with solar magnetic activity. We confirm also the periodicity of about 70  $\mu$Hz of the high-frequency pseudo modes, with a much reduced visibility during the phase of higher activity.


Key words: Sun: helioseismology -- Sun: activity

Offprint request: D. Salabert, david.salabert@unice.fr




© ESO 2004