EDP Sciences
Free access
Volume 444, Number 2, December III 2005
Page(s) 585 - 592
Section The Sun
DOI http://dx.doi.org/10.1051/0004-6361:20053532

A&A 444, 585-592 (2005)
DOI: 10.1051/0004-6361:20053532

The extent of 3-min oscillations in regions other than sunspot plumes

C.-H. Lin1, D. Banerjee2, J. G. Doyle1 and E. O'Shea1

1  Armagh Observatory, College Hill, Armagh BT61 9DG, N. Ireland
    e-mail: chl@arm.ac.uk
2  Indian Institute of Astrophysics, Koramangala, Bangalore 560034, India

(Received 30 May 2005 / Accepted 12 August 2005 )

The active region, AR0554, was observed with NIS/CDS on board SoHO to examine the extent and range of oscillations from a range of features. Among all the NIS spectral lines analysed, significant oscillations were found in Si XII 520 Å, Mg X 625 Å, O V 629 Å, and He I 522 Å. The periods of the strongest oscillations in these lines were $\approx$10-20 min. After the dominant 10-20 min oscillations were filtered out from these lines, only O V 629 Å showed significant (i.e. above the 95% significance level) shorter-period oscillations. Specifically, we found that weak but significant 3-min oscillations are not confined to the umbra/plume but can be seen in many bright locations. The duration of these non-umbral 3-min oscillations is mostly $\approx$20 min. In contrast, the 3-min oscillations within the umbra are strong and stable for longer than 50 min. The duration could be related to the size of the oscillating source region, rather than the lifetime of the oscillation. To find the possible sources of these 3-min oscillations outside of the umbra, we compared the oscillations of single pixels in different regions. The results of our comparison indicate a possible connection between the magnetic fields and the oscillations. Therefore, we suggest that 3-min oscillations may exist in many magnetic structures, but are often too weak to be seen in an unfiltered signal.

Key words: Sun: corona -- Sun: oscillations

© ESO 2005