Vertical distribution of the power of short- and long-period oscillations in a sunspot and in surrounding magnetic elements

Details Vertical distribution of the power of short- and long-period oscillations in a sunspot and in surrounding magnetic elements Vertical distribution of the power of short- and long-period oscillations in a sunspot and in surrounding magnetic elements

Aug 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009cosre..47..279e&link_type=abstract

Cosmic Research, Volume 47, Issue 4, pp.279-286

Physics

3

96.60.Qd, 96.60.Mz

Scientific paper

We present the results of processing three 256-min series of observations of quasi-periodic oscillations of the field of line-of-sight velocities in three sunspots. The Doppler shifts were determined simultaneously for six spectral lines formed at different heights in the solar atmosphere. In addition to the well-known high-frequency (periods of 3-5 min) oscillations, a band of low-frequency oscillations with periods of 60-80 min is revealed in the spectra of the sunspot umbra and magnetic elements located in immediate proximity of the sunspot. Unlike the short-period modes, the power of the long-period mode of line-of-sight velocity oscillations in the sunspot decreases sharply with height: these oscillations are distinctly seen in the line formed at a height of 200 km and almost are not seen in the line with the formation height of 500 km. This is indicative of different physical nature of the short-period and long-period oscillations of a sunspot. If the former are caused by slow magnetosonic waves within the field tube of the spot, the latter are representative of global vertical-radial oscillations of a magnetic element (spot, pore) as a whole near the position of a stable equilibrium.

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