Variability in the power spectrum of solar five-minute oscillations

Details Variability in the power spectrum of solar five-minute oscillations Variability in the power spectrum of solar five-minute oscillations

Jan 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983soph...82..411h&link_type=abstract

(International Astronomical Union and Akademiia Nauk SSSR, Colloquium on Problems of Solar and Stellar Oscillations, 66th, Nauch

Physics

14

Power Spectra, Solar Oscillations, Solar Spectra, Convective Flow, Line Spectra, Photosphere, Temperature Distribution, Velocity Distribution

Scientific paper

It is noted that two-dimensional power spectra of solar five-minute oscillations exhibit prominent ridge structures in (k, omega) space, k being the horizontal wavenumber and omega the temporal frequency. The positions of these ridges in k and omega can be used in probing temperature and velocity structures in the subphotosphere. The progress made in a program to establish whether power spectra taken on separate days show shifts in ridge locations is surveyed, noting that these may arise from different velocity and temperature patterns having been brought into the sampling region by solar rotation. Power spectra are obtained for six days of observations of Doppler velocities using the Mg I 5173 A and Fe I 5434 A spectral lines. Each data set encompasses 8 to 11 hr in time and samples a region 256 x 1024 arcsec in spatial extent, with a spatial resolution of 2 arcsec and temporal sampling of 65 s. Statistically significant shifts are detected in ridge locations between certain data sets. When analyzed in terms of eastward and westward propagating waves, the character of these displacements is seen as implying that changes have occurred in both temperature and horizontal velocity fields underlying the observing window. The velocity changes are estimated to be of the order of 100 m/s.

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