Anisotropy and amplitude structure of low-l 5-min solar oscillations

Details Anisotropy and amplitude structure of low-l 5-min solar oscillations Anisotropy and amplitude structure of low-l 5-min solar oscillations

Jun 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984mmsai..55...69k&link_type=abstract

(European Physical Society, Ministero della Pubblica Istruzione, and Universita di Catania, EPS Study Conference on Oscillations

Astronomy and Astrophysics

Astronomy

1

Pulse Amplitude, Solar Oscillations, Vibration Mode, Anisotropy, Power Spectra, Time Series Analysis

Scientific paper

Line-center Doppler-shift data has been obtained from CCD-spectrograph observations. The 5-hour time series yields useful information at spatial wavelengths near one solar radius along both the solar north-south and east-west orientations. At these wavelengths the 5-min-oscillation velocity field is not isotropic and not well described by modes of uniform excitation. The velocity power density per spherical harmonic increases with decreasing l to 1100 sq cm/sq sec per 350-microhertz angular-frequency bandwidth at l = 4. It is interesting that the calculated low-l dependence in the growth rate of p-modes due to the kappa mechanism shows a similar behavior.

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