Computer Science – Sound
Scientific paper
May 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...180.0605s&link_type=abstract
American Astronomical Society, 180th AAS Meeting, #06.05; Bulletin of the American Astronomical Society, Vol. 24, p.737
Computer Science
Sound
Scientific paper
CCD images of FeI 5434 Angstroms line profiles have previously been collected and analyzed for the average characteristics of wave propagation in the photosphere. The previous analysis determined the velocity at nine depths in the spectral line and 100 horizontal spatial points spanning 70 arc sec. Time series of these velocity frames, lasting 37 minutes, have been Fourier transformed and filtered to pass the five minute modes of the Sun. Through the Hilbert transform and the analytic signal, the instantaneous velocity amplitude and phase were computed at every point in the three dimensional space of altitude, horizontal slit position and time. These data have been further processed to create color-contour maps of vertical acoustic propagation at each time sample. Velocity amplitude, velocity phase, kinetic energy density and acoustic flux are all mapped. Time series of these maps have been assembled into a movie which shows the evolution of vertical acoustic propagation. This movie is a complete visualization of sound waves in the photosphere, based on observation. The amplitude and kinetic energy density behaves as one might expect in the presence of the solar p-modes. However, the phase and acoustic flux have characteristic spatial and temporal scales which are very different from the amplitude. For example, upward and downward flux may occur in the same amplitude structure at different times, or at the same time. These results are consistent with the localized model of p-mode excitation advanced by Goode, Gough and Kosovichev.
Goode Philip. R.
Restaino Sergio R.
Stebbins Robin Tuck
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