What Causes P-mode Asymmetry Reversal?

Abstract

The solar acoustic p-mode line profiles are asymmetric. Velocity spectra have more power on the low-frequency sides, whereas intensity profiles show the opposite sense of asymmetry. Numerical simulations of the upper convection zone have resonant p-modes with the same asymmetries and asymmetry reversal as the observed modes. The temperature and velocity power spectra at optical depth ${\tau }_{\mathrm{cont}}=1$ have the opposite asymmetry as is observed for the intensity and velocity spectra. At a fixed geometrical depth, corresponding to $<{\tau }_{\mathrm{cont}}>=1$, however, the temperature and velocity spectra have the same asymmetry. This indicates that the asymmetry reversal is produced by radiative transfer effects and not by correlated noise.

16 pages, 10 figures, submitted to Astrophysical Journal

References in corpus (2)

• Line asymmetry of solar p-modes: Reversal of asymmetry in intensity power spectra
• Simulations of Oscillation Modes of the Solar Convection Zone

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