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 _ { cont } = 1 have the opposite asymmetry as is observed for the intensity and velocity spectra .
At a fixed geometrical depth , corresponding to < \tau _ { 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 .