Velocity and Intensity Power and Cross Spectra in Numerical Simulations of Solar Convection

Details Velocity and Intensity Power and Cross Spectra in Numerical Simulations of Solar Convection Velocity and Intensity Power and Cross Spectra in Numerical Simulations of Solar Convection

Sep 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008soph..251..549s&link_type=abstract

Solar Physics, Volume 251, Issue 1-2, pp. 549-562

Physics

1

Helioseismology: Direct Modeling, Waves: Modes, Velocity Fields: Photosphere

Scientific paper

Fitting observed power and cross spectra of medium-degree p modes in velocity ( V) and intensity ( I) has been widely used for getting information about the p-mode excitation process and, in particular, for trying to determine the type and location of the acoustic sources. Numerical simulations of solar convection allow one to “observe” velocity and temperature ( T, used as proxy for I) fluctuations in different reference frames. Sampling the oscillations on planes of constant optical depth ( τ-frame) closely corresponds to the observer’s point of view, whereas sampling the oscillations at constant geometrical height ( z-frame) is more appropriate for comparison with predictions from theoretical models based on Eulerian hydrodynamics. The results of the analysis in the two frames show significant differences. Considering the effects introduced on oscillations by the steep temperature gradient of the photosphere and by the temperature- and pressure-dependent continuum opacity, we develop a new model for fitting the simulated V and T power and cross spectra both in the τ- and z-frames and discuss its merits and limitations.

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