Stellar background power spectra from hydrodynamical simulations of stellar atmospheres

Details Stellar background power spectra from hydrodynamical simulations of stellar atmospheres Stellar background power spectra from hydrodynamical simulations of stellar atmospheres

Nov 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998mons.proc...59t&link_type=abstract

The First MONS Workshop: Science with a Small Space Telescope, held in Aarhus, Denmark, June 29 - 30, 1998, Eds.: H. Kjeldsen, T

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14

Scientific paper

The non-p-mode contribution to the temporal irradiance or velocity spectra of the Sun has for a long time been considered as noise, but in recent years it has gradually been appreciated as the signal of granulation. Accordingly these spectra are now referred to as background spectra. We hope that further analysis of these background spectra will serve two purposes: to provide information about convection in other stars; and, as the background still constitutes a noise source when looking for p- and in particular g-modes of solar type stars, to provide us with stricter limits as to what is observable. Based on hydrodynamical simulations of convection in the atmospheres of the Sun, alpha Cen A and Procyon, we calculate irradiance and velocity spectra and infer a few properties of these spectra. Due to the limited horizontal extent of the simulations (covering 6-8 granules each) we only get a signal from the granulation, whereas effects of meso- and supergranulation are missing in our signal. At the high-frequency end we are limited by the horizontal resolution of the simulations.

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