Radiative Hydrodynamic Simulations of Turbulent Convection and Oscillations from Solar-Type to A-Type Stars

Details Radiative Hydrodynamic Simulations of Turbulent Convection and Oscillations from Solar-Type to A-Type Stars Radiative Hydrodynamic Simulations of Turbulent Convection and Oscillations from Solar-Type to A-Type Stars

May 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21640012k&link_type=abstract

American Astronomical Society, AAS Meeting #216, #400.12; Bulletin of the American Astronomical Society, Vol. 41, p.856

Astronomy and Astrophysics

Astronomy

Scientific paper

We use 3D numerical radiative hydrodynamic simulations to study convective and oscillation properties of main sequence stars from the solar-type stars to more massive stars. The solar-type pulsators are characterized by acoustic oscillation modes excited by turbulent granular convection in the upper convective boundary layer. As the stellar mass increases the convection zone shrinks, the scale and intensity of the turbulent motions increases, providing more energy for excitation of acoustic modes. When the stellar mass reaches about 1.6 solar masses the upper convection zone consists of two very thin layers corresponding to H and He ionization, and in addition to the acoustic modes the stars show strong internal gravity modes The thin convection zone is often considered insignificant for the stellar dynamics and variability. However, the 3D radiative hydrodynamics simulations reveal supersonic granular-type convection of the scale significantly larger than the solar granulation, and strong overshooting plumes penetrating into the stable radiative zone. These plumes may contribute to the excitation of oscillation in A-type stars.

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