Study Of Excitation Mechanism Of Solar Oscillation Modes Using Realistic Numerical Simulations

Details Study Of Excitation Mechanism Of Solar Oscillation Modes Using Realistic Numerical Simulations Study Of Excitation Mechanism Of Solar Oscillation Modes Using Realistic Numerical Simulations

May 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...210.4603j&link_type=abstract

American Astronomical Society Meeting 210, #46.03; Bulletin of the American Astronomical Society, Vol. 39, p.161

Astronomy and Astrophysics

Astronomy

Scientific paper

Investigation of the excitation mechanisms of solar oscillations is important for understanding the interaction between turbulence and waves in the Sun and for developing helioseismology diagnostics.
The objective of this research is to study the sources which drive the waves in the Sun by means of realistic numerical simulations. We used a 3D, compressible, non-linear radiative-hydrodynamics code developed by Wray et al. (2005) for simulating the upper solar photosphere and lower atmosphere. This code takes into account several physical phenomena: compressible fluid flow in a highly stratified medium, radiative energy transfer between the fluid elements, and a real-gas equation of state. Strong fluctuations in the outer convective layers of the sun generate dominant acoustic sources in this region. Therefore we simulate the upper layers of the convection zone using 64^3 grid cells. The region extends 6x6 Mm horizontally and from 4.5 Mm below the visible surface to 1 Mm above the surface. We calculate the oscillation power spectra of radial and non-radial modes, extract the eigenfunctions, and calculate the work integral to estimate the depth of the oscillation sources; we then compare with the previous studies of Stein and Nordlund (2001) and Georgobiani et al. (2006) and with the observed properties of solar oscillations.

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