3-D Numerical Models of Red Giant Stars

Details 3-D Numerical Models of Red Giant Stars 3-D Numerical Models of Red Giant Stars

Dec 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998aas...193.4405j&link_type=abstract

American Astronomical Society, 193rd AAS Meeting, #44.05; Bulletin of the American Astronomical Society, Vol. 30, p.1316

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Fully three dimensional and turbulent dynamic numerical simulations of red giant stars are presented. These models directly solve convective motions in the atmosphere of red giants utilizing the Piecewise Parabolic Method (PPM) hydrodynamic code to achieve high effective Reynolds and Rayleigh numbers. Computational meshes as high as 512(3) zones are used in order to admit a wide range of dynamically significant scales. These models show highly non-symmetric global dipolar flows within the convective layer of the 'star' as well as distinct radial pulsations driven by non-linear interactions of accoustic waves with convective motions. Spherical harmonics of the radial velocity are dominated by the dipolar (l=1) mode followed, at higher l values, by a spectrum of modes similar to that of a Kolmogorov turbulence spectrum. Details are given on the approximations of the present models as well as on refinements currently being implemented.

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