Excitation of oscillations in the sun

Journal Article · Fri May 01 04:00:00 EDT 1981 · Sov. Astron. Lett. (Engl. Transl.); (United States)

OSTI ID:5702087

Kosovichev, A; Severnyi, A

The nonstationary equations of gas dynamics are solved numerically in order to analyze the radial adiabatic oscillations of the sun that would result from local perturbations of the thermodynamic parameters in the energy-generating core region (r = 0.1 R/sub sun/) of the sun. Calculations have been performed for a polytropic sphere (n = 3) and a standard solar model. The spherical wave produced by such a perturbation will travel from the center to the surface and back, undergoing successive reflections from the lower boundary of the atmosphere and from the center of the sun. Because of the wave-wake effect, pulsations of roughly-equal5-min period will arise in the atmosphere, taking the form of periodically recurrent wave trains separated by a time interval T = 2..integral../sup R//sub sun0/ c/sub s//sup -1/dr, where c/sub s/ is the velocity of sound. For the standard model sun, T = 119.2 min. The oscillations in the radiation flux and the oscillation power spectrum calculated numerically are compared with the solar pulsations observed.

• Research Organization: Crimean Astrophysical Observatory, USSR Academy of Sciences, Nauchnyi
• OSTI ID: 5702087
• Journal Information: Sov. Astron. Lett. (Engl. Transl.); (United States), Journal Name: Sov. Astron. Lett. (Engl. Transl.); (United States) Vol. 7:3; ISSN SALED
• Country of Publication: United States
• Language: English

Related Subjects

640104* -- Astrophysics & Cosmology-- Solar Phenomena
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
MAIN SEQUENCE STARS
MATHEMATICAL MODELS
NUMERICAL SOLUTION
OSCILLATION MODES
OSCILLATIONS
PULSATIONS
RADIATION FLUX
SPHERICAL HARMONICS
STAR MODELS
STARS
SUN
VARIATIONS