Nonadiabatic, nonradial solar oscillations
Solar gravity mode (g-mode) oscillations are not easy to detect and identify because their surface amplitudes are very small. However, since their largest amplitudes occur in the deep interior of the sun, their correct interpretation could be invaluable in unraveling the interior structure of the sun. Toward this end, some nonadiabatic, nonradial solar g-mode calculations, using the Lagrangian-based eigensolution program of Pesnell, are presented. 2 figs., 2 tabs.
- Research Organization:
- Los Alamos National Lab., NM (USA)
- DOE Contract Number:
- W-7405-ENG-36
- OSTI ID:
- 6961394
- Report Number(s):
- LA-UR-86-4196; CONF-8608130-7; ON: DE87003736
- Country of Publication:
- United States
- Language:
- English
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