The stability of the low-degree 5-minute solar oscillations

Details The stability of the low-degree 5-minute solar oscillations The stability of the low-degree 5-minute solar oscillations

Dec 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984sses.nasa..335k&link_type=abstract

In JPL Solar Seismology from Space. p 335-343 (SEE N85-25060 14-92)

Computer Science

11

Decay Rates, Power Spectra, Solar Oscillations, Damping, Equations Of State, Frequencies, Helium, Hydrogen, Tables (Data)

Scientific paper

The decay rate for many of the low degree p modes observed as 5 minute oscillations of the Sun is discussed and decay rates for modes ranging from radial (l=0) to the nonradial ones with l=5 for overtones 10 through 28. Parameters needed for he solar model are given and the hydrogen mass fraction composition structure is shown as well as the structure given by Christensen-Dalsgaard (1982) for an evolved solar model. The special equation of state and opacity table with X=0.74 for the hydrogen mass fraction in the outer 0.40 of the mass needs slightly more hydrogen in the central regions than obtained by Christensen-Dalsgaard in order to give a complete and consistent model. The difference in helium production between these two models is about 10%, meaning that the total energy radiated by the Sun during its lifetime thus far agrees satisfactorily with accurately calculated evolution sequences.

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