An attempt to understand the Stanford p-mode data

Details An attempt to understand the Stanford p-mode data An attempt to understand the Stanford p-mode data

Dec 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988esasp.286..195g&link_type=abstract

In ESA, Seismology of the Sun and Sun-Like Stars p 195-201 (SEE N89-25819 19-92)

Computer Science

Sound

35

Helioseismology, P Waves, Solar Oscillations, Stellar Models, Data Acquisition, Solar Diameter, Solar Interior, Solar Temperature, Velocity Distribution

Scientific paper

The p-mode frequencies reported by Henning and Scherred (1986), showing anomalous behavior at degree 5 and frequencies below 2 mHz were investigated. No plausible solar model is consistent with them. A density inversion including the low-degree 5 min data of Jimenez et al. (1988) implies that the density of the solar core is 10 percent greater than it is in the standard solar model 1 of Christensen-Dalsgaard (1982). Although that result is in keeping with previous suggestions either that the Sun has a greater evolutionary age than is usually supposed or that there is a cloud of weakly interacting massive particles in the solar core and its environs, the behavior of the sound speed in the core is not consistent with either hypothesis. Both the inferred sound-speed variation, and a secondary inversion for hydrogen abundance (relying on an assumption of thermal balance), provide evidence for material redistribution in the energy-generating core. A sound-speed inversion for the entire radiative interior, using also frequencies of low and intermediate degree compiled by Duvall et al. (1988), confirms the earlier finding that the sound speed in the Sun exceeds that of a standard solar model by up to 1 percent in a region extending 30 percent of the solar radius and centred at r = 0.4R. That is consistent with, though does not necessarily imply, that the opacity in the outer layers of the radiative interior at temperatures of up to 4 million K is underestimated by 20 percent.

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