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Do solar models with weakly interacting massive particles reproduce the Stanford seismic data?

  • A. N. Ellis (a1) and D. O. Gough (a1)

Abstract

The discrepancy between theoretical eigenfrequencies of standard solar models and the frequencies of solar modes of degree between 2 and 5 measured at Stanford is degree-independent for cyclic frequencies above about 2 mHz. Below that frequency the discrepancy for dotriacontapole modes diverges from that of the modes of lower degree. The differences between eigenfrequencies of a simple solar model containing a cloud of weakly interacting particles in its core and of one without do not reproduce this behaviour.

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Copyright

References

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Christensen-Dalsgaard, J. 1982 Mon. Not. R. astr. Soc. 199, 735761
Christensen-Dalsgaard, J. and Gough, D. O. 1984 Solar seismology from space (ed. Ulrich, R K. et. al., JPL 8484, Pasadena) 199–204
Däppen, W., Gilliland, R. L. and Christensen-Dalsgaard, J. 1986 Nature 321, 229231
Faulkner, J. and Gilliland, R. L. 1985 Astrophys J. 299, 9941000
Faulkner, J., Gough, D. O. and Vahia, M. N. 1986 Nature 321 226229
Gough, D. O. 1986 Highlights of Astronomy 7, 283293
Henning, H. M. and Scherrer, P. H. 1986 Seismology of the sun and the distant stars (ed. Gough, D. O., NATO ASI, Reidel, Dordrecht) 5562

Do solar models with weakly interacting massive particles reproduce the Stanford seismic data?

  • A. N. Ellis (a1) and D. O. Gough (a1)

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