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

Published online by Cambridge University Press:  03 August 2017

A. N. Ellis  and
D. O. Gough
A. N. Ellis
Affiliation:
Department of Applied Mathematics and Theoretical Physics, and Institute of Astronomy, University of Cambridge, UK
D. O. Gough
Affiliation:
Department of Applied Mathematics and Theoretical Physics, and Institute of Astronomy, University of Cambridge, UK

Abstract

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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.

Type
Chapter 2: Theory of Solar Oscillations
Information
Symposium - International Astronomical Union , Volume 123: Advances In Hello- and Asteroseismology , 1988 , pp. 111 - 114
Copyright
Copyright © Reidel 1988 

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