Efficiency of convection in variable stars and the sun

Details Efficiency of convection in variable stars and the sun Efficiency of convection in variable stars and the sun

Jun 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979sci...204.1078c&link_type=abstract

Science, vol. 204, June 8, 1979, p. 1078, 1079.

Physics

2

Cepheid Variables, Convective Flow, Stellar Atmospheres, Sun, Stellar Luminosity, Stellar Models, Surface Temperature, Transmission Efficiency

Scientific paper

In a recent report Dearborn and Newman (1978), developing an idea of Ulrich (1975), suggested that small fluctuations in the luminosity of the sun could be caused by variations in the efficiency of convection in its outer layers. The present discussion is concerned with relatively small changes in the structure of the outer layers of Cepheid, which contain only a small fraction of the total mass. Observed changes in the pulsation periods of Cepheid variables can be used to place an upper limit on changes in convective efficiency in their outer layers. This limit implies changes no longer than those suggested as occurring in the sun.

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