Christy, R. F. (1968) The Dynamics of Variable Stars. SIAM Review, 10 (3). pp. 291-302. ISSN 0036-1445. http://resolver.caltech.edu/CaltechAUTHORS:CHRsiamr68
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Several closely related classes of variable stars—here called Cepheid variables—have long been known, as a result of detailed observation, to be vibrating in a spherically symmetric dilational mode. The purpose of the work described here has been to understand this motion and thereby to be able to apply the extensive data on variable stars in augmenting our knowledge of the stars.The coupled equations of spherical hydrodynamics and radiation diffusion have been solved numerically as an initial value problem for a variety of stellar models. Unstable models show a growing amplitude of pulsation which ultimately levels off at a stable maximum amplitude of periodic motion. This final motion and the associated large amplitude light variation agree closely with observed variables. Check calculations show that the results are reliable.The interior dynamics have been examined in order to find the physical, cause of the instability and also in order to understand peculiar secondary features of the pulsation. In addition, overtone pulsation in the first radial overtone has been studied. In a few cases, the instability can lead to stable large amplitude periodic motion in either the fundamental or the first overtone, depending on the initial conditions.
|Additional Information:||©1968 Society for Industrial and Applied Mathematics Received by the editors July 26, 1967. Presented by invitation at the Symposium on Modern Aspects of Dynamics, sponsored by the Air Force Office of Scientific Research, at the 1967 National Meeting of Society for Industrial and Applied Mathematics, held in Washington, D.C., June 11-15, 1967. Alfred P. Sloan Laboratory, California Institute of Technology, Pasadena, California 91109. This work was supported in part by the National Aeronautics and Space Administration under Grant NsG-426 and by the Office of Naval Research under Contract Nonr-220(47).|
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|Deposited On:||15 Dec 2006|
|Last Modified:||26 Dec 2012 09:23|
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