In this article we examine the possibility, previously considered by others, that the pulsed radio sources observed recently are pulsating white dwarfs. We first present the results of radial mode eigenvalue calculations (for various central densities and compositions) which were obtained by integrating the eigenvalue equations themselves rather than by using variational techniques. Computations of non-linear white dwarf pulsations are then presented, in which a hydrodynamic code was used to follow pulsations of finite amplitude driven by pycno-nuclear reactions. Very large amplitude pulsation of neutron stars is also considered. The possibility that the optical pulsation periods are twice as long as the radio periods has arisen from observations1. We discuss a method for such a “frequency doubling” based partly on magnetohy drodynamics.
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- 4.Chandrasekhar, S., Stellar Structure (University of Chicago Press, Chicago, 1938).Google Scholar
- 10.Cameron, A. G. W., Stellar Evolution, Nuclear Astrophysics and Nucleogenesis (Chalk River, Ontario, 1957).Google Scholar
- 14.Wild, J. P., Smerd, S. F., and Weiss, A. A., Ann. Rev. Astro. Astrophys., 1, 360 (1963).Google Scholar
- 17.Maran, S. P., and Cameron, A. G. W., Physics Today (in the press).Google Scholar
- 18.Wild, J. P., Smerd, S. F., and Weiss, A. A., Ann. Rev. Astro. Astrophys., 1, 354 (1963).Google Scholar