On the Pulsational Stability of Stars with Convective Envelopes.

Rabinowitz, Irving N.

doi:10.1086/146408

Cited by 8 publications

(3 citation statements)

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“…The rapid outward increase in S p / p is seen to contribute strongly to the damping in this case. These considerations show that, without some active destabilizing mechanism, most stars, particularly giants and supergiants, should be exceedingly stable against pulsations, as has been shown in the calculations of Cox (1955), Ledoux et aZ(l955) and Rabinowitz (1957). This result is quite satisfactory in that it agrees with the fact that pulsation is indeed very rare among stars (see $1).…”

Section: Efsect Of Ionization Zones On the Radiativesupporting

confidence: 62%

“…It follows that the nuclear sources can be completely neglected as a direct driving mechanism for the pulsations of most common types of variable stars. This conclusion has been confirmed by detailed calculations of Cox (1955), Ledoux et a1 (1955), Rabinowitz (1957 and Davey (1970Davey ( , 1973. I n these kinds of stars, then, the cause of the instability must be sought in the outer stellar layers where the relative pulsation amplitude is appreciable.…”

Section: Nuclear Driving Regions and Their Relative Importancementioning

confidence: 65%

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Pulsating stars

Cox¹

1974

Rep. Prog. Phys.

129

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Pulsating stars are a subset of the class of intrinsic variable stars. I n this review the main emphasis is on purely radial pulsations of spherically symmetric, nonrotating, non-magnetic stars. Most of the problems in this area can be treated on the basis of newtonian mechanics and gravitation. However, some modifications introduced by general relativity are described.After a short review of the relevant stellar time scales, the main observational data on pulsating stars are summarized, and then some elements of the basic theory of pulsating stars are presented. Considerable emphasis is given to the linear theory of radial pulsations, in part because of the important role that this theory has played in the development of our understanding of the causes and nature of stellar pulsations. Nonlinear pulsation calculations are also reviewed. An attempt is made to assess our present understanding of the causes and nature of pulsations in the various known types of pulsating stars and some important unsolved problems are summarized and discussed. One of the most important of these is the interaction between thermal convection and pulsations in stars.Finally, we have included a section concerned with applications of pulsation theory to miscellaneous kinds of objects not ordinarily thought of as pulsating stars : stars in ' quasi-hydrostatic ' equilibrium, relativistic pulsation theory, white dwarfs, neutron stars, rotating stars, magnetic stars and oscillating models of the universe.It is concluded that our understanding of the basic causes and nature of stellar pulsations is, by and large, in a fairly satisfactory state. It seems likely that the gaps that do exist in our present understanding of this subject arise mainly from the sheer complexity of the phenomena involved, and not from any outstanding deficiencies in basic physical theory.

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Section: Efsect Of Ionization Zones On the Radiativesupporting

confidence: 62%

Section: Nuclear Driving Regions and Their Relative Importancementioning

confidence: 65%

Pulsating stars

Cox¹

1974

Rep. Prog. Phys.

129

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“…However, turbulent viscosity may increase the rate of damping greatly. Cox [63] and Rabinowitz [64] both determined the rate of stimulation of stellar pulsations by thermo-nuclear reactions and the rate of damping by radiation. Their numerical values, referring respectively to a radiative giant model and to one with a convective envelope, differed considerably, but agreed in indicating that thermo-nuclear stimulation is negligibly small compared with radiative damping.…”

Section: Pulsations and Stabilitymentioning

confidence: 99%