A Criterion for Nuclear-EnergizedPulsational Instability
1979
- 118Usage
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Example: if you select the 1-year option for an article published in 2019 and a metric category shows 90%, that means that the article or review is performing better than 90% of the other articles/reviews published in that journal in 2019. If you select the 3-year option for the same article published in 2019 and the metric category shows 90%, that means that the article or review is performing better than 90% of the other articles/reviews published in that journal in 2019, 2018 and 2017.
Citation Benchmarking is provided by Scopus and SciVal and is different from the metrics context provided by PlumX Metrics.
Metrics Details
- Usage118
- Downloads111
- Abstract Views7
Article Description
This Note will present briefly some general properties of nuclear-energized pulsations of stars as treated in the linear quasi-adiabatic theory. In particular, the results will be derived from a number of detailed calculations of stellar models.It is well known that an upper limit for the fundamental eigenfrequency of radial pulsation Ѡ0 is given byѠmax2 = 1ʃ0(3Γ1 ‒ 4)q/x dq / 1ʃ0 x2dq,Ѡ2= (2∏/Period)2 R3/GM(e.g., Ledoux and Walraven 1958). According to this expression, Ѡmax2 increases both with decreasing radiation pressure (i.e., increasing Γ1) and with increasing central condensation as measured by the ratio of integrals
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