| GEOPHYSICS, ASTRONOMY, AND ASTROPHYSICS |
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The Pulsation Induced by Mass Transfer in Critically Rotating Stars |
| Jiang-Tao Wang1, Han-Feng Song1,2,3** |
1College of Science, Guizhou University, Guiyang 550025
2Geneva Observatory, University of Geneva, Sauverny CH-1290, Switzerland
3Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming 650011
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| Cite this article: |
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Jiang-Tao Wang, Han-Feng Song 2016 Chin. Phys. Lett. 33 099702 |
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Abstract The structural characteristics of the critically rotating accretor in binaries are investigated during rapid mass transfer. It is found that the accretor is subjected to periodic pulsation due to accretions and rejections of mass and angular momentum. The gainer attempts to attain both hydrostatic and thermal balances. This physical process can cause the thermal structure of the accreting star to fluctuate with a period of $\sim0.19$ y. Stellar wind can be enhanced by a factor of $\sim $$1.25$$\,\times\,$$10^{4}$ when the accretor approaches break-down velocity. Surface entropy and density decrease with the increase of the stellar radius due to the fact that rapid rotation leads to a reduction in the number density and surface temperature. The rotational energy has the same trend as stellar radius due to stellar expansion. Surface opacity which is extremely sensitive to surface temperature has an opposite trend to stellar radius. Moreover, the rate of nuclear energy must be adjusted due to mass removal or accretion at the stellar surface.
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Received: 03 May 2016
Published: 30 September 2016
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| PACS: |
97.10.Cv
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(Stellar structure, interiors, evolution, nucleosynthesis, ages)
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97.10.Kc
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(Stellar rotation)
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97.10.Gz
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(Accretion and accretion disks)
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