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Radiative pressure is an important physical factor and can affect the structure and evolution of the massive star. The Roche lobe, three Lagrangian points and the corresponding Roche potentials are calculated according to the asynchronous rotational Roche potential which includes the radiative pressure. They are compared with the corresponding synchronous rotational Roche potentials. It is found that the centrifugal force greatly reduces the gravitational acceleration at the equator while the radiative pressure can reduce the gravitational acceleration of the massive star. Both the asynchronous rotation and the radiative pressure have an obvious influence on the Roche lobe, the positions of three Lagrangian points, the Roche potentials and the time of mass overflow. Therefore, it is very important to calculate the asynchronous rotational Roche potential which includes the radiative pressure in the massive close binaries.
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Keywords:
- stellar structure and evolution /
- rotation /
- radiative pressure
[1] 黄润乾 2006 恒星物理 (2006 5 第1版) (北京: 中国科学技术出版社) p313
[2] Paczynski B 1971 ARA and A 9 183
[3] Kippenhahn R, Thomas H C 1970 Proceedings of IAU Colloq. 4 Ohio State University Columbus Ohio, September 8-11, 1969 p20
[4] Endal A S, Sofia S 1976 ApJ 210 184
[5] Pinsonneault M H, Kawaler S D, Sofia S, Demarqure P 1989 ApJ 338 424
[6] Pinsonneault M H, Kawaler S D, Demarqure P 1990 ApJS 74 501
[7] Pinsonneault M H, Deliyannis C P, Demarqure P 1991 ApJ 367 239
[8] Wang Y Z, Wu X, Zhong S Y 2012 Acta phy. Sin. 61 61160401 (in Chinese) [王玉诏, 伍歆, 钟双英 2012 61 160401]
[9] Wen D H, Chen W 2011 Chin. Phys. 20 029701
[10] Wen D H, Chen W, Liu L G 2005 中国物理快报 22 1604
[11] Huang R Q 2004 A&A 425 591
[12] Huang R Q 2004 A&A 422 981
[13] Kopal Z 1959 Close Binary Systems (1st Edn.) (New York: Wiley) p30
[14] Eggleton P P 1983 ApJ 268 368
[15] Huang R Q, Taam R E 1990 A&A 236 107
[16] Packet W 1981 A&A 102 17
[17] Petrovic J, Langer N 2005 A&A 435 1013
[18] de Mink S E, Pols O R, Glebbeek E 2007 AIPC 948 321
[19] Dermine T, Jorissen A, Siess L, Frankowski A 2009 A&A 507 891
[20] Maeder A, Georgy C, Meynet G 2008 A&A 479 37
[21] Claret A, Cunha N C S 1997 A&A 318 187
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[1] 黄润乾 2006 恒星物理 (2006 5 第1版) (北京: 中国科学技术出版社) p313
[2] Paczynski B 1971 ARA and A 9 183
[3] Kippenhahn R, Thomas H C 1970 Proceedings of IAU Colloq. 4 Ohio State University Columbus Ohio, September 8-11, 1969 p20
[4] Endal A S, Sofia S 1976 ApJ 210 184
[5] Pinsonneault M H, Kawaler S D, Sofia S, Demarqure P 1989 ApJ 338 424
[6] Pinsonneault M H, Kawaler S D, Demarqure P 1990 ApJS 74 501
[7] Pinsonneault M H, Deliyannis C P, Demarqure P 1991 ApJ 367 239
[8] Wang Y Z, Wu X, Zhong S Y 2012 Acta phy. Sin. 61 61160401 (in Chinese) [王玉诏, 伍歆, 钟双英 2012 61 160401]
[9] Wen D H, Chen W 2011 Chin. Phys. 20 029701
[10] Wen D H, Chen W, Liu L G 2005 中国物理快报 22 1604
[11] Huang R Q 2004 A&A 425 591
[12] Huang R Q 2004 A&A 422 981
[13] Kopal Z 1959 Close Binary Systems (1st Edn.) (New York: Wiley) p30
[14] Eggleton P P 1983 ApJ 268 368
[15] Huang R Q, Taam R E 1990 A&A 236 107
[16] Packet W 1981 A&A 102 17
[17] Petrovic J, Langer N 2005 A&A 435 1013
[18] de Mink S E, Pols O R, Glebbeek E 2007 AIPC 948 321
[19] Dermine T, Jorissen A, Siess L, Frankowski A 2009 A&A 507 891
[20] Maeder A, Georgy C, Meynet G 2008 A&A 479 37
[21] Claret A, Cunha N C S 1997 A&A 318 187
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