1997年7月
Solving the Darwin problem in the first post-Newtonian approximation of general relativity: Compressible model
PHYSICAL REVIEW D
- ,
- 巻
- 56
- 号
- 2
- 開始ページ
- 811
- 終了ページ
- 825
- 記述言語
- 英語
- 掲載種別
- 研究論文(学術雑誌)
- DOI
- 10.1103/PhysRevD.56.811
- 出版者・発行元
- AMERICAN PHYSICAL SOC
Using the ellipsoidal model for the density configuration, we calculate the equilibrium sequence of the corotating binary stars of the polytropic equation of state in the first post-Newtonian approximation of general relativity. After we calibrate this model by comparing with previous numerical results, we perform the stability analysis by calculating the energy and the angular momentum of the system as a function of the orbital separation. We find that the orbital angular velocity at the energy and/or momentum minimum increases with the increase of the compactness of each star, and this fact holds irrespective of the polytropic index. These features agree with those in previous numerical works. We also show that due to the influence of the tidal field from the companion star, the central density of each star slightly decreases.
- リンク情報
- ID情報
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- DOI : 10.1103/PhysRevD.56.811
- ISSN : 0556-2821
- Web of Science ID : WOS:A1997XM24000025