Axisymmetric Simulations of Rotating Stellar Collapse in Full General Relativity

DOI DOI PDF Web Site BIBCODE 被引用文献17件 参考文献44件 オープンアクセス
  • Shibata Masaru
    Department of Physics, University of Illinois at Urbana–Champaign Urbana, IL 61801, USA Department of Earth and Space Science, Graduate School of Science Osaka University Toyonaka 560–0043, Japan

書誌事項

タイトル別名
  • Axisymmetric Simulations of Rotating Stellar Collapse in Full General Relativity. Criteria for Prompt Collapse to Black Holes.
  • -Criteria for Prompt Collapse to Black Holes-

この論文をさがす

説明

Motivated by a recent paper by the Potsdam numerical relativity group, we have constructed a new numerical code for hydrodynamic simulation of axisymmetric systems in full general relativity. In this code, we solve the Einstein field equation using Cartesian coordinates with appropriate boundary conditions. On the other hand, the hydrodynamic equations are solved in cylindrical coordinates. Using this code, we perform simulations to study axisymmetric collapse of rotating stars, which thereby become black holes or new compact stars, in full general relativity. To investigate the effects of rotation on the criterion for prompt collapse to black holes, we first adopt a polytropic equation of state, P=KρΓ, where P, ρ, and K are the pressure, rest mass density, and polytropic constant, with Γ=2. In this case, the collapse is adiabatic ({i.e.}, no change in entropy), and we can focus on the bare effect of rotation. As the initial conditions, we prepare rigidly and differentially rotating stars in equilibrium and then decrease the pressure to induce collapse. In this paper, we consider cases in which q ≡ J/Mg2 < 1, where J and Mg are the angular momentum and the gravitational mass. It is found that the criterion of black hole formation is strongly dependent on the angular momentum parameter q. For q < 0.5, the criterion is not strongly sensitive to q; more precisely, if the rest mass is slightly larger than the maximum allowed value of spherical stars, a black hole is formed. However, for q ≤ 1, it changes significantly: For q ≈ 0.9, the maximum allowed rest mass becomes ∼ 70–80% larger than that for spherical stars. These findings depend only weakly on the rotational profiles given initially. We then report the results for simulations employing a Γ-law equation of state P=(Γ-1)ρε, where ε is the specific internal energy, to study effects of shock heating. We find that the effects of shock heating are particularly important for preventing prompt collapse to black holes in the case of large q [i.e., q = O(1)].

収録刊行物

被引用文献 (17)*注記

もっと見る

参考文献 (44)*注記

もっと見る

キーワード

詳細情報 詳細情報について

問題の指摘

ページトップへ