将受到愚蠢挑战的致密星与光秃秃的黑洞联系起来
Relating Follicly-Challenged Compact Stars to Bald Black Holes
摘要：
致密星满足一定的无毛关系，通过这种关系，它们的多极矩由它们的质量、自旋和四极矩给出。这些关系式近似独立于它们的状态方程，将压力与密度联系起来。这种关系类似于黑洞无毛定理，但它们拥有事件视界，导致它们形成的信息可以隐藏在其中。致密恒星没有视界，因此它们的无毛关系是否与黑洞有关还不清楚。我们调查如何这两个关系是相关的，通过研究多极矩之间的关系与各向异性的压力作为一个玩具模型，这使得这样的恒星比那些各向同性的压力更紧凑的紧凑型恒星。本文用数值方法证明了当紧致度接近黑洞时，紧致星的无毛关系接近黑洞的无毛关系。我们还证明了分析，目前的偶极矩正好达到黑洞极限二次紧凑的强各向异性的明星接近黑洞极限。此外，我们表明，紧凑型恒星逐渐成为扁圆在这个限制，即使长在低紧凑性，由于强各向异性。
英文摘要：
Compact stars satisfy certain no-hair relations through which their multipole moments are given by their mass, spin and quadrupole moment. These relations are approximately independent of their equation of state, relating pressure to density. Such relations are similar to the black hole no-hair theorems, but these possess event horizons inside which information that led to their formation can hide. Compact stars do not possess horizons, so whether their no-hair relations are related to the black hole ones is unclear. We investigate how the two relations are related by studying relations among multipole moments for compact stars with anisotropic pressure as a toy model, which allows such stars to be more compact than those with isotropic pressure. We here show numerically that the compact star no-hair relations approach the black hole ones as the compactness approaches that of a black hole. We also prove analytically that the current dipole moment exactly reaches the black hole limit quadratically in compactness as strongly-anisotropic stars approach the black hole limit. We moreover show that compact stars become progressively oblate in this limit, even if prolate at low compactness due to strong anisotropies.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
