The r-mode instability in strange stars with a crystalline crust
The r-mode instability in strange stars with a crystalline crust
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具有结晶地壳的奇怪恒星的 r 模式不稳定性
DOI：
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发表时间：
2012
期刊：
影响因子：
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通讯作者：
P. Jaikumar
中科院分区：
文献类型：
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作者：
G. Rupak;P. Jaikumar
r模不稳定性被认为限制了致密恒星的旋转速度，可以为夸克物质的稳定退禁闭相的存在提供经验证实，这些夸克物质的稳定退禁闭相是通过量子色动力学中的弱耦合计算预测的。我们构造了一个重约2个太阳质量的奇异夸克星模型，它是由超导夸克物质和一个薄的晶体夸克物质壳构成的。这种晶体夸克壳足够坚固，可以承受r模加热和实际模振幅为O（10^{-2}）的粘性摩擦，这与富中子核构成的壳不同。在核壳边界的粘性摩擦所提供的耗散是必要的和足够的，以获得稳定的旋转速度是一致的，与大多数快速旋转的恒星在低质量的X射线双星。我们的分析意味着，虽然裸奇异星被快速旋转的夸克星的存在所排除，但具有夸克物质外壳的奇异星星是一种明显的可能性。
The r-mode instability, believed to limit the rotation speed of compact stars, can provide empirical confirmation for the existence of stable deconfined phases of quark matter that are predicted by weak coupling calculations in Quantum Chromodynamics. We construct a model for strange quark stars as heavy as 2 solar masses that are made of superconducting quark matter in the bulk and a thin crystalline quark matter crust. This crystalline quark crust is sufficiently robust to withstand r-mode heating and viscous rubbing for realistic mode amplitudes O(10^{-2}), unlike a crust made of neutron-rich nuclei. The dissipation provided by viscous rubbing at the core-crust boundary is both necessary and sufficient to obtain stable rotation speeds that are consistent with the majority of rapidly spinning pulsars in low mass X-ray binaries. Our analysis implies that while bare strange stars are ruled out by the existence of rapidly spinning pulsars, a strange star with a quark matter crust is a distinct possibility.