强磁场奇异夸克星的各向异性流体力学、体粘滞系数和R模
Anisotropic Hydrodynamics, Bulk Viscosities and R-Modes of Strange Quark Stars with Strong Magnetic Fields
摘要：
在强磁场中，奇异夸克物质的输运系数变为各向异性。我们确定的一般形式的完整的输运系数在强磁场的存在下。利用局域线性响应方法，我们分别计算了由非轻子弱过程$u+s\leftrightarrow u+d$引起的横向和平行于$B$场的体粘滞系数$\zperp$和$\zpara$.我们发现，对于磁场$B<10^{17}$ G，$\zperp$和$\zpara$对磁场的依赖性很弱，它们可以用零磁场下的体粘滞系数来近似.对于场$B>10^{18}$ G，$\zperp$和$\zpara$对场的依赖性都很强，它们都表现出de Haas-van Alphen型振荡.随着磁场的增加，这些振荡的幅度增加，这最终导致在参数空间的某些区域中的负$\zperp$。我们表明，改变符号的$\zperp$信号的流体动力学不稳定性。作为应用，我们讨论了新的体粘滞系数对旋转奇异夸克星r模不稳定性的影响。我们发现当磁场超过$B= 10^{17}$ G时，奇异夸克星的不稳定区受到影响。对于大一个数量级的磁场，不稳定区域显著扩大，使得磁化的奇异星比未磁化的奇异星更容易受到$r$模不稳定性的影响。
英文摘要：
In strong magnetic fields the transport coefficients of strange quark matter become anisotropic. We determine the general form of the complete set of transport coefficients in the presence of a strong magnetic field. By using a local linear response method, we calculate explicitly the bulk viscosities $\zperp$ and $\zpara$ transverse and parallel to the $B$-field respectively, which arise due to the non-leptonic weak processes $u+s\leftrightarrow u+d$. We find that for magnetic fields $B<10^{17}$ G, the dependence of $\zperp$ and $\zpara$ on the field is weak, and they can be approximated by the bulk viscosity for zero magnetic field. For fields $B>10^{18}$ G, the dependence of both $\zperp$ and $\zpara$ on the field is strong, and they exhibit de Haas-van Alphen-type oscillations. With increasing magnetic field, the amplitude of these oscillations increases, which eventually leads to negative $\zperp$ in some regions of parameter space. We show that the change of sign of $\zperp$ signals a hydrodynamic instability. As an application, we discuss the effects of the new bulk viscosities on the r-mode instability in rotating strange quark stars. We find that the instability region in strange quark stars is affected when the magnetic fields exceeds the value $B= 10^{17}$ G. For fields which are larger by an order of magnitude, the instability region is significantly enlarged, making magnetized strange stars more susceptible to $r$-mode instability than their unmagnetized counterparts.
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