引力波对中子星形状的制约
Gravitational wave constraints on the shape of neutron stars
摘要：
我们表明，有一个直接的关系上限（或潜在的未来测量）的m = 2四极矩的缓慢旋转的中子星和l = m = 2变形的恒星的表面，在充分的广义相对论，一阶的扰动。这种关系只取决于恒星的质量和半径结构。关于恒星的组成，我们所要做的就是假设其表面的应力-能量张量是理想流体的张量，这在几乎所有感兴趣的情况下都是正确的，并且具有很好的精确度，而且那里的磁场配置是无力的，这可能是一个很好的近似。然后，我们应用这种关系的恒星有直接LIGO/室女座的界限上的m = 2的四极矩，低于自旋下降的限制，并与预期的表面变形由于旋转。特别是，我们发现，LIGO观测约束蟹状星云脉冲星的l = m = 2表面变形小于其l = 2，m = 0变形由于旋转，对于我们考虑的所有因果状态方程，一个声明，将无法仅使用电磁观测的l = m = 2变形的上限。
英文摘要：
We show that there is a direct relation between upper limits on (or potential future measurements of) the m = 2 quadrupole moments of slowly rotating neutron stars and the l = m = 2 deformation of the star's surface, in full general relativity, to first order in the perturbation. This relation only depends on the star's structure through its mass and radius. All one has to assume about the star's constituents is that the stress-energy tensor at its surface is that of a perfect fluid, which will be true with good accuracy in almost all the situations of interest, and that the magnetic field configuration there is force-free, which is likely to be a good approximation. We then apply this relation to the stars which have direct LIGO/Virgo bounds on their m = 2 quadrupole moment, below the spin-down limit, and compare with the expected surface deformations due to rotation. In particular, we find that LIGO observations have constrained the Crab pulsar's l = m = 2 surface deformation to be smaller than its l = 2, m = 0 deformation due to rotation, for all the causal equations of state we consider, a statement that would not have been able to be made just using the upper bounds on the l = m = 2 deformation from electromagnetic observations.
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