强环向场新生磁星的早期演化
Early evolution of newly born magnetars with a strong toroidal field
摘要：
我们提出了一个国家的最先进的方案，为新诞生的磁星作为强源的引力波（GWs）在形成后的早期。本文讨论了快速旋转超磁化中子星天体物理学的几个方面，包括向超流转变前的早期冷却、磁场对中子星平衡形状的影响、完全简并的斜旋转体的内部动力学状态以及对新生中子星的电磁转矩的强度。我们表明，我们的方案与最近对银河系中AXP和SGR周围SNR的研究是一致的，这些研究将来自中央NS的电磁能量输入限制在<= 10^51 erg。我们进一步表明，如果这个条件得到满足，那么GW信号从这样的来源是潜在的检测与即将到来的一代GW探测器到室女星系团的距离，事件率<= 1/年可以估计。最后，我们指出，内部磁场在10^16 G范围内的衰减在非常早期的阶段与NS冷却强烈耦合，从而显著减缓了这两个过程：磁场可以保持这种强度至少10^3年，在此期间，核心温度保持在10^8 K的数倍以上。
英文摘要：
We present a state-of-the-art scenario for newly born magnetars as strong sources of Gravitational Waves (GWs)in the early days after formation. We address several aspects of the astrophysics of rapidly rotating, ultramagnetized neutron stars (NSs), including early cooling before transition to superfluidity, the effects of the magnetic field on the equilibrium shape of NSs, the internal dynamical state of a fully degenerate, oblique rotator and the strength of the electromagnetic torque on the newly born NS. We show that our scenario is consistent with recent studies of SNRs surrounding AXPs and SGRs in the Galaxy that constrain the electromagnetic energy input from the central NS to be <= 10^51 erg. We further show that if this condition is met, then the GW signal from such sources is potentially detectable with the forthcoming generation of GW detectors up to Virgo cluster distances where an event rate <= 1/yr can be estimated. Finally, we point out that the decay of an internal magnetic field in the 10^16 G range couples strongly to the NS cooling at very early stages, thus significantly slowing down both processes: the field can remain this strong for at least 10^3 yrs, during which the core temperature stays higher than several times 10^8 K.
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