磁星不岁差的影响
Implications of magnetar non-precession
摘要：
被称为异常X射线源和软伽马重复源的物体通常被识别为磁星，具有超强磁场的中子星。到目前为止，这些天体的旋转历史还没有揭示出自由进动的证据。与此同时，这些天体的磁轴一般不会与它们的自旋轴平行或正交。在本文中，我们表明，这两个观测的组合，再加上简单的刚体动力学，导致非平凡的预测磁星的内部属性：（i）磁星地壳的弹性应力接近理论上限，地壳物质产量或（ii）有一个“钉扎”超流成分在磁星内部。作为这些想法的一个潜在的可观察的结果，我们指出，在没有钉扎超流的情况下，比目前观察到的更强磁场强度的磁星必须是几乎对齐/正交的旋转体。
英文摘要：
The objects known as anomalous X-ray pulsars and soft gamma repeaters are commonly identified with magnetars, neutron stars with ultrastrong magnetic fields. The rotational history of these objects has, so far, revealed no evidence of free precession. At the same time these objects do not generally appear to have magnetic axes nearly parallel or orthogonal to their spin axes. In this paper we show that the combination of these two observations, together with simple rigid-body dynamics, leads to non-trivial predictions about the interior properties of magnetars: either (i) elastic stresses in magnetar crusts are close to the theoretical upper limit above which the crustal matter yields or (ii) there is a "pinned" superfluid component in the magnetar interior. As a potentially observable consequence of these ideas we point out that, in the case of no pinned superfluidity, magnetars of stronger magnetic field strength than those currently observed would have to be nearly aligned/orthogonal rotators.
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