磁星的起源和演化
Origin and evolution of magnetars
摘要：
我们提出了一个人口合成研究的磁星，它允许X射线选择效应的观察到的属性，调查的假设，他们是从人口的祖先，更大的质量比那些正常的无线电hapsars。我们假设异常的X射线辐射是由一个不参与恒星自旋下降的环形场或纠缠场的衰变引起的。我们发现，我们可以解释所观察到的属性，如周期和场分布和周期-周期导数图，如果我们适当地参数化的异常X射线光度的时间演化为时间的指数衰减函数。要求中子星的磁通量是起源质量的强函数，磁星的质量范围为20-45太阳质量。与射电双星不同的是，由于磁星的快速自旋下降，磁星对出生自旋周期的约束很弱。我们的模型预测出生率约为每世纪0.15-0.3。
英文摘要：
We present a population synthesis study of the observed properties of the magnetars, which allows for X-ray selection effects, investigating the hypothesis that they are drawn from a population of progenitors that are more massive than those of the normal radio pulsars. We assume that the anomalous X-ray emission is caused by the decay of a toroidal or tangled up field that does not partake in the spin down of the star. We find that we can explain the observed properties, such as the period and field distributions and the Period - Period derivative diagram, if we suitably parametrise the time evolution of the anomalous X-ray luminosity as an exponentially decaying function of time. The magnetic flux of the neutron stars is required to be a strong function of the progenitor mass with the magnetars arising from the mass range 20-45 solar masses. Unlike with the radio pulsars, the magnetars only weakly constrain the birth spin period, due to their rapid spin-down. Our model predicts a birthrate of about 0.15-0.3 per century.
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