射电磁星的基本面
The fundamental plane for radio magnetars
摘要：
高磁场是中子星的一个显著特征，在过去几十年里，人们已经认识到存在着超磁化中子星（或磁星）的源（软伽马中继器和异常X射线源）。磁星被认为是由磁能驱动的，而不是像普通的射电望远镜那样由旋转驱动的。直到最近，无线电静默和磁场通常高于量子临界值（Bq~4.4x10 ^{13} G），是磁星的特征属性之一。最近发现的无线电脉冲发射从其中的几个，和一个低偶极磁场软伽马中继器，进一步削弱了一个干净的分离之间的想法正常的恒星和磁星。在这封信中，我们表明磁星的无线电发射可能是由旋转能驱动的，类似于正常的无线电磁星中发生的情况。磁星无线电发射的特殊特征应该在这些源的复杂磁几何中追踪。此外，我们建议，磁星的无线电活动或不活动，可以预测从恒星的旋转周期，其时间导数和静态X射线光度的知识。
英文摘要：
High magnetic fields are a distinguishing feature of neutron stars and the existence of sources (the soft gamma repeaters and the anomalous X-ray pulsars) hosting an ultra-magnetized neutron star (or magnetar) has been recognized in the past few decades. Magnetars are believed to be powered by magnetic energy and not by rotation, as with normal radio pulsars. Until recently, the radio quietness and magnetic fields typically above the quantum critical value (Bq~4.4x10^{13} G), were among the characterizing properties of magnetars. The recent discovery of radio pulsed emission from a few of them, and of a low dipolar magnetic field soft gamma repeater, weakened further the idea of a clean separation between normal pulsars and magnetars. In this Letter we show that radio emission from magnetars might be powered by rotational energy, similarly to what occurs in normal radio pulsars. The peculiar characteristics of magnetars radio emission should be traced in the complex magnetic geometry of these sources. Furthermore, we propose that magnetar radio activity or inactivity can be predicted from the knowledge of the star's rotational period, its time derivative and the quiescent X-ray luminosity.
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