Neutrinos from Relativistic Outflows of Fast Spinning Magnetars
Neutrinos from Relativistic Outflows of Fast Spinning Magnetars
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DOI：
10.1071/as04069
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发表时间：
2005-04
影响因子：
6.3
通讯作者：
Q. Luo
中科院分区：
文献类型：
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作者：
Q. Luo
脉冲星的自转周期很短，只有几毫秒，磁场通过发电机过程放大到1015-1016 g。这种毫秒磁星的自转速度很快，释放出高能中微子和伽马射线。具体来说，离子在极隙（如在正常脉冲星中）和相对论性磁星风中的加速被考虑。在这两种情况下，离子都可以被加速到超高能量，这些高能离子可以通过与来自热中子星的热辐射或作为磁星风沉积能量的恒星外壳的加热内边界区域的相互作用而导致高能中微子和伽马射线的产生。讨论了计划中的冰立方中微子观测站等千米尺度中微子探测器对中微子通量的可探测性。
Abstract Pulsars may be born with a short rotation period of milliseconds with the magnetic field amplified through dynamo processes up to ∼1015–1016 G. Such millisecond magnetars spin down rapidly, emitting bursts of high-energy neutrinos and gamma rays. Specifically, acceleration of ions in both the polar gap (as in a normal pulsar) and the relativistic magnetar wind is considered. In both cases ions can be accelerated to ultra-high energies and these energetic ions can lead to production of high-energy neutrinos and gamma rays through interaction with thermal radiation from the hot neutron star or the heated inner boundary region of the stellar envelope as the result of the deposition of energy by the magnetar wind. The detectability of the neutrino flux by a kilometre-scale neutrino detector such as the planned IceCube neutrino observatory is discussed.