Formation of very strongly magnetized neutron stars - Implications for gamma-ray bursts
Formation of very strongly magnetized neutron stars - Implications for gamma-ray bursts
复制标题
DOI：
10.1086/186413
复制
发表时间：
1992-06
期刊：
影响因子：
--
通讯作者：
R. Duncan;C. Thompson
中科院分区：
文献类型：
--
作者：
R. Duncan;C. Thompson
有人提出，磁星（高场中子星）的主要观测特征是由其巨大的磁能储备提供动力的伽马射线爆发。如果它们获得很大的反冲力，大多数磁星就会脱离银河系，或者驻留在延伸的、弱束缚的银河日冕中。有证据表明软伽马中继器是年轻的磁星。有人认为，对流发电机在中子星双星合并后也能产生非常强的偶极子场，但前提是合并后的恒星存活时间长达约 10-100 毫秒。讨论了几种可以在这些恒星诞生时赋予其足以逃离银盘的大反冲力的机制。
It is proposed that the main observational signature of magnetars, high-field neutron stars, is gamma-ray bursts powered by their vast reservoirs of magnetic energy. If they acquire large recoils, most magnetars are unbound from the Galaxy or reside in an extended, weakly bound Galactic corona. There is evidence that the soft gamma repeaters are young magnetars. It is argued that a convective dynamo can also generate a very strong dipole field after the merger of a neutron star binary, but only if the merged star survives for as long as about 10-100 ms. Several mechanisms which could impart a large recoil to these stars at birth, sufficient to escape from the Galactic disk, are discussed.