Science. 1985 May 24;228(4702):1015-6. doi: 10.1126/science.228.4702.1015.
Pulsars with pulsation periods in the millisecond range are thought to be neutron stars that have acquired an extraordinarily short spin period through the accretion of stellar material spiraling down onto the neutron star from a nearby companion. Nearly all the angular momentum and most of the mass of the companion star is transferred to the neutron star. During this process, wherein the neutron star consumes its companion, it is required that a disk of stellar material be formed around the neutron star. In conventional models it is supposed that the disk is somehow lost when the accretion phase is finished, so that only the rapidly spinning neutron star remains. However, it is possible that, after the accretion phase, a residual disk remains in stable orbit around the neutron star. The end result of such an accretion process is an object that looks much like a miniature (about 100 kilometers), heavy version of Saturn: a central object (the neutron star) surrounded by a durable disk.
毫秒脉冲星被认为是通过吸积物质从附近伴星螺旋下降到中子星而获得极短自转周期的中子星。几乎所有伴星的角动量和大部分质量都转移到了中子星上。在这个过程中，当中子星消耗其伴星时，需要在中子星周围形成一个恒星物质盘。在传统模型中，假设在吸积阶段结束时，磁盘会以某种方式丢失，因此只剩下快速旋转的中子星。然而，在吸积阶段之后，残留的磁盘可能会稳定地绕着中子星运行。这种吸积过程的最终结果是一个看起来非常像微型（约 100 公里）、重版土星的物体：一个中央物体（中子星）被一个持久的磁盘包围着。
