The three types of high-mass X-ray pulsator
The three types of high-mass X-ray pulsator
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DOI：
10.1093/mnras/220.4.1047
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发表时间：
1986-06
影响因子：
4.8
通讯作者：
R. Corbet
中科院分区：
文献类型：
--
作者：
R. Corbet
高质量X射线脉动器根据其观测特性可分为三个不同的组：1）Be星系统，2）具有长脉冲周期（〜102 - 103 s）的非Be星系统，以及3）具有短脉冲周期（〜100 - 101 s）的非Be星系统。利用各组之间传质过程的差异来解释不同的特性。将高质量脉动器分为三个明确定义的组，如果仅知道脉动器的一些参数，则可以预测脉动器的一些特性。因此，X 射线源 H0850-42、OAO1653-40 和 1E1048.1-5937 的光学对应物预计要么是 Be 星，要么是低质量双星（可能性较小）。短周期系统的轨道（Po）和自旋（Ps）周期可能是反相关的，中间极性白矮星双星也表现出这种现象。对于长周期系统，Po 和 Ps 之间并不像 Be 星系统那样具有很强的关系。结果表明，对于 Be 星系统，如果这些系统中中子星的阿尔文半径和共转半径相等，则这种关系不能用恒星风的吸积来解释。然而，不排除来自非膨胀大气的吸积。超巨星系统的 Ps 和 Po 之间缺乏任何相关性，是由于吸积物质的角动量较低。然而，Be 星系统可能会产生显着的角动量，从而形成吸积盘。
High mass X-ray pulsators are shown to be divisible into three distinct groups on the basis of their observational properties: 1) the Be star systems, 2) non-Be star systems with long pulse periods, (~102 — 103 s), and 3) non-Be star systems with short pulse periods (~100 — 101 s). Differences in mass transfer processes between the groups are invoked to account for the different properties. The separation of high mass pulsators into three clearly defined groups enables some of the properties of a pulsator to be predicted if only a few of its parameters are known. Because of this the optical counterparts of the X-ray sources H0850-42, OAO1653-40 and 1E1048.1-5937 are predicted to be either Be stars or, much less likely, low mass binaries. The orbital (Po) and spin (Ps) periods of the short period systems may be anti-correlated, a phenomenon which is also exhibited by the intermediate polar white dwarf binaries. For the long period systems there is no strong relationship between Po and Ps as there is for the Be star systems. It is shown that for the Be star systems this relationship cannot be accounted for by accretion from a stellar wind if there is equality between the Alfven and corotation radii of the neutron stars in these systems. However, accretion from a non-expanding atmosphere is not excluded. The lack of any correlation between Ps and Po for the supergiant systems is attributed to the low angular momentum of accreted matter. The Be star systems, however, probably accrete significant angular momentum which can result in an accretion disk.