论文标题
在超新星残留物中高质量X射线二进制中的年轻增值中子星的起源
Origin of young accreting neutron stars in high-mass X-ray binaries in supernova remnants
论文作者
论文摘要
最近，已经发现了超新星残留物内部X射线二进制系统中的几位中子星（NSS）。它们代表了NSS的标准磁旋转演变的难题，因为它们的年龄（$ \ lyssim 10^5 $年）比风能增强发作之前的弹出器和螺旋桨阶段的预期持续时间短得多。为了解释这种系统的外观，我们考虑了NSS的旋转演变，并在弹出器和螺旋桨阶段之间的前进/向后转变中具有早期回累和不对称性（所谓的Shysteresis效应，V。Shvartsman于1970年提出了所谓的滞后作用）。结果表明，在成功的后备发作中具有初始自旋时期的某些现实值，恒星风质和磁场后，年轻的NS可能不会在其演变过程中进入喷射器阶段，从而导致超级诺沃省残余物的生命周期内相对较快地开始增生。对于标准磁场，$ \ sim 10^{12} $ 〜g和初始旋转期$ \ sim 0.1 $ 〜- 〜0.2〜s增生率$ \ gtrsim 10^{14} $ 〜-〜 $ 10^{15} $ 10^{15} $ 〜g〜s $^s $^{ - 1} $足以避免弹出器阶段。
Recently, several accreting neutron stars (NSs) in X-ray binary systems inside supernova remnants have been discovered. They represent a puzzle for the standard magneto-rotational evolution of NSs, as their ages ($\lesssim 10^5$ years) are much shorter than the expected duration of Ejector and Propeller stages preceding the onset of wind accretion. To explain appearance of such systems, we consider rotational evolution of NSs with early fallback accretion and asymmetry in forward/backward transitions between Ejector and Propeller stages (so-called hysteresis effect proposed by V. Shvartsman in 1970). It is shown that after a successful fallback episode with certain realistic values of the initial spin period, stellar wind properties, and magnetic field, a young NS may not enter the Ejector stage during its evolution which results in a relatively rapid initiation of accretion within the lifetime of a supernova remnant. For a standard magnetic field $\sim 10^{12}$~G and initial spin period $\sim 0.1$~--~0.2~s accretion rate $\gtrsim 10^{14}$~--~$10^{15}$~g~s$^{-1}$ is enough to avoid the Ejector stage.
