论文标题
高质量X射线二进制4U 2206 +54/BD +53 2790的起源
The origin of the high-mass X-ray binary 4U 2206+54/BD +53 2790
论文作者
论文摘要
Based on the Gaia EDR3 astrometric parameters and our new systemic radial velocity of the high-mass X-ray binary 4U 2206+54/BD+53 2790, we studied the trace back motion of the system and propose that it originated in the subgroup of the Cepheus OB1 association (Age~4-10 Myr) with its brightest star BD+53 2820 (B0V; l〜 $ 10^{4.7} $ l $ _ \ odot $）。 4U 2206+54的运动年龄约为2.8 $ \ pm $ 0.4 MYR，相对于该成员Star（BD+53 2820），距离为3.1-3.3 kpc，空间速度为75-100 km/s。这个失控的速度表明，在超新星爆炸期间，由4U 2206+54托管的中子星的祖先损失了约4-9 $ m _ {\ odot} $，而后者则获得了至少200-350 km/s的踢球速度。由于高质量X射线二进制4U 2206+54/bd+53 2790出生于CEP OB1亚组的成员，因此系统中最初最庞大的恒星终止了〜7-9 MYR之内的演变，对应于初始质量> = 32 $ M _ {\ odot} $。
Based on the Gaia EDR3 astrometric parameters and our new systemic radial velocity of the high-mass X-ray binary 4U 2206+54/BD+53 2790, we studied the trace back motion of the system and propose that it originated in the subgroup of the Cepheus OB1 association (Age~4-10 Myr) with its brightest star BD+53 2820 (B0V; L~$10^{4.7}$L$_\odot$). The kinematic age of 4U 2206+54 is about 2.8$\pm$0.4 Myr, it is at a distance of 3.1-3.3 kpc and has a space velocity of 75-100 km/s with respect to this member star (BD+53 2820) of the Cep OB1 association. This runaway velocity indicates that the progenitor of the neutron star hosted by 4U 2206+54 lost about 4-9 $M_{\odot}$ during the supernova explosion and the latter one received a kick velocity of at least 200-350 km/s. Since the high-mass X-ray binary 4U 2206+54/BD+53 2790 was born as a member of a subgroup of Cep OB1, the initially most massive star in the system terminated its evolution within ~7-9 Myr, corresponding to an initial mass >= 32$M_{\odot}$.
