Be X射线双星
Be X射线双星是一种高质量X射线双星，由一颗中子星和一颗Be星组成。通常中子星会以一个广阔的椭圆轨道环绕着Be星，而Be星的星风亦多会形成一个与中子星轨道交错的平面。每当中子星与Be星的星风相遇时，大量气体便依附在中子星上。气体会下沉到中子星并产生一股强烈的X射线。[1]
LSI+61°303
LSI+61°303，亦即周期性伽玛射线源CG135+01，有可能是这种双星的例子。其每26.496天便会发出无线电波。可见光和红外线的波长变动周期亦为26.5天。[2]其致密天体的质量未被准确测出，但推定它因其巨大质量并非中子星而是黑洞。[3]
英仙座X
英仙座X是由仙后座γ变星和脉冲星组成的双星，其X射线周期较长和较稳定。但也观测到一些X射线的闪焰，相信是由于吸积盘的变动，但未有发现其与光学变动的关联。[4]
至1996年达Be X射线双星级别的20多个天体中惟LSI+61°303及英仙座X发出明显较高光度及频率的X射线（kT ≈ 10–20 keV，对比其他的kT ≤ 1 keV）。LSI+61°303亦发出强烈的无线电波，使其近似于其他短周期高质量X射线双星。[2]
参考
- ^ Reig, Pablo. Be/X-ray binaries. Astrophysics and Space Science. 2011, 332: 1. Bibcode:2011Ap&SS.332....1R. arXiv:1101.5036
. doi:10.1007/s10509-010-0575-8.
- ^ 2.0 2.1 Taylor AR, Young G, Peracaula M, Kenny HT, Gregory PC. An X-ray outburst from the radio emitting X-ray binary LSI+61°303. Astron Astrophys. 1996, 305: 817–24. Bibcode:1996A&A...305..817T.
- ^ Taylor AR, Young G, Peracaula M, Kenny HT, Gregory PC. An X-ray outburst from the radio emitting X-ray binary LSI+61°303. Astron. Astrophys. 1996, 305: 817–24. Bibcode:1996A&A...305..817T.
- ^ Massi, M; Migliari, S; Chernyakova, M. The black hole candidate LS I +61°0303. Monthly Notices of the Royal Astronomical Society. 2017, 468 (3): 3689. Bibcode:2017MNRAS.468.3689M. arXiv:1704.01335 . doi:10.1093/mnras/stx778.
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