Joint Hα and X-Ray Observations of Massive X-Ray Binaries. III. The Be X-Ray Binaries HDE 245770 = A0535+26 and X Persei
Joint Hα and X-Ray Observations of Massive X-Ray Binaries. III. The Be X-Ray Binaries HDE 245770 = A0535+26 and X Persei
复制标题
大型 X 射线双星的 Hα 和 X 射线联合观测 III。
DOI：
10.1086/514325
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发表时间：
2007
期刊：
影响因子：
--
通讯作者：
R. Zaballa
中科院分区：
文献类型：
--
作者：
E. Grundstrom;E. Grundstrom;T. Boyajian;T. Boyajian;C. Finch;D. Gies;D. Gies;Wenjin Huang;Wenjin Huang;Wenjin Huang;M. McSwain;D. O'Brien;R. L. Riddle;R. L. Riddle;M. Trippe;S. Williams;S. Williams;D. Wingert;D. Wingert;R. Zaballa
本文介绍了Be X射线双星HDE 245770 = A0535+26和X Per的Hα监测结果。我们使用的Hα等效宽度与所采用的值的Be星星的有效温度，磁盘倾角，和磁盘的外边界，以确定作为时间的函数的磁盘的半最大发射半径。HDE 245770的观测记录了快速的光谱变化，这显然伴随着一个新的周星盘的再生。该磁盘在1998-2000年期间迅速增长，但随后几年增长放缓。外盘半径可能被盘气体和中子星星轨道周期之间的共振截断。最近的两次X射线爆发似乎与过去十年中达到的最大磁盘半最大发射半径相吻合。我们对X Per的观测表明，它的拱星盘最近已经增长到接近记录的比例，同时该系统的X射线通量急剧增加，这可能是盘的质量吸积增强的结果。我们发现，围绕X Per的圆盘的Hα半最大发射半径达到了大约6倍于恒星半径的大小，然而，这个值远低于Be星星和中子星星之间的最小距离。我们认为，在近星点的潮汐相互作用激发的螺旋臂可能有助于解除磁盘气体半径的中子星星同伴吸积变得更有效。
We present results from an Hα monitoring campaign of the Be X-ray binary systems HDE 245770 = A0535+26 and X Per. We use the Hα equivalent widths together with adopted values of the Be star effective temperature, disk inclination, and disk outer boundary to determine the half-maximum emission radius of the disk as a function of time. The observations of HDE 245770 document the rapid spectral variability that apparently accompanied the regeneration of a new circumstellar disk. This disk grew rapidly during the years 1998-2000, but then slowed in growth in subsequent years. The outer disk radius is probably truncated by resonances between the disk gas and neutron star orbital periods. Two recent X-ray outbursts appear to coincide with the largest disk half-maximum emission radius attained over the last decade. Our observations of X Per indicate that its circumstellar disk has recently grown to near-record proportions, and concurrently the system has dramatically increased in X-ray flux, presumably the result of enhanced mass accretion from the disk. We find that the Hα half-maximum emission radius of the disk surrounding X Per reached a size about 6 times larger than the stellar radius, a value, however, that is well below the minimum separation between the Be star and neutron star. We suggest that spiral arms excited by tidal interaction at periastron may help lift disk gas out to radii where accretion by the neutron star companion becomes more effective.
DOI：
10.1007/s00159-013-0069-0
发表时间：
2003-10
影响因子：
3.5
作者：
J. Porter;T. Rivinius
通讯作者：
J. Porter;T. Rivinius