标题： 一个麦哲伦云中的超软X射线双星系统 显示英文标题

标题： A Supersoft X-Ray Binary in the Small Magellanic Cloud

摘要： 光度观测结果表明，在两年内获得的超软X射线源1E 0035.4-7230显示，非常蓝的光学对应体（V(maximum)=20.2，B-V=-0.15，U-B=-1.06）经历近正弦变化，周期为0.1719256天，振幅为Delta V~0.3星等。 ROSAT观测显示X射线也以大约相同的周期变化。 然而，X射线最小值可能比光学最小值提前约四分之一周期，或者两个波长区域之间存在小的周期差异。 我们认为这个X射线源是一个密近双星系统，光学光主要来自围绕致密星的吸积盘。 光学光谱显示弱而可变的He II（4686埃）发射，这可能起源于该盘。 讨论了光变曲线的可能解释，包括X射线加热次级星。 X射线光变曲线中的非常宽的最小值表明X射线可能在较大的吸积盘冕（ADC）中散射，该冕部分被遮挡，可能是由于盘边缘的方位不规则凸起。 如果该系统位于大麦哲伦星云的距离，则其辐射接近爱丁顿光度。 显示英文摘要

摘要： Photometric observations of the supersoft X-ray source 1E 0035.4-7230 obtained during two years reveal that the very blue optical counterpart (V (maximum)=20.2, B-V=-0.15, U-B=-1.06) undergoes nearly sinusoidal variations with a period of 0.1719256 days and an amplitude of Delta V~0.3 mag. ROSAT observations show the X-rays vary with approximately the same period. However, either the X-ray minimum precedes the optical minimum by about a quarter cycle or there is a small period difference between the two wavelength regions. We consider that this X-ray source is a close binary, with the optical light coming primarily from an accretion disk surrounding the compact star. Optical spectra show weak, variable He II (4686 Angstrom) emission which probably originates in this disk. Possible interpretations of the light curve are discussed, including X-ray heating of the secondary star. The very broad minimum in the X-ray light curve suggests the X-rays may be scattered in a large accretion disk corona (ADC) which is partially occulted, probably by an azimuthally irregular bulge on the disk rim. If this system lies at the distance of the Small Magellanic Cloud, it radiates near the Eddington luminosity.