论文标题
从其外壳中哄骗剥落的二进制V367 cygni
Coaxing the Eclipsing Binary V367 Cygni Out of Its Shell
论文作者
论文摘要
W Serpentis System V367 Cygni提出了覆盖0.63-0.69UM的光谱〜17000。在圆周系统外壳中形成的FEII和SIII的吸收线是突出的特征，它们的深度随时间稳定，这表明壳平滑地分布和混杂。均匀性的进一步证据来自在壳线的最深部分中测得的适度径向速度变化。建议先前归因于壳旋转的动作是供体星光谱中污染的伪像。提取了供体星光谱，与早期至中巨人的光谱相一致。供体光谱中金属线的深度随轨道相变化，这表明斑点活性覆盖了该恒星表面的很大一部分。还提取了围绕第二颗恒星的积聚磁盘的光谱，并注意到Herbig ae/Be恒星的发射光谱。除了具有轨道相的变化外，H $α$随着时间标准不超过两个轨道而变化。 HEI 6678发射的暂定检测是接近初级最小值，但在其他阶段不进行。最后，从v367 CYG中及其周围的热尘发射的预计发射是更多或无对称的对称性，并且在系统距离处延伸超过28个Arcsec或0.09 PC-V367 CYG因此将物质驱逐到大量的周围空间中。
Spectra that cover 0.63 - 0.69um with a spectral resolution ~ 17000 are presented of the W Serpentis system V367 Cygni. Absorption lines of FeII and SiII that form in a circumsystem shell are prominent features, and the depths of these are stable with time, suggesting that the shell is smoothly distributed and well-mixed. Further evidence of uniformity comes from modest radial velocity variations measured in the deepest parts of the shell lines. It is suggested that motions previously attributed to rotation of the shell are instead artifacts of contamination from the donor star spectrum. A donor star spectrum is extracted that is consistent with that of an early to mid-A giant. The depths of metallic lines in the donor spectrum vary with orbital phase, suggesting that spot activity covers a large fraction of the surface of that star. A spectrum of the accretion disk that surrounds the second star is also extracted, and similarities are noted with the emission spectra of Herbig Ae/Be stars. In addition to variations with orbital phase, H$α$ changes with time over timescales of no more than two orbits. A tentative detection of HeI 6678 emission is made near primary minimum, but not at other phases. Finally, projected emission from hot dust in and around V367 Cyg is more-or-less symmetric and extends over 28 arcsec, or 0.09 pc at the distance of the system -- V367 Cyg is thus expelling matter into a large volume of the surrounding space.
