QU隆凸：一个SNeIa的祖先？
QU Carinae: a SNeIa progenitor?
摘要：
在2006年至2007年获得的新星样激变变量QU车的光学光谱的径向速度，线轮廓，和线识别进行了研究。我们无法证实1982年以来所报告的10.9小时轨道周期，部分原因是我们的采样对于这一目的并不理想，而且我们怀疑，因为我们的径向速度因不稳定的风引起的线轮廓变化而扭曲。P-Cygni配置文件中发现的几个发射线，包括那些C IV。光谱中有丰富的碳谱线，表明施主星中有碳富集。[O III] 5007和[N II] 6584的存在可能是由于系统附近的弥漫星云。在光谱中的风签名和星云线的存在是一致的吸积风演化的情况下，已建议导致SNeIa。我们认为，QU车是CV的V Sge子类的成员，和一个可能的SNeIa祖。结果表明，QU Car最近的光变曲线具有约1等的低态，与V Sge的光变曲线相似，加强了QU Car与V Sge星、超软X射线源和SNeIa祖星的联系。
英文摘要：
Optical spectra obtained in 2006-07 of the nova-like cataclysmic variable QU Car are studied for radial velocities, line profiles, and line identifications. We are not able to confirm the reported 10.9 hr orbital period from 1982,partly because our sampling is not ideal for this purpose and also, we suspect, because our radial velocities are distorted by line profile changes due to an erratic wind. P-Cygni profiles are found in several of the emission lines, including those of C IV. Carbon lines are abundant in the spectra, suggesting a carbon enrichment in the doner star. The presence of [O III] 5007Åand [N II] 6584Åis likely due to a diffuse nebula in the vicinity of the system. The wind signatures in the spectra and the presence of nebular lines are in agreement with the accretion wind evolution scenario that has been suggested to lead to SNeIa. We argue that QU Car is a member of the V Sge subclass of CVs, and a possible SNeIa progenitor. It is shown that the recent light curve of QU Car has ~1 mag low states, similar to the light curve of V Sge, strengthening the connection of QU Car with V Sge stars, supersoft x-ray sources, and SNeIa progenitors.
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