经典造父变星的质量为3至11 M $\odot$的理论预测，但那些测量，在3.6和5 M $\odot$之间的集群。因此，它们的质量-光度关系受到很差的约束，阻碍了我们对基本恒星物理和莱维特定律的理解。所有造父变星的质量都来自对11个双星系统的分析，其中只有5个是双线的，非常适合精确的动力学质量测定。我们提出了一个项目来分析一个新的，众多的造父变星在双线二进制（SB 2）系统提供质量测定在一个很宽的质量区间，并研究它们的演变。我们分析了一个样本的41个候选二进制LMC造父变星沿P-L关系，这可能是伴随着发光的红巨星，并提出间接和直接的指标，他们的二进制。在光谱研究的子样本的18个最明亮的候选人，为16个我们检测到线的两个组成部分的光谱，已经翻两番的造父变星的数量在SB 2系统。因此，对整个样本的观测可能会使目前所有的造父变星质量估计值增加四倍。对于我们的大多数候选人，不稳定的固有周期变化占主导地位的光旅行时间的影响，由于二进制。然而，后者可以解释四颗造父变星的周期性相位调制。我们的项目为LMC，银河系和其他星系中造父变星的未来精确动力学质量测定铺平了道路，这将有可能增加已知造父变星质量的数量，甚至是10倍，极大地提高了我们对这些重要恒星的了解。
英文摘要：
Masses of classical Cepheids of 3 to 11 M$\odot$ are predicted by theory but those measured, clump between 3.6 and 5 M$\odot$. As a result, their mass-luminosity relation is poorly constrained, impeding our understanding of basic stellar physics and the Leavitt Law. All Cepheid masses come from the analysis of 11 binary systems, including only 5 double-lined and well-suited for accurate dynamical mass determination. We present a project to analyze a new, numerous group of Cepheids in double-lined binary (SB2) systems to provide mass determinations in a wide mass interval and study their evolution. We analyze a sample of 41 candidate binary LMC Cepheids spread along the P-L relation, that are likely accompanied by luminous red giants, and present indirect and direct indicators of their binarity. In a spectroscopic study of a subsample of 18 brightest candidates, for 16 we detected lines of two components in the spectra, already quadrupling the number of Cepheids in SB2 systems. Observations of the whole sample may thus lead to quadrupling all the Cepheid mass estimates available now. For the majority of our candidates, erratic intrinsic period changes dominate over the light travel-time effect due to binarity. However, the latter may explain the periodic phase modulation for 4 Cepheids. Our project paves the way for future accurate dynamical mass determinations of Cepheids in the LMC, Milky Way, and other galaxies, which will potentially increase the number of known Cepheid masses even 10-fold, hugely improving our knowledge about these important stars.
A Galactic intermediate-mass stripped star with a Wolf-Rayet-like wind
Max-Planck-Institut für Astronomie（马克斯·普朗克天文学研究所）；Universität Heidelberg（海德堡大学）；California Institute of Technology（加州理工学院）；Boston University（波士顿大学）；University of California, Berkeley（加利福尼亚大学伯克利分校）；Max-Planck-Institut für Astrophysik（马克斯·普朗克天体物理学研究所）
