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arXiv 1705.04487astro-ph.SR
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II型和反常造父变星的周期光度和周期半径关系

The period-luminosity and period-radius relations of Type II and anomalous Cepheids

Martin A. T. Groenewegen, Monika Jurkovic

备注：
A&A accepted
发表信息：
A&A 604, A29 (2017)
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摘要：

方法：在随附的论文（arXiv：1705.00886）中，我们通过构建光谱能量分布（SED）并将其与模型大气和尘埃辐射转移模型（在尘埃过量的情况下）拟合，确定了OGLE-III巡天中发现的LMC和SMC中335个T2 Cs和AC的光度和有效温度。基于这些结果，我们研究PL和PR关系。利用现有的脉动模型，我们推导出的周期光度质量温度金属丰度的关系，然后估计脉动质量的RR天琴座和经典造父变星。结果如下：T2 Cs的PL关系似乎并不依赖于金属丰度，并且，排除尘埃RV Tau星，是$M_{\rm bol}= +0.12 -1.78 \log P$（$P < 50$天）。还提出了基波和第一泛音LMC AC的关系。T2 C的PR关系也表现出很少或没有依赖于金属丰度或周期。我们的首选关系结合了SMC和LMC恒星以及所有T2 C子类，并且是$\log R = 0.846 + 0.521 \log P$。还提出了基波和第一泛音LMC AC的关系。对于短周期T2 Cs、BL Her亚型和AC，来自RR Lyeclium和经典造父变星脉动模型的脉动质量吻合良好，并且分别与文献中的估计值（即$M_{\rm BLH} \sim 0.49$ \msol \和$M_{\rm AC} ~\sim 1.3$ \msol）一致。W Vir星的质量与BL Her星相似，而pWVir星和RV Tau星的质量则不太清楚。对于许多RV Tau来说，质量与AGB后（单星）演化的标准图像相冲突，质量要么太大（$\gtrsim$ 1 \msol），要么太小（$\lesssim$ 0.4 \msol）。

英文摘要：

Method: In an accompanying paper (arXiv: 1705.00886) we determined luminosity and effective temperature for the 335 T2Cs and ACs in the LMC and SMC discovered in the OGLE-III survey, by constructing the spectral energy distribution (SED) and fitting this with model atmospheres and a dust radiative transfer model (in the case of dust excess). Building on these results we study the PL and PR relations. Using existing pulsation models for RR Lyrae and classical Cepheids we derive the period-luminosity-mass-temperature-metallicity relations, and then estimate the pulsation mass. Results: The PL relation for the T2Cs does not appear to depend on metallicity, and, excluding the dusty RV Tau stars, is $M_{\rm bol}= +0.12 -1.78 \log P$ (for $P < 50$ days). Relations for fundamental and first overtone LMC ACs are also presented. The PR relation for T2C also shows little or no dependence on metallicity or period. Our preferred relation combines SMC and LMC stars and all T2C subclasses, and is $\log R = 0.846 + 0.521 \log P$. Relations for fundamental and first overtone LMC ACs are also presented. The pulsation masses from the RR Lyrae and classical Cepheid pulsation models agree well for the short period T2Cs, the BL Her subtype, and ACs, and are consistent with estimates in the literature, i.e. $M_{\rm BLH} \sim 0.49$ \msol\ and $M_{\rm AC} ~\sim 1.3$ \msol, respectively. The masses of the W Vir appear similar to the BL Her. The situation for the pWVir and RV Tau stars is less clear. For many RV Tau the masses are in conflict with the standard picture of (single-star) post-AGB evolution, the masses being either too large ($\gtrsim$ 1 \msol) or too small ($\lesssim$ 0.4 \msol).

机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。

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