标题： 重新审视碳丰富沃夫-拉叶双星的尘埃产生影响 显示英文标题

标题： Revisiting the Impact of Dust Production from Carbon-Rich Wolf-Rayet Binaries

摘要： 我们提出了一个尘埃谱能量分布（SED）和双星群体分析，重新审视了碳丰富沃尔夫-拉叶（WC）双星风中的尘埃产生率（DPR）及其对星系尘埃预算的影响。对19个银河系WC“尘埃星”的DustEM SED模型显示了$\dot{M}_d\sim10^{-10}-10^{-6}$ M$_\odot$ 年$^{-1}$的DPRs 和$\chi_C$的碳尘凝结分数，范围在$0.002 - 40\%$。 有利于高效尘埃星的大型（$0.1 - 1.0$$\mu$m）尘粒尺寸组成，其中$\chi_C\gtrsim1\%$。 已知轨道周期的尘埃星结果验证了$\chi_C$、轨道周期、WC质量损失率和风速之间的幂律关系，这与碰撞风双星中尘埃形成理论模型的预测一致。 我们将尘埃产生纳入双星群体和光谱综合（BPASS）模型，以分析WC尘埃星、渐近巨星分支星（AGB）、红超巨星（RSG）和核心坍缩超新星（SN）的尘埃产生率。 假设恒定恒星形成（SF）和同时期$10^6$M$_\odot$星族的BPASS模型在低、类似大麦哲伦云（LMC）和太阳金属丰度（Z = 0.001、0.008 和 0.020）下进行了计算。 无论是恒定恒星形成还是同时期模型都表明，超新星在所有金属丰度下都是净尘埃破坏者。 恒星形成率(SF)模型在类似大麦哲伦云(LMC)金属丰度的情况下表明，渐近巨星分支(AGB)星的尘埃产出量略高于沃尔夫-拉耶(WC)双星和红超巨星(RSG)，产出比为$2-3$，而在太阳金属丰度下，WC双星在 $\sim60$百万年内一直是主要的尘埃来源，直到AGB星开始贡献尘埃，其尘埃输入量与WC双星相当。 同时期的群体模型显示，在“爆发性”恒星形成情况下，AGB星在晚期（约$t\gtrsim 70$百万年）主导尘埃生产。 显示英文摘要

摘要： We present a dust spectral energy distribution (SED) and binary stellar population analysis revisiting the dust production rates (DPRs) in the winds of carbon-rich Wolf-Rayet (WC) binaries and their impact on galactic dust budgets. DustEM SED models of 19 Galactic WC ``dustars" reveal DPRs of $\dot{M}_d\sim10^{-10}-10^{-6}$ M$_\odot$ yr$^{-1}$ and carbon dust condensation fractions, $\chi_C$, between $0.002 - 40\%$. A large ($0.1 - 1.0$ $\mu$m) dust grain size composition is favored for efficient dustars where $\chi_C\gtrsim1\%$. Results for dustars with known orbital periods verify a power-law relation between $\chi_C$, orbital period, WC mass-loss rate, and wind velocity consistent with predictions from theoretical models of dust formation in colliding-wind binaries. We incorporated dust production into Binary Population and Spectral Synthesis (BPASS) models to analyze dust production rates from WC dustars, asymptotic giant branch stars (AGBs), red supergiants (RSGs), and core-collapse supernovae (SNe). BPASS models assuming constant star formation (SF) and a co-eval $10^6$ M$_\odot$ stellar population were performed at low, Large Magellanic Cloud (LMC)-like, and solar metallicities (Z = 0.001, 0.008, and 0.020). Both constant SF and co-eval models show that SNe are net dust destroyers at all metallicities. Constant SF models at LMC-like metallicities show that AGB stars slightly outproduce WC binaries and RSGs by factors of $2-3$, whereas at solar metallicites WC binaries are the dominant source of dust for $\sim60$ Myr until the onset of AGBs, which match the dust input of WC binaries. Co-eval population models show that for "bursty" SF, AGB stars dominate dust production at late times ($t\gtrsim 70$ Myr).