什么时候明星会去BOOM？
When Do Stars Go BOOM?
摘要：
恒星产生白矮星的最大质量是一个重要的天体物理量。建立这一极限的最佳方法之一是在年轻星团中寻找WD，其中只有大质量恒星有时间演化，并且可以从WD的冷却时间以及星团的年龄来确定祖先的质量。到目前为止，年轻的银河系星团中的WD成员的质量还没有超过1.1 $~M_{\odot}$，远低于$1.38~M_{\odot}$的拉塞卡质量，也没有质量超过$6~M_{\odot}$的祖先。然而，寻找逃离集群环境的潜在大规模WD产生了有趣的候选者。为了进一步扩大星团样本，我们使用HST在麦哲伦星云中调查了四个年轻的大质量星团，寻找可能从质量为10 $~M_{\odot}$的恒星演化而来的明亮WD。我们位于五个潜在的WD候选人在最古老的四个集群检查，迄今发现的第一个河外单个WD。由于这些热的WD在光学波长下非常微弱，最终的确认可能需要等待30米级望远镜的光谱学。
英文摘要：
The maximum mass of a star that can produce a white dwarf (WD) is an important astrophysical quantity. One of the best approaches to establishing this limit is to search for WDs in young star clusters in which only massive stars have had time to evolve and where the mass of the progenitor can be established from the cooling time of the WD together with the age of the cluster. Searches in young Milky Way clusters have not thus far yielded WD members more massive than about 1.1$~M_{\odot}$, well below the Chandrasekhar mass of $1.38~M_{\odot}$, nor progenitors with masses in excess of about $6~M_{\odot}$. However, the hunt for potentially massive WDs that escaped their cluster environs is yielding interesting candidates. To expand the cluster sample further, we used HST to survey four young and massive star clusters in the Magellanic Clouds for bright WDs that could have evolved from stars as massive as 10$~M_{\odot}$. We located five potential WD candidates in the oldest of the four clusters examined, the first extragalactic single WDs thus far discovered. As these hot WDs are very faint at optical wavelengths, final confirmation will likely have to await spectroscopy with 30-metre class telescopes.
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。
