Ia型超新星酝酿过程中的中子化
Neutronization During Type Ia Supernova Simmering
摘要：
在一颗白矮星（WD）燃烧成Ia型超新星（SN Ia）之前，这颗恒星在一个对流的碳燃烧区“沸腾”了大约1000年。我们发现，在这段时间内，弱相互作用使中子过剩量增加，其增加量取决于爆炸前燃烧的碳的总量。这一贡献是除了通过22 Ne丰度的金属丰度（Z）依赖的中子化（如Timmes，Brown和Truran所研究的）之外。主要结果是，当Z/Z_ \odot <2/3时，我们预计中子化水平会有一个下限，这个下限在金属丰度贡献中占主导地位，如果大量能量通过对流Urca过程损失给中微子，那么它对更大的金属丰度可能很重要。这将掩盖在低金属丰度时Ia超新星性质与银河系环境之间的任何相关性。此外，我们表明，最近的观测超新星Ia星系环境的依赖性清楚地表明，金属丰度本身不能提供充分观察到的事件的多样性。
英文摘要：
Prior to the incineration of a white dwarf (WD) that makes a Type Ia supernova (SN Ia), the star "simmers" for ~1000 years in a convecting, carbon burning region. We have found that weak interactions during this time increase the neutron excess by an amount that depends on the total quantity of carbon burned prior to the explosion. This contribution is in addition to the metallicity (Z) dependent neutronization through the 22Ne abundance (as studied by Timmes, Brown, & Truran). The main consequence is that we expect a floor to the level of neutronization that dominates over the metallicity contribution when Z/Z_\odot<2/3, and it can be important for even larger metallicities if substantial energy is lost to neutrinos via the convective Urca process. This would mask any correlations between SN Ia properties and galactic environments at low metallicities. In addition, we show that recent observations of the dependences of SNe Ia on galactic environments make it clear that metallicity alone cannot provide for the full observed diversity of events.
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。
