Extreme Mass Loss in Low-mass Type Ib/c Supernova Progenitors
Extreme Mass Loss in Low-mass Type Ib/c Supernova Progenitors
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DOI：
10.3847/2041-8213/ac9b3d
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发表时间：
2022-10
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影响因子：
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通讯作者：
Samantha C. Wu;J. Fuller
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文献类型：
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作者：
Samantha C. Wu;J. Fuller
许多核坍缩超新星（SNe）的氢和低质量的喷出物，如超剥离SNe和类型Ibn的SNe，被观察到与致密的星周物质（CSM）的相互作用。这些事件可能是由氦星的核心坍缩引起的，这些氦星已经被一个双星伴星严重剥离，并在其生命的最后几周到几年内喷射出大量物质。在氦星星模型运行到天之前，核心崩溃，我们确定了一个范围的氦核心质量为2.5-3 M，其信封大幅扩大，由于氦壳燃烧，而核心经历氖和氧燃烧。当以双星系统为模型时，这些氦星的快速膨胀导致了极高的后期质量转移率（M现在为10− 2 M yr−1），在核心坍缩前的几周到几十年开始。我们考虑在这些系统中产生CSM的两种情况：要么质量传递保持稳定，质量损失是从系统中的吸积同伴附近的驱动器，或质量传递变得不稳定，并导致一个共同的信封事件（CEE）通过该氦信封是未绑定的。由此得出的CSM性质与超剥离SNe和几个Ibn型SNe的CSM质量（<$10 −2-1 M）和半径（<$1013 -1016 cm）一致。此外，经历CEE的系统可能会产生短周期的中子星星双星，在不到1亿年的时间内合并。
Many core-collapse supernovae (SNe) with hydrogen-poor and low-mass ejecta, such as ultra-stripped SNe and type Ibn SNe, are observed to interact with dense circumstellar material (CSM). These events likely arise from the core collapse of helium stars that have been heavily stripped by a binary companion and have ejected significant mass during the last weeks to years of their lives. In helium star models run to days before core collapse we identify a range of helium core masses ≈2.5–3 M ⊙ whose envelopes expand substantially due to the helium shell burning while the core undergoes neon and oxygen burning. When modeled in binary systems, the rapid expansion of these helium stars induces extremely high rates of late-stage mass transfer ( Ṁ≳10−2M⊙yr−1 ) beginning weeks to decades before core collapse. We consider two scenarios for producing CSM in these systems: either mass transfer remains stable and mass loss is driven from the system in the vicinity of the accreting companion, or mass transfer becomes unstable and causes a common envelope event (CEE) through which the helium envelope is unbound. The ensuing CSM properties are consistent with the CSM masses (∼10−2–1 M ⊙) and radii (∼1013–1016 cm) inferred for ultra-stripped SNe and several type Ibn SNe. Furthermore, systems that undergo a CEE could produce short-period neutron star binaries that merge in less than 100 Myr.