A hot and fast ultra-stripped supernova that likely formed a compact neutron star binary
A hot and fast ultra-stripped supernova that likely formed a compact neutron star binary
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DOI：
10.1126/science.aas8693
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发表时间：
2018-10
期刊：
影响因子：
56.9
通讯作者：
K. De;M. Kasliwal;E. Ofek;T. J. Moriya;Jamison Burke;Jamison Burke;Yi Cao;S. B. Cenko
中科院分区：
文献类型：
--
作者：
K. De;M. Kasliwal;E. Ofek;T. J. Moriya;Jamison Burke;Jamison Burke;Yi Cao;S. B. Cenko
中子星星的爆炸起源已知某些类型的核心坍缩超新星会产生中子星星（NS）。最近从它的引力波发射中检测到了一个双NS合并，但目前还不清楚如何形成这样一个紧密的双系统。德等人发现了一颗具有不寻常性质的核心坍缩超新星，包括在爆炸前去除了星星的外层。他们将其解释为已经包含一个NS的相互作用双星系统中的第二颗超新星。由于爆炸可能在一个紧密的轨道上产生了第二个NS（而不是黑洞），它可能是NS系统形成的一个例子。一颗不寻常的核心坍缩超新星似乎在紧密的轨道上形成了一颗双中子星星。致密中子星星双星系统是由大质量双星通过恒星演化产生的，其中包括两次超新星爆炸。这些系统形成的最后阶段还没有被直接观察到。我们报告了iPTF 14gqr（SN 2014 ft）的发现，这是一颗Ic型超新星，具有快速演化的光变曲线，表明其喷出物质量极低（太阳质量为0.2），动能也很低（1.2 × 1050尔格）。早期的光度学和光谱学揭示了扩展的富氦包层的冲击冷却的证据，可能是在爆炸前的一次强烈的质量损失事件中喷射出来的。综上所述，我们解释iPTF 14gqr作为超剥离超新星的证据，在紧凑的双星系统中形成中子星。
Explosive origin of a binary neutron star Some types of core-collapse supernovae are known to produce a neutron star (NS). A binary NS merger was recently detected from its gravitational wave emission, but it is unclear how such a tight binary system can be formed. De et al. discovered a core-collapse supernova with unusual properties, including the removal of the outer layers of the star before the explosion. They interpret this as the second supernova in an interacting binary system that already contains one NS. Because the explosion probably produced a second NS (rather than a black hole) in a tight orbit, it could be an example of how binary NS systems form. Science, this issue p. 201 An unusual core-collapse supernova appears to have formed a binary neutron star in a tight orbit. Compact neutron star binary systems are produced from binary massive stars through stellar evolution involving up to two supernova explosions. The final stages in the formation of these systems have not been directly observed. We report the discovery of iPTF 14gqr (SN 2014ft), a type Ic supernova with a fast-evolving light curve indicating an extremely low ejecta mass (≈0.2 solar masses) and low kinetic energy (≈2 × 1050 ergs). Early photometry and spectroscopy reveal evidence of shock cooling of an extended helium-rich envelope, likely ejected in an intense pre-explosion mass-loss episode of the progenitor. Taken together, we interpret iPTF 14gqr as evidence for ultra-stripped supernovae that form neutron stars in compact binary systems.