Richardson Noel D, Pavao Clarissa M, Eldridge Jan J, Pablo Herbert, Chené André-Nicolas, Wysocki Peter, Gies Douglas R, Younes George, Hare Jeremy
Department of Physics and Astronomy, Embry-Riddle Aeronautical University, Prescott, AZ, USA.
Department of Physics, University of Auckland, Auckland, New Zealand.
Nature. 2023 Feb;614(7946):45-47. doi: 10.1038/s41586-022-05618-9. Epub 2023 Feb 1.
Ultra-stripped supernovae are different from other terminal explosions of massive stars, as they show little or no ejecta from the actual supernova event. They are thought to occur in massive binary systems after the exploding star has lost its surface through interactions with its companion. Such supernovae produce little to no kick, leading to the formation of a neutron star without loss of the binary companion, which itself may also evolve into another neutron star. Here we show that a recently discovered high-mass X-ray binary, CPD -29 2176 (CD -29 5159; SGR 0755-2933), has an evolutionary history that shows the neutron star component formed during an ultra-stripped supernova. The binary has orbital elements that are similar both in period and in eccentricity to 1 of 14 Be X-ray binaries that have known orbital periods and eccentricities. The identification of the progenitors systems for ultra-stripped supernovae is necessary as their evolution pathways lead to the formation of binary neutron star systems. Binary neutron stars, such as the system that produced the kilonova GW170817 that was observed with both electromagnetic and gravitational energy, are known to produce a large quantity of heavy elements.
超剥离超新星不同于大质量恒星的其他末期爆炸，因为它们在实际超新星事件中显示出很少或几乎没有抛射物。它们被认为发生在大质量双星系统中，即爆炸恒星通过与伴星的相互作用失去其表面之后。此类超新星产生的反冲力很小或几乎没有，导致形成一颗中子星而不会失去双星伴星，而这颗伴星本身也可能演变成另一颗中子星。在此我们表明，最近发现的一个高质量X射线双星CPD -29 2176（CD -29 5159；SGR 0755-2933）具有的演化历史表明，其中子星成分是在一次超剥离超新星爆发期间形成的。该双星的轨道要素在周期和偏心率方面与14个已知轨道周期和偏心率的Be X射线双星中的1个相似。确定超剥离超新星的前身系统很有必要，因为它们的演化路径会导致双星中子星系统的形成。已知双星中子星，比如产生了电磁能和引力能均被观测到的千新星GW170817的系统，会产生大量重元素。
