论文标题
Asassn-16OH：没有大量弹射的Nova爆发 - 一种新型的Supersoft X射线源
ASASSN-16oh: A nova outburst with no mass ejection -- A new type of supersoft X-ray source in old populations
论文作者
论文摘要
Asassn-16OH是一个特殊的瞬态超级X射线源，在小麦哲伦云的领域中没有质量驱除签名。 Maccarone等。 （2019年）得出的结论是，Asassn-16OH是第一个具有SuperSoft X射线的矮人Nova，源自白矮人（WD）上的赤道增生带。 Hillman等。 （2019年）提出了一种热核失控模型，即X射线和$ v $/$ i $ $ $ $ $ $ $ $ $ $。我们计算了与Hillman等人相同的参数模型，发现它们在大规模上进行操纵，并且其最佳拟合$ V $ Light Curves是6磁磁带，并且比Asassn-16OH慢了10倍。我们提出了一个矮小新星爆发期间高质量积聚速率引起的NOVA模型，即，X射线源自燃气WD的表面，而$ V/I $ $光子来自辐照盘。我们的模型解释了Asassn-16OH的主要观察性能。我们还获得了热核失控模型，没有质量弹射的WD质量和质量积聚率的广泛参数，包括$ z = 0.001 $和$ z = 0.0001 $的自然和强迫Novae。它们是一种新型的定期超级X射线源，没有大量弹射，也是$ V $/$ i $ $ bands的明亮瞬态，如果它们有大磁盘。我们建议这样的物体是IA型超新星祖细胞的候选者，因为其质量以很高的效率$（\ sim 100 \％）$增加。
ASASSN-16oh is a peculiar transient supersoft X-ray source without a mass-ejection signature in the field of the Small Magellanic Cloud. Maccarone et al. (2019) concluded that ASASSN-16oh is the first dwarf nova with supersoft X-ray that originated from an equatorial accretion belt on a white dwarf (WD). Hillman et al. (2019) proposed a thermonuclear runaway model that both the X-rays and $V$/$I$ photons are emitted from the hot WD. We calculated the same parameter models as Hillman et al.'s and found that they manipulated on/off the mass-accretion, and their best fit $V$ light curves are 6 mag fainter, and decay about 10 times slower, than that of ASASSN-16oh. We propose a nova model induced by a high rate of mass accretion during a dwarf nova outburst, i.e., the X-rays originate from the surface of the hydrogen-burning WD whereas the $V/I$ photons are from the irradiated disk. Our model explains the main observational properties of ASASSN-16oh. We also obtained thermonuclear runaway models with no mass ejection for a wide range of parameters of the WD mass and mass accretion rates including both natural and forced novae in low-metal environments of $Z=0.001$ and $Z=0.0001$. They are a new type of periodic supersoft X-ray sources with no mass ejection, and also a bright transient in $V$/$I$ bands if they have a large disk. We suggest that such objects are candidates of Type Ia supernova progenitors because its mass is increasing at a very high efficiency $(\sim 100 \%)$.
