标题： 超新星D6幸存者的光谱和运动学分析 显示英文标题

标题： Spectroscopic and kinematic analyses of a warm survivor of a D6 supernova

摘要： SDSSJ163712.21+363155.9 是一颗候选超高速星，最初通过斯隆数字巡天中其异常光谱被识别出来，该光谱显示氧、镁和硅线红移了数千$100\,$公斤/秒，这导致推测它是由热核超新星抛射出去的。 我们获得了 SDSSJ1637+3631 的 GTC OSIRIS 光谱，确定了一个温暖（$T_\mathrm{eff}=15680\pm250\,$开尔文）以碳和氧为主的气氛，并且富含硅、硫和钙等中间质量元素。 我们认为 SDSSJ1637+3631 是一颗吸积白矮星的供体，在动力驱动的双简并双爆轰（D6）Ia 型超新星中爆炸，目前的成分与由沉积的超新星喷出物富集的 CO 白矮星核心一致。 尽管 SDSSJ1637+3631 的盖亚视差精度较低，但我们的光谱表面重力（$\log g=6.3\pm0.3\,$德西贝尔）有助于将其切向速度限制在$1950^{+810}_{-530}\,$公斤/秒，这为 D6 机制提供了额外的支持。 假设 SDSSJ1637+3631 是一个 D6 幸存者，我们构建了一个结合所有天体测量、光谱和测光信息的动力学模型，同时也包括银河系的结构和引力势。 我们的模型将抛射位置定位在银河盘的内几千秒差距范围内（虽然排除了银河中心），抛射速度为$1870^{+360}_{-300}\,$公斤/秒，飞行时间为$4.5^{+0.4}_{-0.5}\,$百万年。 显示英文摘要

摘要： SDSSJ163712.21+363155.9 is a candidate hyper-runaway star, first identified from its unusual spectrum in the Sloan Digital Sky Survey, which exhibits oxygen, magnesium, and silicon lines redshifted by several $100\,$km/s, leading to the suggestion it was ejected from a thermonuclear supernova. We have acquired GTC OSIRIS spectroscopy of SDSSJ1637+3631 establishing a warm ($T_\mathrm{eff}=15680\pm250\,$K) carbon+oxygen dominated atmosphere, that is also abundant in the intermediate mass elements silicon, sulphur, and calcium. We interpret SDSSJ1637+3631 as the donor to an accreting white dwarf that exploded in a dynamically-driven double-degenerate double-detonation (D6) type Ia supernova, where the current composition is consistent with a CO white dwarf core, enriched with intermediate mass elements from deposited supernova ejecta. While SDSSJ1637+3631 has a low-precision Gaia parallax, our spectroscopic surface gravity ($\log g=6.3\pm0.3\,$dex) helps constrain its tangential velocity to $1950^{+810}_{-530}\,$km/s, providing additional support to the D6 mechanism. Under the assumption that SDSSJ1637+3631 is a D6 survivor, we construct a kinematic model combining all astrometric, spectroscopic, and photometric information, but also including the structure and gravitational potential of the Milky Way. Our model localises the ejection site to the inner few kpc of the Galactic disc (though excluding the Galactic centre), with an ejection speed of $1870^{+360}_{-300}\,$km/s, and a $4.5^{+0.4}_{-0.5}\,$Myr time of flight.