一颗D6超新星温暖幸存者的光谱与运动学分析
Spectroscopic and kinematic analyses of a warm survivor of a D6 supernova
AI总结：
研究结合GTC OSIRIS光谱与银河系运动学模型，确认SDSSJ1637+3631为富含中等质量元素的D6 Ia型超新星幸存供体星，并约束其抛射源、速度与飞行时间。
摘要：
SDSSJ163712.21+363155.9是一颗候选超高速逃逸星，最初因其在Sloan Digital Sky Survey中不同寻常的光谱而被识别；其光谱显示氧、镁和硅谱线红移达数百km/s，因此有人提出它是在一次热核超新星中被抛射出来的。我们获得了SDSSJ1637+3631的GTC OSIRIS光谱，确认其具有温暖（T_eff=15680±250 K）的碳+氧主导大气，并且富含硅、硫和钙等中等质量元素。我们将SDSSJ1637+3631解释为一颗正在吸积的白矮星的供体星，该白矮星在一次动力学驱动的双简并双爆轰（D6）Ia型超新星中爆炸；其当前成分与因沉积的超新星抛射物而富集中等质量元素的CO白矮星核心相符。尽管SDSSJ1637+3631的Gaia视差精度较低，但我们由光谱得到的表面重力（log g=6.3±0.3 dex）有助于将其切向速度约束为1950^{+810}_{-530} km/s，从而为D6机制提供额外支持。在假设SDSSJ1637+3631是D6幸存者的前提下，我们构建了一个结合所有天体测量、光谱和光度信息，同时纳入银河系结构与引力势的运动学模型。该模型将抛射位置定位于银盘内部数kpc范围内（但排除银心），抛射速度为1870^{+360}_{-300} km/s，飞行时间为4.5^{+0.4}_{-0.5} Myr。
英文摘要：
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.
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