恒星自转作为检验银心广义相对论的新观测量
Stellar rotation as a new observable to test general relativity in the Galactic Center
摘要：
银河系中心的S星是各种广义相对论效应的极好试验台。虽然以前的工作集中在模拟它们围绕Sgr A*（银河系中心的超大质量黑洞）的轨道运动，但在这里，我们探索了使用S星旋转来测试广义相对论预测的德西特进动的可能性。我们发现，通过重新定向的旋转轴的S-星，德西特岁差将改变在恒星光谱中的吸收线的表观宽度。我们的数值模拟表明，新发现的S4714和S62是最适合这样的测试，因为它们的近心距离相对于Sgr A* 小。根据恒星的初始倾角，在$20-40$年的周期内，谱线宽度的变化量将达到$20-76\,{\rm km\,s^{-1}}$。这种变化与当前的检测限相当。由于岁差率对轨道偏心率和恒星四极结构敏感，因此监测S星的旋转也可以帮助我们更好地约束S星的轨道根数及其内部结构。
英文摘要：
S-stars in the Galactic Center are excellent testbeds of various general relativistic effects. While previous works focus on modeling their orbital motion around Sgr A*--the supermassive black hole in the Galactic Center--here we explore the possibility of using the rotation of S-stars to test the de Sitter precession predicted by general relativity. We show that by reorienting the rotation axes of S-stars, de Sitter precession will change the apparent width of the absorption lines in the stellar spectra. Our numerical simulations suggest that the newly discovered S4714 and S62 are best suited for such a test because of their small pericenter distances relative to Sgr A*. Depending on the initial inclination of the star, the line width would vary by as much as $20-76\,{\rm km\,s^{-1}}$ within a period of $20-40$ years. Such a variation is comparable to the current detection limit. Since the precession rate is sensitive to the orbital eccentricity and stellar quadrupole structure, monitoring the rotation of S-stars could also help us better constrain the orbital elements of the S-stars and their internal structures.
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