论文标题
恒星旋转作为可观察到银河系中心一般相对性的新的新型旋转
Stellar rotation as a new observable to test general relativity in the Galactic Center
论文作者
论文摘要
银河中心的S-Star是具有各种一般相对论效应的出色测试床。虽然先前的作品着重于建模其围绕SGR A*的轨道运动 - 银河中心中的超质量黑洞 - 但我们探索了使用S-Stars旋转来测试通过一般相对性预测的Sitter Prepession的可能性。我们表明，通过重新定位S-Star的旋转轴，De Sitter进动将改变恒星光谱中吸收线的明显宽度。我们的数值模拟表明，新发现的S4714和S62最适合于这种测试，因为它们相对于SGR A*的小吃者距离很小。根据恒星的初始倾向，线宽度在$ 20-40 $ $年内的范围将差异高达$ 20-76 \，{\ rm km \，s^{ - 1}} $。这种变化与当前的检测极限相当。由于进动率对轨道偏心率和出色的四极结构敏感，因此监测S-Star的旋转也可以帮助我们更好地限制S-Stars及其内部结构的轨道元素。
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.
