Lense-Thirring precession after a supermassive black hole disrupts a star

• 成果类型: Article
• 署名作者: Pasham, Dheeraj R.; Zajacek, Michal; Nixon, C. J.; Coughlin, Eric R.; Sniegowska, Marzena; Janiuk, Agnieszka; Czerny, Bozena; Wevers, Thomas; Guolo, Muryel; Ajay, Yukta; Loewenstein, Michael
• 署名单位: Massachusetts Institute of Technology (MIT); Masaryk University; University of Leeds; Syracuse University; Tel Aviv University; Polish Academy of Sciences; Center for Theoretical Physics - Polish Academy of Sciences; Space Telescope Science Institute; European Southern Observatory; Johns Hopkins University; University System of Maryland; University of Maryland College Park; National Aeronautics & Space Administration (NASA); NASA Goddard Space Flight Center; National Aeronautics & Space Administration (NASA); NASA Goddard Space Flight Center
• 刊物名称: Nature
• ISSN/ISSBN: 0028-4837
• DOI: 10.1038/s41586-024-07433-w
• 发表日期: 2024-06-13
• 页码: 325-328
• 关键词: tidal disruption; binary-systems; accretion; simulations; variability; instability; disk; spectrum; flares; MODEL

摘要

An accretion disk formed around a supermassive black hole after it disrupts a star is expected to be initially misaligned with respect to the equatorial plane of the black hole. This misalignment induces relativistic torques (the Lense-Thirring effect) on the disk, causing the disk to precess at early times, whereas at late times the disk aligns with the black hole and precession terminates(1,2). Here we report, using high-cadence X-ray monitoring observations of a tidal disruption event (TDE), the discovery of strong, quasi-periodic X-ray flux and temperature modulations. These X-ray modulations are separated by roughly 15 days and persist for about 130 days during the early phase of the TDE. Lense-Thirring precession of the accretion flow can produce this X-ray variability, but other physical mechanisms, such as the radiation-pressure instability(3,4), cannot be ruled out. Assuming typical TDE parameters, that is, a solar-like star with the resulting disk extending at most to the so-called circularization radius, and that the disk precesses as a rigid body, we constrain the disrupting dimensionless spin parameter of the black hole to be 0.05 less than or similar to |a| less than or similar to 0.5.