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- W2053670057 abstract "We study accretion processes for tidally disrupted stars approaching supermassive black holes on bound orbits, by performing three-dimensional smoothed particle hydrodynamics simulations with a pseudo-Newtonian potential. We find that there is a critical value of the orbital eccentricity below which all the stellar debris remains bound to the black hole. For high but subcritical eccentricities, all the stellar mass is accreted on to the black hole in a finite time, causing a significant deviation from the canonical t−5/3 mass fallback rate. When a star is on a moderately eccentric orbit and its pericentre distance is deeply inside the tidal disruption radius, there can be several orbit crossings of the debris streams due to relativistic precession. This dissipates orbital energy in shocks, allowing for rapid circularization of the debris streams and formation of an accretion disc. The resultant accretion rate greatly exceeds the Eddington rate and differs strongly from the canonical rate of t−5/3. By contrast, there is little dissipation due to orbital crossings for the equivalent simulation with a purely Newtonian potential. This shows that general relativistic precession is crucial for accretion disc formation via circularization of stellar debris from stars on moderately eccentric orbits." @default.
- W2053670057 created "2016-06-24" @default.
- W2053670057 creator A5019013125 @default.
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- W2053670057 date "2013-07-18" @default.
- W2053670057 modified "2023-10-15" @default.
- W2053670057 title "Finite, intense accretion bursts from tidal disruption of stars on bound orbits" @default.
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- W2053670057 doi "https://doi.org/10.1093/mnras/stt871" @default.
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