Rates of Stellar Tidal Disruption

Autor: Hagai B. Perets, Elena M. Rossi, Michael Kesden, Nicholas Stone, Eugene Vasiliev, Pau Amaro-Seoane
Přispěvatelé: European Space Agency, Ministerio de Economía, Industria y Competitividad (España), National Natural Science Foundation of China
Rok vydání: 2020
Předmět:
010504 meteorology & atmospheric sciences
Astrophysics::High Energy Astrophysical Phenomena
FOS: Physical sciences
General Relativity and Quantum Cosmology (gr-qc)
Astrophysics::Cosmology and Extragalactic Astrophysics
Galactic nuclei
01 natural sciences
General Relativity and Quantum Cosmology
Tidal disruption event
0103 physical sciences
Astrophysics::Solar and Stellar Astrophysics
010303 astronomy & astrophysics
Astrophysics::Galaxy Astrophysics
0105 earth and related environmental sciences
High Energy Astrophysical Phenomena (astro-ph.HE)
Supermassive black hole
Astronomy
Astronomy and Astrophysics
Astrophysics - Astrophysics of Galaxies
Galaxy
Stars
Planetary science
Space and Planetary Science
Astrophysics of Galaxies (astro-ph.GA)
Physics::Accelerator Physics
Astrophysics::Earth and Planetary Astrophysics
Astrophysics - High Energy Astrophysical Phenomena
Geology
Zdroj: Space Science Reviews, 216(3), 35
Digital.CSIC. Repositorio Institucional del CSIC
instname
ISSN: 1572-9672
0038-6308
Popis: arXiv:2003.08953v1
Tidal disruption events occur rarely in any individual galaxy. Over the last decade, however, time-domain surveys have begun to accumulate statistical samples of these flares. What dynamical processes are responsible for feeding stars to supermassive black holes? At what rate are stars tidally disrupted in realistic galactic nuclei? What may we learn about supermassive black holes and broader astrophysical questions by estimating tidal disruption event rates from observational samples of flares? These are the questions we aim to address in this Chapter, which summarizes current theoretical knowledge about rates of stellar tidal disruption, and compares theoretical predictions to the current state of observations.
N.C.S. received financial support from the NASA Astrophysics Theory Research Program (Grant NNX17AK43G; PI B. Metzger). M. K. acknowledges support from NSF Grant No. PHY-1607031 and NASA Award No. 80NSSC18K0639. E.M.R. acknowledges support from NWO TOP grant Module 2, project number 614.001.401. P.A.S. acknowledges support from the Ramón y Cajal Programme of the Ministry of Economy, Industry and Competitiveness of Spain, the COST Action GWverse CA16104, and the National Key R&D Program of China (2016YFA0400702) and the National Science Foundation of China (11721303).
Databáze: OpenAIRE
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