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000617689 0247_ $$2arXiv$$aarXiv:2307.07338
000617689 0247_ $$2datacite_doi$$a10.3204/PUBDB-2024-06980
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000617689 088__ $$2arXiv$$aarXiv:2307.07338
000617689 1001_ $$0P:(DE-HGF)0$$aRyu, Taeho$$b0$$eCorresponding author
000617689 245__ $$aCollisions of red giants in galactic nuclei
000617689 260__ $$aOxford$$bOxford Univ. Press$$c2024
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000617689 500__ $$a16 pages, 14 figures, 2 tables, accepted for publication in MNRAS, comments welcome, movies here: https://www.youtube.com/playlist?list=PLxLK3qI02cQd9lyIo6DIqm1tQnx_-G3Ut
000617689 520__ $$aIn stellar-dense environments, stars can collide with each other. For collisions close to a supermassive black hole (SMBH), the collisional kinetic energy can be so large that the colliding stars can be destroyed, potentially releasing an amount of energy comparable to that of a supernova. These black hole-driven disruptive collisions have been examined mostly analytically, with the non-linear hydrodynamical effects being left largely unstudied. Using the moving-mesh hydrodynamics code arepo, we investigate high-velocity (>10^3 km s^−1) collisions between 1 M_⊙ giants with varying radii, impact parameters, and initial approaching velocities, and estimate their observables. Very strong shocks across the collision surface efficiently convert |${\gtrsim} 10~{{\ \rm per\ cent}}$| of the initial kinetic energy into radiation energy. The outcome is a gas cloud expanding supersonically, homologously, and quasi-spherically, generating a flare with a peak luminosity ≃10^41–10^44 erg s^−1 in the extreme ultraviolet band (≃10 eV). The luminosity decreases approximately following a power law of t^−0.7 initially, then t^−0.4 after t ≃ 10 d at which point it would be bright in the optical band (≲1eV). Subsequent, and possibly even brighter, emission would be generated due to the accretion of the gas cloud on to the nearby SMBH, possibly lasting up to multiyear time-scales. This inevitable BH–collision product interaction can contribute to the growth of BHs at all mass scales, in particular, seed BHs at high redshifts. Furthermore, the proximity of the events to the central BH makes them a potential tool for probing the existence of dormant BHs, even very massive ones which cannot be probed by tidal disruption events.
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000617689 650_7 $$2autogen$$ahydrodynamics
000617689 650_7 $$2autogen$$astars: kinematics and dynamics
000617689 650_7 $$2autogen$$aGalaxy: nucleus
000617689 650_7 $$2autogen$$aquasars: supermassive black holes
000617689 650_7 $$2autogen$$aTransients
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000617689 7001_ $$aSeoane, Pau Amaro$$b1
000617689 7001_ $$0P:(DE-H253)PIP1080492$$aTaylor, Andrew$$b2
000617689 7001_ $$aOhlmann, Sebastian T.$$b3
000617689 77318 $$2Crossref$$3journal-article$$a10.1093/mnras/stae396$$bOxford University Press (OUP)$$d2024-02-07$$n4$$p6193-6209$$tMonthly Notices of the Royal Astronomical Society$$v528$$x0035-8711$$y2024
000617689 773__ $$0PERI:(DE-600)2016084-7$$a10.1093/mnras/stae396$$gVol. 528, no. 4, p. 6193 - 6209$$n4$$p6193-6209$$tMonthly notices of the Royal Astronomical Society$$v528$$x0035-8711$$y2024
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