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Neutrino pair annihilation near accreting, stellar-mass black holes

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Neutrino pair annihilation near accreting, stellar-mass black holes

dc.contributor.author	Birkl, R.
dc.contributor.author	Aloy Toras, Miguel Angel
dc.contributor.author	Janka, H.-Th
dc.contributor.author	Müller, E.
dc.date.accessioned	2010-08-10T10:55:56Z
dc.date.available	2010-08-10T10:55:56Z
dc.date.issued	2007
dc.identifier.citation	BIRKL, R. ; Aloy Toras, Miguel Angel ; Janka, H.-Th ; Müller, E. , 2007, Neutrino pair annihilation near accreting, stellar-mass black holes, Astronomy and Astrophysics, vol. 463, no. 1, p. 51-67	en
dc.identifier.uri	http://hdl.handle.net/10550/16813
dc.description.abstract	Context. We investigate the deposition of energy and momentum due to the annihilation of neutrinos (ν) and antineutrinos (¯ν) in the vicinity of steady, axisymmetric accretion tori around stellar-mass black holes (BHs). This process is widely considered as an energy source for driving ultrarelativistic outflows with the potential to produce gamma-ray bursts. Aims. We analyze the influence of general relativistic (GR) effects in combination with different neutrinosphere properties on the ν¯ν-annihilation efficiency and spatial distribution of the energy deposition rate. Methods. Assuming axial symmetry, we numerically compute the annihilation rate 4-vector. For this purpose, we construct the local neutrino distribution by ray-tracing neutrino trajectories in a Kerr space-time using null geodesics. We vary the value of the dimensionless specific angular momentum a of the central BH, which provides the gravitational field in our models. We also study different shapes of the neutrinospheres, spheres, thin disks, and thick accretion tori, whose structure ranges from idealized tori to equilibrium non-selfgravitating matter distributions. Furthermore, we compute Newtonian models where the influence of the gravitational field on the annihilation process is neglected. Results. Compared to Newtonian calculations, GR effects increase the total annihilation rate measured by an observer at infinity by a factor of two when the neutrinosphere is a thin disk, but the increase is only ≈25% for toroidal and spherical neutrinospheres. Comparing cases with similar luminosities, thin disk models yield the highest energy deposition rates by ν¯ν-annihilation, and spherical neutrinospheres the lowest ones, independently of whether GR effects are included. Increasing a from 0 to 1 enhances the energy deposition rate measured by an observer at infinity by roughly a factor of 2 due to the change of the inner radius of the neutrinosphere. General relativity and rotation cause important differences in the spatial distribution of the energy deposition rate by ν¯ν-annihilation.	en
dc.language.iso	en	en
dc.subject	Gamma rays ; Bursts ; Neutrinos ; Accretion ; Accretion disks ; Relativity ; Black hole physics ; Neutron	en
dc.title	Neutrino pair annihilation near accreting, stellar-mass black holes	en
dc.type	journal article	es_ES
dc.subject.unesco	UNESCO::ASTRONOMÍA Y ASTROFÍSICA	en
dc.subject.unesco	UNESCO::ASTRONOMÍA Y ASTROFÍSICA::Cosmología y cosmogonia	en
dc.identifier.doi	10.1051/0004-6361:20066293	en
dc.identifier.idgrec	035922	en
dc.type.hasVersion	VoR	es_ES
dc.identifier.url	http://www.aanda.org/articles/aa/pdf/2007/07/aa6293-06.pdf	en