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Nuclear gamma-ray emission from very hot accretion flows

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Kafexhiu,  Ervin
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

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Aharonian,  F.
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

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Citation

Kafexhiu, E., Aharonian, F., & Barkov, M. (2019). Nuclear gamma-ray emission from very hot accretion flows. Astronomy and Astrophysics, 623: A174. doi:10.1051/0004-6361/201833948.


Cite as: http://hdl.handle.net/21.11116/0000-0005-4C54-8
Abstract
Optically thin accretion plasmas can reach ion temperatures T-i >= 10(10) K and thus trigger nuclear reactions. Using a large nuclear interactions network, we studied the radial evolution of the chemical composition of the accretion flow toward the black hole and computed the emissivity in nuclear gamma-ray lines. In the advection dominated accretion flow (ADAF) regime, CNO and heavier nuclei are destroyed before reaching the last stable orbit. The overall luminosity in the de-excitation lines for a solar composition of plasma can be as high as few times 10(-5) the accretion luminosity ((M) over dotc(2)) and can be increased for heavier compositions up to 10(-3). The e ffi ciency of transformation of the kinetic energy of the outflow into high energy (>= 100 MeV) gamma-rays through the production and decay of pi(0)-mesons can be higher, up to 10 2 of the accretion luminosity. We show that in the ADAF model up to 15% of the mass of accretion matter can "evaporate" in the form of neutrons.