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Numerical models of VHE emission by magnetic reconnection in X-ray binaries: GRMHD simulations and Monte Carlo cosmic-ray emission

Published online by Cambridge University Press:  30 December 2019

J. C. Rodríguez-Ramírez ,
E. M. de Gouveia Dal Pino  and
R. Alves Batista
J. C. Rodríguez-Ramírez
Affiliation:
Instituto de Astronomia, Geofísica e Ciências Atmosféricas (IAG-USP), Universidade de São Paulo. Cidade Universitaria R. do Matão, 1226 05508-090 São Paulo, SP Brasil email: juan.rodriguez@iag.usp.br
R. Alves Batista
Affiliation:
Instituto de Astronomia, Geofísica e Ciências Atmosféricas (IAG-USP), Universidade de São Paulo. Cidade Universitaria R. do Matão, 1226 05508-090 São Paulo, SP Brasil email: juan.rodriguez@iag.usp.br
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Abstract

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Galactic microquasars have been detected at very-high-energies (VHE) (> 100 GeV) and the particle acceleration mechanisms that produce this emission are not yet well-understood. Here we investigate a hadronic emission scenario where cosmic-rays (CRs) are accelerated in magnetic reconnection events by the turbulent, advected-dominated accretion flow (ADAF) believed to be present in the hard state of black hole binaries. We present Monte Carlo simulations of CR emission plus γ-γ and inverse Compton cascades, injecting CRs with a total energy consistent with the magnetic energy of the plasma. The background gas density, magnetic, and photon fields where CRs propagate and interact are modelled with general relativistic (GR), magneto-hydrodynamical simulations together with GR radiative transfer calculations. Our approach is applied to the microquasar Cygnus X-1, where we show a model configuration consistent with the VHE upper limits provided by MAGIC collaboration.

Keywords

radiation mechanisms: non-thermalX-rays: binariesmagnetohydrodynamicsaccretion disks
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S346: High-mass X-ray Binaries: Illuminating the Passage from Massive Binaries to Merging Compact Objects , August 2018 , pp. 388 - 393
Copyright
© International Astronomical Union 2019 

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