DDp.2.49 — Possible mechanism for radio and gamma-ray emissions in accreting black hole sources

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Aug 10th at 6:00 PM until 6:00 PM

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Author(s): Chandra Bahadur Singh1, Elisabete de Gouveia Dal Pino1, Luis Henrique Sinki Kadowaki1

Institution(s): 1. IAG-USP

We attempt to explain the observed radio and gamma-ray emission produced in the
surrounds of black holes by employing a magnetically-dominated accretion flow (MDAF) model
and fast magnetic reconnection triggered by turbulence. In earlier work, standard disk model was
used and we refine the model by focusing on the sub-Eddington regime to address the
fundamental plane of black hole activity. The results do not change substantially with regard to
previous work ensuring that the details of the accretion physics are not relevant in the magnetic
reconnection process occurring in the corona. Rather our work puts fast magnetic reconnection
events as a powerful mechanism operating in the core region, near the jet base of black hole
sources on more solid ground. For microquasars and low-luminosity active galactic nuclei
(LLAGNs) the observed correlation between radio emission and mass of the sources can be
explained by this process. The corresponding gamma-ray emission also seems to be produced in
the same core region. On the other hand, the emission from blazars and gamma-ray bursts
(GRBs) cannot be correlated to core emission based on fast reconnection.