ON THE ROLE OF FAST MAGNETIC RECONNECTION IN ACCRETING BLACK HOLE SOURCES

Autor(es)

Singh, C. B. ^[1] ; De Gouveia Dal Pino, E. M. ^[1] ; Kadowaki, L. H. S. ^[1]

Afiliação do(s) autor(es)

^[1] Univ Sao Paulo, Dept Astron IAG USP, Sao Paulo - Brazil

• Tipo de documento: Artigo Científico
• Fonte: Astrophysical Journal Letters; v. 799, n. 2 FEB 1 2015.
• Citações Web of Science: 18

Resumo

We attempt to explain the observed radio and gamma-ray emission produced in the surroundings of black holes by employing a magnetically dominated accretion flow model and fast magnetic reconnection triggered by turbulence. In earlier work, a 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 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, the observed correlation between radio emission and the 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, emission from blazars and gamma-ray bursts cannot be correlated to core emission based on fast reconnection. (AU)

• Processo FAPESP: 13/09065-8 - Origem e colimação de Jatos de Fontes Compactas e Mecanismos de Aceleração
• Beneficiário: Chandra Bahadur Singh
• Modalidade de apoio: Bolsas no Brasil - Pós-Doutorado
• Processo FAPESP: 11/51275-4 - Magnetic field effects and particle acceleration in gamma-ray bursts (GRBs): theory, numerical simulations, and observational prospects
• Beneficiário: Elisabete Maria de Gouveia Dal Pino
• Modalidade de apoio: Auxílio à Pesquisa - Regular