A magnetic reconnection model for explaining the multiwavelength emission of the microquasars Cyg X-1 and Cyg X-3

Autor(es)

Khiali, B. ^[1] ; de Gouveia Dal Pino, E. M. ^[1] ; del Valle, M. V. ^[2]

Afiliação do(s) autor(es)

^[1] Univ Sao Paulo, IAG, Sao Paulo, SP - Brazil

^[2] CCT La Plata, IAR, Buenos Aires, DF - Argentina

• Tipo de documento: Artigo Científico
• Fonte: Monthly Notices of the Royal Astronomical Society; v. 449, n. 1, p. 34-48, MAY 1 2015.
• Citações Web of Science: 14

Resumo

Recent studies have indicated that cosmic ray acceleration by a first-order Fermi process in magnetic reconnection current sheets can be efficient enough in the surrounds of compact sources. In this work, we discuss this acceleration mechanism operating in the core region of galactic black hole binaries (or microquasars) and show the conditions under which this can be more efficient than shock acceleration. In addition, we compare the corresponding acceleration rate with the relevant radiative loss rates obtaining the possible energy cut-off of the accelerated particles and also compute the expected spectral energy distribution (SED) for two sources of this class, namely Cygnus X-1 and Cygnus X-3, considering both leptonic and hadronic processes. The derived SEDs are comparable to the observed ones in the low-and high-energy ranges. Our results suggest that hadronic non-thermal emission due to photomeson production may produce the very high energy gamma-rays in these microquasars. (AU)

• Processo FAPESP: 06/50654-3 - Investigação de fenômenos de altas energias e plasmas astrofísicos: teoria, observação e simulações numéricas
• Beneficiário: Elisabete Maria de Gouveia Dal Pino
• Modalidade de apoio: Auxílio à Pesquisa - Temático