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(Reference retrieved automatically from Web of Science through information on FAPESP grant and its corresponding number as mentioned in the publication by the authors.)

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

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Khiali, B. [1] ; de Gouveia Dal Pino, E. M. [1] ; del Valle, M. V. [2]
Total Authors: 3
[1] Univ Sao Paulo, IAG, Sao Paulo, SP - Brazil
[2] CCT La Plata, IAR, Buenos Aires, DF - Argentina
Total Affiliations: 2
Document type: Journal article
Source: Monthly Notices of the Royal Astronomical Society; v. 449, n. 1, p. 34-48, MAY 1 2015.
Web of Science Citations: 14

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)

FAPESP's process: 06/50654-3 - Investigation of high energy and plasma astrophysics phenomena: theory, observation, and numerical simulations
Grantee:Elisabete Maria de Gouveia Dal Pino
Support type: Research Projects - Thematic Grants