A hadronic emission model for black hole-disc impacts in the blazar OJ 287. Issue 4 (4th September 2020)

• Record Type: Journal Article
• Authors: Rodríguez-Ramírez, J C; Kushwaha, P; de Gouveia Dal Pino, E M; Santos-Lima, R
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 498:Issue 4(2020)
• Page Start: 5424
• Page End: 5436
• Publication Date: 2020-09-04
• Subjects: astroparticle physics -- radiation mechanisms: non-thermal -- shock waves -- BL Lacertae objects: individual; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/staa2664
• Languages: English
• ISSNs: 0035-8711

Abstract

ABSTRACT: A supermassive black hole (SMBH) binary in the core of the blazar OJ 287 has been invoked in previous works to explain its observed optical flare quasi-periodicity. Following this picture, we investigate a hadronic origin for the X-ray and γ -ray counterparts of the November 2015 major optical flare of this source. An impact outflow must result after the lighter SMBH (the secondary) crosses the accretion disc of the heavier one (the primary). We then consider acceleration of cosmic ray (CR) protons in the shock driven by the impact outflow as it expands and collides with the active galactic nucleus (AGN) wind of the primary SMBH. We show that the emission of these CRs can reproduce the X-ray and γ -ray flare data self-consistently with the optical component of the 2015 November major flare. The derived emission models are consistent with a magnetic field B ∼ 5 G in the emission region and a power-law index of q ∼ 2.2 for the energy distribution of the emitting CRs. The mechanical luminosity of the AGN wind represents $\lesssim 50{{\ \rm per\ cent}}$ of the mass accretion power of the primary SMBH in all the derived emission profiles.