TeV Neutrinos and Hard X-Rays from Relativistic Reconnection in the Corona of NGC 1068

被引：20

作者：

Fiorillo, Damiano F. G. ^{[1
]}

Petropoulou, Maria ^{[2
,3
]}

Comisso, Luca ^{[4
]}

Peretti, Enrico ^{[1
,5
]}

Sironi, Lorenzo ^{[4
,6
]}

机构：

[1] Univ Copenhagen, Niels Bohr Inst, Niels Bohr Int Acad, DK-2100 Copenhagen, Denmark

[2] Univ Campus Zografos, Natl & Kapodistrian Univ Athens, Dept Phys, GR-15784 Athens, Greece

[3] Univ Campus Zografos, Inst Accelerating Syst & Applicat, Athens, Greece

[4] Columbia Univ, Dept Astron, Columbia Astrophys Lab, New York, NY 10027 USA

[5] Univ Paris Cite, CNRS, Astroparticule & Cosmol, 10 Rue Alice Domon & Leonie Duquet, F-75013 Paris, France

[6] Flatiron Inst, Ctr Computat Astrophys, 162 5th Ave, New York, NY 10010 USA

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2024年 / 961卷 / 01期

关键词：

ACTIVE GALACTIC NUCLEI; HIGH-ENERGY NEUTRINOS; NONTHERMAL PARTICLE-ACCELERATION; RADIATIVE MAGNETIC RECONNECTION; GAMMA-RAY; EMISSION; COMPTONIZATION; FLARES; SPECTRA; SIMULATIONS;

D O I：

10.3847/2041-8213/ad192b

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The recent discovery of astrophysical neutrinos from the Seyfert galaxy NGC 1068 suggests the presence of nonthermal protons within a compact "coronal" region close to the central black hole. The acceleration mechanism of these nonthermal protons remains elusive. We show that a large-scale magnetic reconnection layer, of the order of a few gravitational radii, may provide such a mechanism. In such a scenario, rough energy equipartition between magnetic fields, X-ray photons, and nonthermal protons is established in the reconnection region. Motivated by recent 3D particle-in-cell simulations of relativistic reconnection, we assume that the spectrum of accelerated protons is a broken power law, with the break energy being constrained by energy conservation (i.e., the energy density of accelerated protons is at most comparable to the magnetic energy density). The proton spectrum is dnp/dEp proportional to Ep-1 below the break and dnp/dEp proportional to Ep-s above the break, with IceCube neutrino observations suggesting s similar or equal to 3. Protons above the break lose most of their energy within the reconnection layer via photohadronic collisions with the coronal X-rays, producing a neutrino signal in good agreement with the recent observations. Gamma rays injected in photohadronic collisions are cascaded to lower energies, sustaining the population of electron-positron pairs that makes the corona moderately Compton thick.

引用

页数：13

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