Neutrino and pair creation in reconnection-powered coronae of accreting black holes
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2024
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| author | Karavola, D. Petropoulou, M. Fiorillo, D. F. G. Comisso, L. Sironi, L. |
| author_facet | Karavola, D. Petropoulou, M. Fiorillo, D. F. G. Comisso, L. Sironi, L. |
| contents | A ubiquitous feature of accreting black hole systems is their hard X-ray emission which is thought to be produced through Comptonization of soft photons by electrons and positrons in the vicinity of the black hole, in a region with optical depth of order unity. The origin and composition of this Comptonizing region, known as the corona, is a matter open for debate. In this paper we investigate the role of relativistic protons accelerated in black-hole magnetospheric current sheets for the pair enrichment and neutrino emission of AGN coronae. Our model has two free parameters, namely the proton plasma magnetization $σ_{\rm p}$, which controls the peak energy of the neutrino spectrum, and the Eddington ratio $λ_{\rm X, Edd}$ (defined as the ratio between X-ray luminosity $L_{\rm X}$ and Eddington luminosity $L_{\rm Edd}$), which controls the amount of energy transferred to secondary particles. For sources with $λ_{\rm X, Edd} \gtrsim λ_{\rm Edd, crit}$ (where $λ_{\rm Edd, crit} \sim 10^{-1}$ for $σ_{\rm p}=10^5$ or $\sim 10^{-2}$ for $σ_{\rm p}=10^7$), proton-photon interactions and $ γγ$ annihilation produce enough secondary pairs to achieve Thomson optical depths $τ_{\rm T} \sim 0.1-10$. In the opposite case of $λ_{\rm X, Edd} \lesssim λ_{\rm Edd, crit}$, the coronal pairs cannot originate only from hadronic interactions. Additionally, we find that the neutrino luminosity scales as $L^2_{\rm X}/L_{\rm Edd}$ for $λ_{\rm X, Edd} \lesssim λ_{\rm Edd, crit}$, while it is proportional to $L_{\rm X}$ for higher $λ_{\rm X, Edd}$ values. We apply our model to four Seyfert galaxies, including NGC 1068, and discuss our results in light of recent IceCube observations. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2410_12638 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Neutrino and pair creation in reconnection-powered coronae of accreting black holes Karavola, D. Petropoulou, M. Fiorillo, D. F. G. Comisso, L. Sironi, L. High Energy Astrophysical Phenomena A ubiquitous feature of accreting black hole systems is their hard X-ray emission which is thought to be produced through Comptonization of soft photons by electrons and positrons in the vicinity of the black hole, in a region with optical depth of order unity. The origin and composition of this Comptonizing region, known as the corona, is a matter open for debate. In this paper we investigate the role of relativistic protons accelerated in black-hole magnetospheric current sheets for the pair enrichment and neutrino emission of AGN coronae. Our model has two free parameters, namely the proton plasma magnetization $σ_{\rm p}$, which controls the peak energy of the neutrino spectrum, and the Eddington ratio $λ_{\rm X, Edd}$ (defined as the ratio between X-ray luminosity $L_{\rm X}$ and Eddington luminosity $L_{\rm Edd}$), which controls the amount of energy transferred to secondary particles. For sources with $λ_{\rm X, Edd} \gtrsim λ_{\rm Edd, crit}$ (where $λ_{\rm Edd, crit} \sim 10^{-1}$ for $σ_{\rm p}=10^5$ or $\sim 10^{-2}$ for $σ_{\rm p}=10^7$), proton-photon interactions and $ γγ$ annihilation produce enough secondary pairs to achieve Thomson optical depths $τ_{\rm T} \sim 0.1-10$. In the opposite case of $λ_{\rm X, Edd} \lesssim λ_{\rm Edd, crit}$, the coronal pairs cannot originate only from hadronic interactions. Additionally, we find that the neutrino luminosity scales as $L^2_{\rm X}/L_{\rm Edd}$ for $λ_{\rm X, Edd} \lesssim λ_{\rm Edd, crit}$, while it is proportional to $L_{\rm X}$ for higher $λ_{\rm X, Edd}$ values. We apply our model to four Seyfert galaxies, including NGC 1068, and discuss our results in light of recent IceCube observations. |
| title | Neutrino and pair creation in reconnection-powered coronae of accreting black holes |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2410.12638 |