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@ARTICLE{Karavola:618942,
      author       = {Karavola, Despina and Petropoulou, M. and Fiorillo, Damiano
                      Francesco Giuseppe and Comisso, L. and Sironi, L.},
      title        = {{N}eutrino and pair creation in reconnection-powered
                      coronae of accreting black holes},
      reportid     = {PUBDB-2024-07253, arXiv:2410.12638},
      year         = {2024},
      note         = {DFGF is supported by the Alexander vonHumboldt Foundation
                      (Germany)},
      abstract     = {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 $\sigma_{\rm p}$, which controls the peak
                      energy of the neutrino spectrum, and the Eddington ratio
                      $\lambda_{\rm Edd}$ (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 $\lambda_{\rm Edd}
                      \gtrsim \lambda_{\rm Edd, crit}$ (where $\lambda_{\rm Edd,
                      crit} \sim 10^{-1}$ for $\sigma_{\rm p}=10^5$ or $\sim
                      10^{-2}$ for $\sigma_{\rm p}=10^7$), proton-photon
                      interactions and $ \gamma \gamma$ annihilation produce
                      enough secondary pairs to achieve Thomson optical depths
                      $\tau_{\rm T} \sim 0.1-10$. Additionally, we find that the
                      neutrino luminosity scales as $L^2_{\rm X}/L_{\rm Edd}$ for
                      $\lambda_{\rm Edd} \lesssim \lambda_{\rm Edd, crit}$, while
                      it is proportional to $L_{\rm X}$ for higher $\lambda_{\rm
                      Edd}$ values. We apply our model to four Seyfert galaxies,
                      including NGC 1068, and discuss our results in light of
                      recent IceCube observations.},
      cin          = {$Z_THAT$},
      cid          = {$I:(DE-H253)Z_THAT-20210408$},
      pnm          = {613 - Matter and Radiation from the Universe (POF4-613) /
                      INTERACTIONS - NBIA INTERACTIONS POSTDOCTORAL PROGRAMME
                      (847523)},
      pid          = {G:(DE-HGF)POF4-613 / G:(EU-Grant)847523},
      experiment   = {EXP:(DE-MLZ)NOSPEC-20140101},
      typ          = {PUB:(DE-HGF)25},
      eprint       = {2410.12638},
      howpublished = {arXiv:2410.12638},
      archivePrefix = {arXiv},
      SLACcitation = {$\%\%CITATION$ = $arXiv:2410.12638;\%\%$},
      url          = {https://bib-pubdb1.desy.de/record/618942},
}