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dc.contributor.authorBöttcher, M.
dc.contributor.authorReimer, A.
dc.contributor.authorSweeney, K.
dc.contributor.authorPrakash, A.
dc.date.accessioned2015-04-08T06:57:12Z
dc.date.available2015-04-08T06:57:12Z
dc.date.issued2013
dc.identifier.citationBöttcher, M. et al. 2013. Leptonic and hadronic modeling of Fermi-detected blazars. Astrophysical journal, 768: Article no 54. [https://doi.org/10.1088/0004-637X/768/1/54]en_US
dc.identifier.issn0004-637X
dc.identifier.issn1538-4357 (Online)
dc.identifier.urihttp://hdl.handle.net/10394/13661
dc.identifier.urihttps://doi.org/10.1088/0004-637X/768/1/54
dc.description.abstractWe describe new implementations of leptonic and hadronic models for the broadband emission from relativistic jets in active galactic nuclei in a temporary steady state. For the leptonic model, a temporary equilibrium between particle injection/acceleration, radiative cooling, and escape from a spherical emission region is evaluated, and the self-consistent radiative output is calculated. For the hadronic model, a temporary equilibrium between particle injection/acceleration, radiative and adiabatic cooling, and escape is evaluated for both primary electrons and protons. A new, semianalytical method to evaluate the radiative output from cascades initiated by internal γγ pair production is presented. We use our codes to fit snapshot spectral energy distributions (SEDs) of a representative set of Fermi-LAT-detected blazars. We find that the leptonic model provides acceptable fits to the SEDs of almost all blazars with parameters close to equipartition between the magnetic field and the relativistic electron population. However, the hard γ-ray spectrum of AO 0235+164, in contrast to the very steep IR–optical–UV continuum, poses a severe problem for the leptonic model. If charge neutrality in leptonic models is provided by cold protons, the kinetic energy carried by the jet should be dominated by protons. We find satisfactory representations of the snapshot SEDs of most blazars in our sample with the hadronic model presented here. However, in the case of two quasars the characteristic break at a few GeV energies cannot be well modeled. All of our hadronic model fits require powers in relativistic protons in the range Lp ~ 1047–1049 erg s−1.en_US
dc.language.isoenen_US
dc.publisherIOP Scienceen_US
dc.subjectGalaxies: activeen_US
dc.subjectgalaxies: jetsen_US
dc.subjectgamma rays: galaxiesen_US
dc.subjectradiation mechanisms: non-thermalen_US
dc.subjectrelativistic processesen_US
dc.titleLeptonic and hadronic modeling of Fermi-detected blazarsen_US
dc.typeArticleen_US
dc.contributor.researchID24420530 - Böttcher, Markus


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