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Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/8261
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dc.contributor.authorBoxi, Sovan-
dc.contributor.authorGupta, Nayantara-
dc.date.accessioned2024-06-05T04:06:27Z-
dc.date.available2024-06-05T04:06:27Z-
dc.date.issued2024-01-15-
dc.identifier.citationThe Astrophysical Journal, 2024, Vol.961, p61en_US
dc.identifier.urihttp://hdl.handle.net/2289/8261-
dc.descriptionOpen Accessen_US
dc.description.abstractThe very-high-energy γ-ray source HESS J1809-193 has been detected by the LHAASO and HAWC observatory beyond 100 TeV energy. It is an interesting candidate for exploring the underlying mechanisms of γ-ray production due to the presence of supernova remnants, pulsars, and molecular clouds close to it. We have considered the injection of the energetic cosmic rays from a past explosion, whose reminiscent may be SNR G011.0-00.0, which is located within the extended γ-ray source HESS J1809-193. We explain the multiwavelength data from the region of HESS J1809-193 with synchrotron, inverse Compton, and bremsstrahlung emission of cosmic-ray electrons and secondary γ-ray production in interactions of cosmic-ray protons with the cold protons in the localmolecular clouds within a time-dependent framework including the diffusion loss of cosmic rays. The observational data have been modeled with the secondary photons produced by the time-evolved cosmic-ray spectrum assuming the age of the explosion is 4500 yr.en_US
dc.language.isoenen_US
dc.publisherAmerican Astronomical Societyen_US
dc.relation.urihttps://ui.adsabs.harvard.edu/abs/2024ApJ...961...61B/abstracten_US
dc.relation.urihttps://arxiv.org/abs/2311.07481en_US
dc.relation.urihttps://doi.org/10.3847/1538-4357/ad0da9en_US
dc.rights2024, The Author(s)en_US
dc.subjectHigh energy astrophysicsen_US
dc.subjectGamma-raysen_US
dc.subjectSupernova remnantsen_US
dc.titleHESS J1809-193: Gamma-Ray Emission by Cosmic Rays from a Past Explosionen_US
dc.typeArticleen_US
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