HESS J1809-193: Gamma-Ray Emission by Cosmic Rays from Past Explosion
arXiv:2311.07481 · doi:10.3847/1538-4357/ad0da9
Abstract
The very high energy gamma-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 gamma-ray production due to the presence of supernova remnants, pulsar 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 gamma-ray source HESS J1809-193. We explain the multi-wavelength data from the region of HESS J1809-193 with synchrotron, inverse Compton, bremsstrahlung emission of cosmic ray electrons and secondary gamma-ray production in interactions of cosmic ray protons with the cold protons in the local molecular clouds within a time-dependent framework including the diffusion loss of cosmic rays. The observational data has been modelled with the secondary photons produced by the time-evolved cosmic ray spectrum, assuming the age of the explosion is 4500 years.
8 pages, 6 figures, Accepted in ApJ
References in corpus (8)
- Extended gamma-ray sources around pulsars constrain the origin of the positron flux at Earth
- Parametrization of gamma-ray production cross-sections for pp interactions in a broad proton energy range from the kinematic threshold to PeV energies
- FOREST Unbiased Galactic plane Imaging survey with the Nobeyama 45-m telescope (FUGIN) I: Project Overview and Initial Results
- Discovery of 35 New Supernova Remnants in the Inner Galaxy
- A radiation transfer model for the Milky-Way: I. Radiation fields and application to High Energy Astrophysics
- X-ray emission from PSR J1809-1917 and its pulsar wind nebula, possibly associated with the TeV gamma-ray source HESS J1809-193
- HESS J1809193: a halo of escaped electrons around a pulsar wind nebula?
- Revisiting the Chandra Observation on the Region of PSR J1809-1917: Indication of an X-ray Halo and Implication for the Origin of HESS J1809-193