Modeling the Saddle-like GeV–TeV Spectrum of HESS J1809–193: Gamma Rays Arising from Reverse-shocked Pulsar Wind Nebula?
The evolution of pulsar wind nebulae (PWNe) could be expected to leave imprints in gamma rays. We suggest that the intriguing GeV–TeV spectral energy distribution (SED) of HESS J1809–193 and Fermi-LAT source J1810.3–1925e is very likely to be the gamma-ray signature of PWN J1809–193 in light of the...
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2025-01-01
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| author | Jiaxu Sun Yang Chen Yiwei Bao Xiao Zhang Xin Zhou |
| author_facet | Jiaxu Sun Yang Chen Yiwei Bao Xiao Zhang Xin Zhou |
| author_sort | Jiaxu Sun |
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| description | The evolution of pulsar wind nebulae (PWNe) could be expected to leave imprints in gamma rays. We suggest that the intriguing GeV–TeV spectral energy distribution (SED) of HESS J1809–193 and Fermi-LAT source J1810.3–1925e is very likely to be the gamma-ray signature of PWN J1809–193 in light of the scenario that the PWN was struck by the reverse shock of the parent supernova remnant. Based on the evolutionary theory of PWNe, we consider that, when the PWN was disrupted during a collision by the reverse shock, some VHE electrons escaped impulsively. The remaining electrons stayed in the relic PWN, which was displaced from the pulsar. The VHE part of the remaining electrons was depleted by the strong magnetic field that was enhanced by the reverse shock compression in the reverberation stage, leaving the other part of them generating GeV emission. The particles injected from the pulsar after the disruption enter the relic PWN through the newly formed tunnel called the cocoon. The gamma-ray emission from the escaped electrons can account for the TeV spectrum of component A of HESS J1809–193 or the TeV halo, while the electrons remaining after disruption can account for the GeV spectrum of J1810.3–1925e. Thus, the combination of contributions from these two populations of electrons naturally reproduces the saddle-like SED of HESS 1809–193 and J1810.3–1925e from 5 GeV to 30 TeV, together with the spectral hardening around 100 GeV. We also show that the post-disruption injection of electrons can explain the spectrum of the relatively faint gamma-ray emission of component B of HESS J1809–193. |
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| spelling | doaj-art-6431ae6bc8c343db915a19aa4e2345bd2025-02-06T07:01:39ZengIOP PublishingThe Astrophysical Journal1538-43572025-01-0198019810.3847/1538-4357/ada93eModeling the Saddle-like GeV–TeV Spectrum of HESS J1809–193: Gamma Rays Arising from Reverse-shocked Pulsar Wind Nebula?Jiaxu Sun0https://orcid.org/0009-0000-5615-7769Yang Chen1https://orcid.org/0000-0002-4753-2798Yiwei Bao2https://orcid.org/0000-0001-8918-5248Xiao Zhang3https://orcid.org/0000-0002-9392-547XXin Zhou4https://orcid.org/0000-0003-2418-3350School of Astronomy & Space Science, Nanjing University , 163 Xianlin Avenue, Nanjing 210023, People's Republic of China ; ygchen@nju.edu.cnSchool of Astronomy & Space Science, Nanjing University , 163 Xianlin Avenue, Nanjing 210023, People's Republic of China ; ygchen@nju.edu.cn; Key Laboratory of Modern Astronomy and Astrophysics, Nanjing University , Ministry of Education, Nanjing 210023, People's Republic of ChinaTsung-Dao Lee Institute, Shanghai Jiao Tong University , Shanghai 201210, People's Republic of China ; sjtu0538015@sjtu.edu.cn; School of Physics and Astronomy, Shanghai Jiao Tong University , Shanghai 200240, People's Republic of ChinaSchool of Physics and Technology, Nanjing Normal University , Nanjing 210023, Jiangsu, People's Republic of China ; xiaozhang@njnu.edu.cnPurple Mountain Observatory and Key Laboratory of Radio Astronomy, Chinese Academy of Sciences , 10 Yuanhua Road, Nanjing 210023, People's Republic of ChinaThe evolution of pulsar wind nebulae (PWNe) could be expected to leave imprints in gamma rays. We suggest that the intriguing GeV–TeV spectral energy distribution (SED) of HESS J1809–193 and Fermi-LAT source J1810.3–1925e is very likely to be the gamma-ray signature of PWN J1809–193 in light of the scenario that the PWN was struck by the reverse shock of the parent supernova remnant. Based on the evolutionary theory of PWNe, we consider that, when the PWN was disrupted during a collision by the reverse shock, some VHE electrons escaped impulsively. The remaining electrons stayed in the relic PWN, which was displaced from the pulsar. The VHE part of the remaining electrons was depleted by the strong magnetic field that was enhanced by the reverse shock compression in the reverberation stage, leaving the other part of them generating GeV emission. The particles injected from the pulsar after the disruption enter the relic PWN through the newly formed tunnel called the cocoon. The gamma-ray emission from the escaped electrons can account for the TeV spectrum of component A of HESS J1809–193 or the TeV halo, while the electrons remaining after disruption can account for the GeV spectrum of J1810.3–1925e. Thus, the combination of contributions from these two populations of electrons naturally reproduces the saddle-like SED of HESS 1809–193 and J1810.3–1925e from 5 GeV to 30 TeV, together with the spectral hardening around 100 GeV. We also show that the post-disruption injection of electrons can explain the spectrum of the relatively faint gamma-ray emission of component B of HESS J1809–193.https://doi.org/10.3847/1538-4357/ada93ePulsar wind nebulaeSupernova remnantsGamma-ray sourcesCosmic rays |
| spellingShingle | Jiaxu Sun Yang Chen Yiwei Bao Xiao Zhang Xin Zhou Modeling the Saddle-like GeV–TeV Spectrum of HESS J1809–193: Gamma Rays Arising from Reverse-shocked Pulsar Wind Nebula? The Astrophysical Journal Pulsar wind nebulae Supernova remnants Gamma-ray sources Cosmic rays |
| title | Modeling the Saddle-like GeV–TeV Spectrum of HESS J1809–193: Gamma Rays Arising from Reverse-shocked Pulsar Wind Nebula? |
| title_full | Modeling the Saddle-like GeV–TeV Spectrum of HESS J1809–193: Gamma Rays Arising from Reverse-shocked Pulsar Wind Nebula? |
| title_fullStr | Modeling the Saddle-like GeV–TeV Spectrum of HESS J1809–193: Gamma Rays Arising from Reverse-shocked Pulsar Wind Nebula? |
| title_full_unstemmed | Modeling the Saddle-like GeV–TeV Spectrum of HESS J1809–193: Gamma Rays Arising from Reverse-shocked Pulsar Wind Nebula? |
| title_short | Modeling the Saddle-like GeV–TeV Spectrum of HESS J1809–193: Gamma Rays Arising from Reverse-shocked Pulsar Wind Nebula? |
| title_sort | modeling the saddle like gev tev spectrum of hess j1809 193 gamma rays arising from reverse shocked pulsar wind nebula |
| topic | Pulsar wind nebulae Supernova remnants Gamma-ray sources Cosmic rays |
| url | https://doi.org/10.3847/1538-4357/ada93e |
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