A Photo-Hadronic Model of the Large Scale Jets of 3C 273 and PKS 1136-135
| Autor: | Fumio Takahara, Masaaki Kusunose |
|---|---|
| Jazyk: | angličtina |
| Rok vydání: | 2018 |
| Předmět: |
High Energy Astrophysical Phenomena (astro-ph.HE)
Physics Photon Active galactic nucleus Proton 010308 nuclear & particles physics Astrophysics::High Energy Astrophysical Phenomena Cosmic microwave background FOS: Physical sciences Synchrotron radiation Astronomy and Astrophysics Quasar Astrophysics Electron Astrophysics::Cosmology and Extragalactic Astrophysics 01 natural sciences Pair production Space and Planetary Science 0103 physical sciences Astrophysics - High Energy Astrophysical Phenomena 010303 astronomy & astrophysics Astrophysics::Galaxy Astrophysics |
| Popis: | X-ray bright knots of kpc-scale jets of several radio loud quasars have been an actively discussed issue. Among various models to explain observations, synchrotron radiation from the electron population different from radio to IR emitting electrons is promising. However, the origin of this electron population has been debated. Recently, we proposed that this electron population is produced by proton-photon collisions (mainly, Bethe-Heitler process), and we applied this model to PKS 0637-752. We found that this model works if the proton power is by an order of magnitude larger than the Eddington power. In this paper we apply this model to the X-ray emission in the knots of 3C 273 and PKS 1136-135. The target photons for electron-positron pair production are supplied by synchrotron radiation at radio-IR by primary electrons and by the active galactic nucleus (AGN) core as well as cosmic microwave background (CMB) radiation. The effects of the AGN photons are included for the first time in the hadronic model. Though the observed X-ray flux is obtained with the contribution of the AGN photons, the required proton power turns out to be highly super-Eddington. However, we find that our model works for a nearly Eddington proton power, if the photon density of the AGN is enhanced. This can occur if the AGN photons are more beamed toward the X-ray knots than toward our line of sight and the AGN photon frequency is shifted by the Doppler effect. 20 pages, 11 figures, accepted for publication in ApJ |
| Databáze: | OpenAIRE |
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