Gespeichert in:
| Hauptverfasser: | , |
|---|---|
| Format: | Preprint |
| Veröffentlicht: |
2024
|
| Schlagworte: | |
| Online-Zugang: | https://arxiv.org/abs/2403.04518 |
| Tags: |
Tag hinzufügen
Keine Tags, Fügen Sie den ersten Tag hinzu!
|
| _version_ | 1866910357269774336 |
|---|---|
| author | Wang, Chi-Zhuo Jiang, Yun-Guo |
| author_facet | Wang, Chi-Zhuo Jiang, Yun-Guo |
| contents | The variation mechanism of blazars is a long-standing unresolved problem. In this work, we present a scenario to explain diverse variation phenomena for ON 231, where the jet emissions are composed of the flaring and the less variable components (most probably from the post-flaring blobs), and the variation is dominated by shock-in-jet instead of the Doppler effect. We perform correlation analysis for the multiwavelength light curves and find no significant correlations. For optical band, ON 231 exhibits a harder when brighter (HWB) trend, and the trend seems to shift at different periods. Correspondingly, the correlation between polarization degree and flux exhibits a V-shaped behavior, and a similar translation relation during different periods is also found. These phenomena could be understood via the superposition of the flaring component and slowly varying background component. We also find that the slopes of HWB trend become smaller at higher flux levels, which indicates the energy-dependent acceleration processes of the radiative particles. For X-ray, we discover a trend transition from HWB to softer when brighter (SWB) to HWB. We consider that the X-ray emission is composed of both the synchrotron tail and the Synchrotron Self-Compton components, which could be described by two log-parabolic functions. By varying the peak frequency, we reproduce the observed trend transition in a quantitative manner. For $γ$-ray, we find the SWB trend, which could be explained naturally if a very-high-energy $γ$-ray background component exists. Our study elucidates the variation mechanism of intermediate synchrotron-peaked BL Lac objects. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2403_04518 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Revealing the variation mechanism of ON 231 via the two-components shock-in-jet model Wang, Chi-Zhuo Jiang, Yun-Guo High Energy Astrophysical Phenomena The variation mechanism of blazars is a long-standing unresolved problem. In this work, we present a scenario to explain diverse variation phenomena for ON 231, where the jet emissions are composed of the flaring and the less variable components (most probably from the post-flaring blobs), and the variation is dominated by shock-in-jet instead of the Doppler effect. We perform correlation analysis for the multiwavelength light curves and find no significant correlations. For optical band, ON 231 exhibits a harder when brighter (HWB) trend, and the trend seems to shift at different periods. Correspondingly, the correlation between polarization degree and flux exhibits a V-shaped behavior, and a similar translation relation during different periods is also found. These phenomena could be understood via the superposition of the flaring component and slowly varying background component. We also find that the slopes of HWB trend become smaller at higher flux levels, which indicates the energy-dependent acceleration processes of the radiative particles. For X-ray, we discover a trend transition from HWB to softer when brighter (SWB) to HWB. We consider that the X-ray emission is composed of both the synchrotron tail and the Synchrotron Self-Compton components, which could be described by two log-parabolic functions. By varying the peak frequency, we reproduce the observed trend transition in a quantitative manner. For $γ$-ray, we find the SWB trend, which could be explained naturally if a very-high-energy $γ$-ray background component exists. Our study elucidates the variation mechanism of intermediate synchrotron-peaked BL Lac objects. |
| title | Revealing the variation mechanism of ON 231 via the two-components shock-in-jet model |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2403.04518 |