Exploring <i>γ</i>-Ray Flares from High-Redshift Blazar B3 1343+451 at GeV Energies
We study the temporal and spectral variability properties of the high-redshift blazar B3 1343+451 utilizing Fermi-LAT data from 2008 to 2022 in the energy range of 0.1–300 GeV. We identify six major flares with many substructures and analyze their temporal and spectral properties in detail. The fast...
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2024-11-01
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| author | Xiongfei Geng Yang Liu Gang Cao Jing Fan Xiongbang Yang Nan Ding Minghu Gao Yehui Yang Zhijie Zhang |
| author_facet | Xiongfei Geng Yang Liu Gang Cao Jing Fan Xiongbang Yang Nan Ding Minghu Gao Yehui Yang Zhijie Zhang |
| author_sort | Xiongfei Geng |
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| description | We study the temporal and spectral variability properties of the high-redshift blazar B3 1343+451 utilizing Fermi-LAT data from 2008 to 2022 in the energy range of 0.1–300 GeV. We identify six major flares with many substructures and analyze their temporal and spectral properties in detail. The fastest rise and decay timescales are found to be 4.8 ± 0.48 h and 5.28 ± 0.72 h, respectively. The size of the emission region is constrained to be <i>R</i> ∼ 5.18 × <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mn>10</mn><mn>15</mn></msup></semantics></math></inline-formula>–1.56 × <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mn>10</mn><mn>16</mn></msup></semantics></math></inline-formula> cm with the typical Doppler factors of <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mi>δ</mi></semantics></math></inline-formula> ∼ 10–30. Most of the peaks from the flares exhibit a symmetric temporal profile within the error bars, implying that the rise and decay timescales are dominated by the disturbances caused by dense plasma blobs passing through the standing shock front in the jet region. We also find that four flares are better fitted with a log-parabolic distribution, while two flares are better fitted with a power-law distribution. Our results indicate that the emission regions vary from one flare to another, which is consistent with earlier results. |
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| issn | 2218-1997 |
| language | English |
| publishDate | 2024-11-01 |
| publisher | MDPI AG |
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| series | Universe |
| spelling | doaj-art-3c607bcb6be44b6cb47a26a8b3aa01ac2025-08-20T02:04:44ZengMDPI AGUniverse2218-19972024-11-01101142310.3390/universe10110423Exploring <i>γ</i>-Ray Flares from High-Redshift Blazar B3 1343+451 at GeV EnergiesXiongfei Geng0Yang Liu1Gang Cao2Jing Fan3Xiongbang Yang4Nan Ding5Minghu Gao6Yehui Yang7Zhijie Zhang8School of Electrical and Information Technology, Yunnan Minzu University, Kunming 650504, ChinaSchool of Physics and Astronomy, Yunnan University, Kunming 650091, ChinaDepartment of Mathematics, Yunnan University of Finance and Economics, Kunming 650221, ChinaSchool of Electrical and Information Technology, Yunnan Minzu University, Kunming 650504, ChinaDepartment of Mathematics, Yunnan University of Finance and Economics, Kunming 650221, ChinaSchool of Physical Science and Technology, Kunming University, Kunming 650214, ChinaSchool of Electrical and Information Technology, Yunnan Minzu University, Kunming 650504, ChinaSchool of Electrical and Information Technology, Yunnan Minzu University, Kunming 650504, ChinaDepartment of Astronomy and Jiujiang Research Institute, Xiamen University, Xiamen 361005, ChinaWe study the temporal and spectral variability properties of the high-redshift blazar B3 1343+451 utilizing Fermi-LAT data from 2008 to 2022 in the energy range of 0.1–300 GeV. We identify six major flares with many substructures and analyze their temporal and spectral properties in detail. The fastest rise and decay timescales are found to be 4.8 ± 0.48 h and 5.28 ± 0.72 h, respectively. The size of the emission region is constrained to be <i>R</i> ∼ 5.18 × <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mn>10</mn><mn>15</mn></msup></semantics></math></inline-formula>–1.56 × <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mn>10</mn><mn>16</mn></msup></semantics></math></inline-formula> cm with the typical Doppler factors of <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mi>δ</mi></semantics></math></inline-formula> ∼ 10–30. Most of the peaks from the flares exhibit a symmetric temporal profile within the error bars, implying that the rise and decay timescales are dominated by the disturbances caused by dense plasma blobs passing through the standing shock front in the jet region. We also find that four flares are better fitted with a log-parabolic distribution, while two flares are better fitted with a power-law distribution. Our results indicate that the emission regions vary from one flare to another, which is consistent with earlier results.https://www.mdpi.com/2218-1997/10/11/423blazarsγ-rayactive galactic nucleiB3 1343+451 |
| spellingShingle | Xiongfei Geng Yang Liu Gang Cao Jing Fan Xiongbang Yang Nan Ding Minghu Gao Yehui Yang Zhijie Zhang Exploring <i>γ</i>-Ray Flares from High-Redshift Blazar B3 1343+451 at GeV Energies Universe blazars γ-ray active galactic nuclei B3 1343+451 |
| title | Exploring <i>γ</i>-Ray Flares from High-Redshift Blazar B3 1343+451 at GeV Energies |
| title_full | Exploring <i>γ</i>-Ray Flares from High-Redshift Blazar B3 1343+451 at GeV Energies |
| title_fullStr | Exploring <i>γ</i>-Ray Flares from High-Redshift Blazar B3 1343+451 at GeV Energies |
| title_full_unstemmed | Exploring <i>γ</i>-Ray Flares from High-Redshift Blazar B3 1343+451 at GeV Energies |
| title_short | Exploring <i>γ</i>-Ray Flares from High-Redshift Blazar B3 1343+451 at GeV Energies |
| title_sort | exploring i γ i ray flares from high redshift blazar b3 1343 451 at gev energies |
| topic | blazars γ-ray active galactic nuclei B3 1343+451 |
| url | https://www.mdpi.com/2218-1997/10/11/423 |
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