Multiwavelength Emission of Gamma-Ray Burst Prompt Phase. II. Spectral Polarimetry
Polarization spectra were predicted within the photosphere model. To seek more clues to distinguish between the models, both the time-resolved and time-integrated polarization spectra from optical band to MeV gamma-rays of the magnetic reconnection model are studied here. There are two newly found d...
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IOP Publishing
2025-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/ada5f1 |
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| author | Jia-Sheng Li Mi-Xiang Lan |
| author_facet | Jia-Sheng Li Mi-Xiang Lan |
| author_sort | Jia-Sheng Li |
| collection | DOAJ |
| description | Polarization spectra were predicted within the photosphere model. To seek more clues to distinguish between the models, both the time-resolved and time-integrated polarization spectra from optical band to MeV gamma-rays of the magnetic reconnection model are studied here. There are two newly found differences between the two models. First, the time-integrated polarization degree of the magnetic reconnection model would in general increase with frequency for on-axis observations, while it is not monotonous for the photosphere model. Second, the variations of both the time-integrated and the time-resolved polarization angles (PAs) with frequency of the magnetic reconnection model are not random, while the time-integrated PA varies randomly with frequency for the photosphere model. Therefore, future energy-resolved polarization analysis could distinguish between the two models. In addition, the PA rotation spectra are studied for the first time. The rotation value of PA within the burst duration will decrease with the increase of the observational energy band. Most significant PA rotation would happen for slightly off-axis observations in each energy band. The PA would rotate even for on-axis observations in the optical band. Compared with the aligned magnetic field case, the PA rotation is quite rare in the gamma-ray band for the case with a toroidal field in the radiation region. |
| format | Article |
| id | doaj-art-4276796a1d404339b2207b38f637b829 |
| institution | Kabale University |
| issn | 1538-4357 |
| language | English |
| publishDate | 2025-01-01 |
| publisher | IOP Publishing |
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| series | The Astrophysical Journal |
| spelling | doaj-art-4276796a1d404339b2207b38f637b8292025-01-28T06:58:34ZengIOP PublishingThe Astrophysical Journal1538-43572025-01-01979221910.3847/1538-4357/ada5f1Multiwavelength Emission of Gamma-Ray Burst Prompt Phase. II. Spectral PolarimetryJia-Sheng Li0Mi-Xiang Lan1https://orcid.org/0000-0001-5641-2598Center for Theoretical Physics and College of Physics, Jilin University , Changchun 130012, People’s Republic of China ; lanmixiang@jlu.edu.cnCenter for Theoretical Physics and College of Physics, Jilin University , Changchun 130012, People’s Republic of China ; lanmixiang@jlu.edu.cnPolarization spectra were predicted within the photosphere model. To seek more clues to distinguish between the models, both the time-resolved and time-integrated polarization spectra from optical band to MeV gamma-rays of the magnetic reconnection model are studied here. There are two newly found differences between the two models. First, the time-integrated polarization degree of the magnetic reconnection model would in general increase with frequency for on-axis observations, while it is not monotonous for the photosphere model. Second, the variations of both the time-integrated and the time-resolved polarization angles (PAs) with frequency of the magnetic reconnection model are not random, while the time-integrated PA varies randomly with frequency for the photosphere model. Therefore, future energy-resolved polarization analysis could distinguish between the two models. In addition, the PA rotation spectra are studied for the first time. The rotation value of PA within the burst duration will decrease with the increase of the observational energy band. Most significant PA rotation would happen for slightly off-axis observations in each energy band. The PA would rotate even for on-axis observations in the optical band. Compared with the aligned magnetic field case, the PA rotation is quite rare in the gamma-ray band for the case with a toroidal field in the radiation region.https://doi.org/10.3847/1538-4357/ada5f1Gamma-ray burstsMagnetic fieldsStarlight polarization |
| spellingShingle | Jia-Sheng Li Mi-Xiang Lan Multiwavelength Emission of Gamma-Ray Burst Prompt Phase. II. Spectral Polarimetry The Astrophysical Journal Gamma-ray bursts Magnetic fields Starlight polarization |
| title | Multiwavelength Emission of Gamma-Ray Burst Prompt Phase. II. Spectral Polarimetry |
| title_full | Multiwavelength Emission of Gamma-Ray Burst Prompt Phase. II. Spectral Polarimetry |
| title_fullStr | Multiwavelength Emission of Gamma-Ray Burst Prompt Phase. II. Spectral Polarimetry |
| title_full_unstemmed | Multiwavelength Emission of Gamma-Ray Burst Prompt Phase. II. Spectral Polarimetry |
| title_short | Multiwavelength Emission of Gamma-Ray Burst Prompt Phase. II. Spectral Polarimetry |
| title_sort | multiwavelength emission of gamma ray burst prompt phase ii spectral polarimetry |
| topic | Gamma-ray bursts Magnetic fields Starlight polarization |
| url | https://doi.org/10.3847/1538-4357/ada5f1 |
| work_keys_str_mv | AT jiashengli multiwavelengthemissionofgammarayburstpromptphaseiispectralpolarimetry AT mixianglan multiwavelengthemissionofgammarayburstpromptphaseiispectralpolarimetry |