GRB 171205A: Hypernova and Newborn Neutron Star
GRB 171205A is a low-luminosity, long-duration gamma-ray burst (GRB) associated with SN 2017iuk, a broad-line type Ic supernova (SN). It is consistent with having been formed in the core collapse of a widely separated binary, which we have called the binary-driven hypernova of type III. The core col...
| Main Authors: | , , , , |
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| Format: | Article |
| Language: | English |
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IOP Publishing
2023-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/acb771 |
| _version_ | 1797702073721028608 |
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| author | Yu Wang L. M. Becerra C. L. Fryer J. A. Rueda R. Ruffini |
| author_facet | Yu Wang L. M. Becerra C. L. Fryer J. A. Rueda R. Ruffini |
| author_sort | Yu Wang |
| collection | DOAJ |
| description | GRB 171205A is a low-luminosity, long-duration gamma-ray burst (GRB) associated with SN 2017iuk, a broad-line type Ic supernova (SN). It is consistent with having been formed in the core collapse of a widely separated binary, which we have called the binary-driven hypernova of type III. The core collapse of the CO star forms a newborn NS ( ν NS) and the SN explosion. Fallback accretion transfers mass and angular momentum to the ν NS, here assumed to be born non-rotating. The accretion energy injected into the expanding stellar layers powers the prompt emission. The multiwavelength power-law afterglow is explained by the synchrotron radiation of electrons in the SN ejecta, powered by energy injected by the spinning ν NS. We calculate the amount of mass and angular momentum gained by the ν NS, as well as the ν NS rotational evolution. The ν NS spins up to a period of 47 ms, then releases its rotational energy powering the synchrotron emission of the afterglow. The paucity of the ν NS spin explains the low-luminosity characteristic and that the optical emission of the SN from the nickel radioactive decay outshines the optical emission from the synchrotron radiation. From the ν NS evolution, we infer that the SN explosion had to occur at most 7.36 h before the GRB trigger. Therefore, for the first time, the analysis of the GRB data leads to the time of occurrence of the CO core collapse leading to the SN explosion and the electromagnetic emission of the GRB event. |
| first_indexed | 2024-03-12T04:44:54Z |
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| language | English |
| last_indexed | 2024-03-12T04:44:54Z |
| publishDate | 2023-01-01 |
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| series | The Astrophysical Journal |
| spelling | doaj.art-55ff2b456b1047278e207f35104474432023-09-03T09:29:32ZengIOP PublishingThe Astrophysical Journal1538-43572023-01-0194529510.3847/1538-4357/acb771GRB 171205A: Hypernova and Newborn Neutron StarYu Wang0L. M. Becerra1C. L. Fryer2https://orcid.org/0000-0003-2624-0056J. A. Rueda3R. Ruffini4https://orcid.org/0000-0003-0829-8318ICRA, Dipartimento di Fisica, Università di Roma “La Sapienza” , Piazzale Aldo Moro 5, I-00185 Roma, Italy ; yu.wang@inaf.it, laura.marcela.becerra@gmail.com, fryer@lanl.gov; ICRANet , Piazza della Repubblica 10, I-65122 Pescara, Italy ; jorge.rueda@icra.it; INAF–Osservatorio Astronomico d’Abruzzo , Via M. Maggini snc, I-64100, Teramo, Italy ; ruffini@icra.itICRANet , Piazza della Repubblica 10, I-65122 Pescara, Italy ; jorge.rueda@icra.it; Escuela de Física, Universidad Industrial de Santander , A.A.678, Bucaramanga, 680002, ColombiaCenter for Theoretical Astrophysics, Los Alamos National Laboratory , Los Alamos, NM, 87545, USA; Computer, Computational, and Statistical Sciences Division, Los Alamos National Laboratory , Los Alamos, NM, 87545, USA; The University of Arizona , Tucson, AZ 85721, USA; Department of Physics and Astronomy, The University of New Mexico , Albuquerque, NM 87131, USA; The George Washington University , Washington, DC 20052, USAICRA, Dipartimento di Fisica, Università di Roma “La Sapienza” , Piazzale Aldo Moro 5, I-00185 Roma, Italy ; yu.wang@inaf.it, laura.marcela.becerra@gmail.com, fryer@lanl.gov; ICRANet , Piazza della Repubblica 10, I-65122 Pescara, Italy ; jorge.rueda@icra.it; ICRANet-Ferrara, Dipartimento di Fisica e Scienze della Terra, Università degli Studi di Ferrara , Via Saragat 1, I-44122 Ferrara, Italy; Dipartimento di Fisica e Scienze della Terra, Università degli Studi di Ferrara , Via Saragat 1, I-44122 Ferrara, Italy; INAF – Istituto di Astrofisica e Planetologia Spaziali, Via Fosso del Cavaliere 100, I-00133 Rome, ItalyICRA, Dipartimento di Fisica, Università di Roma “La Sapienza” , Piazzale Aldo Moro 5, I-00185 Roma, Italy ; yu.wang@inaf.it, laura.marcela.becerra@gmail.com, fryer@lanl.gov; ICRANet , Piazza della Repubblica 10, I-65122 Pescara, Italy ; jorge.rueda@icra.it; INAF , Viale del Parco Mellini 84, I-00136 Rome, ItalyGRB 171205A is a low-luminosity, long-duration gamma-ray burst (GRB) associated with SN 2017iuk, a broad-line type Ic supernova (SN). It is consistent with having been formed in the core collapse of a widely separated binary, which we have called the binary-driven hypernova of type III. The core collapse of the CO star forms a newborn NS ( ν NS) and the SN explosion. Fallback accretion transfers mass and angular momentum to the ν NS, here assumed to be born non-rotating. The accretion energy injected into the expanding stellar layers powers the prompt emission. The multiwavelength power-law afterglow is explained by the synchrotron radiation of electrons in the SN ejecta, powered by energy injected by the spinning ν NS. We calculate the amount of mass and angular momentum gained by the ν NS, as well as the ν NS rotational evolution. The ν NS spins up to a period of 47 ms, then releases its rotational energy powering the synchrotron emission of the afterglow. The paucity of the ν NS spin explains the low-luminosity characteristic and that the optical emission of the SN from the nickel radioactive decay outshines the optical emission from the synchrotron radiation. From the ν NS evolution, we infer that the SN explosion had to occur at most 7.36 h before the GRB trigger. Therefore, for the first time, the analysis of the GRB data leads to the time of occurrence of the CO core collapse leading to the SN explosion and the electromagnetic emission of the GRB event.https://doi.org/10.3847/1538-4357/acb771Gamma-ray burstsNeutron starsPulsars |
| spellingShingle | Yu Wang L. M. Becerra C. L. Fryer J. A. Rueda R. Ruffini GRB 171205A: Hypernova and Newborn Neutron Star The Astrophysical Journal Gamma-ray bursts Neutron stars Pulsars |
| title | GRB 171205A: Hypernova and Newborn Neutron Star |
| title_full | GRB 171205A: Hypernova and Newborn Neutron Star |
| title_fullStr | GRB 171205A: Hypernova and Newborn Neutron Star |
| title_full_unstemmed | GRB 171205A: Hypernova and Newborn Neutron Star |
| title_short | GRB 171205A: Hypernova and Newborn Neutron Star |
| title_sort | grb 171205a hypernova and newborn neutron star |
| topic | Gamma-ray bursts Neutron stars Pulsars |
| url | https://doi.org/10.3847/1538-4357/acb771 |
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