A mega-electron volt emission line in the spectrum of a gamma-ray burst.

Autor:	Ravasio ME; Department of Astrophysics, Institute for Mathematics, Astrophysics and Particle Physics, Radboud University, Nijmegen 6525 AJ, Netherlands.; Osservatorio Astronomico di Brera, Istituto Nazionale di Astrofisica, Merate 23807, Italy., Salafia OS; Osservatorio Astronomico di Brera, Istituto Nazionale di Astrofisica, Merate 23807, Italy.; Sezione di Milano-Bicocca, Istituto Nazionale di Fisica Nucleare, Milan 20146, Italy., Oganesyan G; Gran Sasso Science Institute, L'Aquila I-67100, Italy.; Laboratori Nazionali del Gran Sasso, Istituto Nazionale di Fisica Nucleare, L'Aquila I-67100, Italy., Mei A; Gran Sasso Science Institute, L'Aquila I-67100, Italy.; Laboratori Nazionali del Gran Sasso, Istituto Nazionale di Fisica Nucleare, L'Aquila I-67100, Italy., Ghirlanda G; Osservatorio Astronomico di Brera, Istituto Nazionale di Astrofisica, Merate 23807, Italy.; Sezione di Milano-Bicocca, Istituto Nazionale di Fisica Nucleare, Milan 20146, Italy., Ascenzi S; Gran Sasso Science Institute, L'Aquila I-67100, Italy.; Laboratori Nazionali del Gran Sasso, Istituto Nazionale di Fisica Nucleare, L'Aquila I-67100, Italy.; Institute of Space Sciences, Consejo Superior de Investigaciones Científicas, Campus Universitat Autònoma de Barcelona, Barcelona E-08193, Spain.; Institut d'Estudis Espacials de Catalunya, Barcelona E-08034, Spain., Banerjee B; Gran Sasso Science Institute, L'Aquila I-67100, Italy.; Laboratori Nazionali del Gran Sasso, Istituto Nazionale di Fisica Nucleare, L'Aquila I-67100, Italy., Macera S; Gran Sasso Science Institute, L'Aquila I-67100, Italy.; Laboratori Nazionali del Gran Sasso, Istituto Nazionale di Fisica Nucleare, L'Aquila I-67100, Italy., Branchesi M; Gran Sasso Science Institute, L'Aquila I-67100, Italy.; Laboratori Nazionali del Gran Sasso, Istituto Nazionale di Fisica Nucleare, L'Aquila I-67100, Italy., Jonker PG; Department of Astrophysics, Institute for Mathematics, Astrophysics and Particle Physics, Radboud University, Nijmegen 6525 AJ, Netherlands.; Netherlands Institute for Space Research, Leiden 2333 CA, Netherlands., Levan AJ; Department of Astrophysics, Institute for Mathematics, Astrophysics and Particle Physics, Radboud University, Nijmegen 6525 AJ, Netherlands.; Department of Physics, University of Warwick, Coventry CV4 7AL, UK., Malesani DB; Department of Astrophysics, Institute for Mathematics, Astrophysics and Particle Physics, Radboud University, Nijmegen 6525 AJ, Netherlands.; Cosmic Dawn Center, Copenhagen, Denmark.; Niels Bohr Institute, University of Copenhagen, Copenhagen N 2200, Denmark., Mulrey KB; Department of Astrophysics, Institute for Mathematics, Astrophysics and Particle Physics, Radboud University, Nijmegen 6525 AJ, Netherlands.; Nationaal Instituut voor Kernfysica en Hoge-Energiefysica, Amsterdam 1098 XG, Netherlands., Giuliani A; Istituto di Astrofisica Spaziale e Fisica Cosmica, Istituto Nazionale di Astrofisica, Milan I-20133, Italy., Celotti A; Osservatorio Astronomico di Brera, Istituto Nazionale di Astrofisica, Merate 23807, Italy.; Scuola Internazionale Superiore di Studi Avanzati, Trieste I-34136, Italy.; Sezione di Trieste, Istituto Nazionale di Fisica Nucleare, Trieste I-34127, Italy., Ghisellini G; Osservatorio Astronomico di Brera, Istituto Nazionale di Astrofisica, Merate 23807, Italy.
Jazyk:	angličtina
Zdroj:	Science (New York, N.Y.) [Science] 2024 Jul 26; Vol. 385 (6707), pp. 452-455. Date of Electronic Publication: 2024 Jul 25.
DOI:	10.1126/science.adj3638
Abstrakt:	A long gamma-ray burst (GRB) is observed when the collapse of a massive star produces an ultrarelativistic outflow pointed toward Earth. Gamma-ray spectra of long GRBs are smooth, typically modeled by joint power-law segments describing a continuum, with no detected spectral lines. We report a significant (>6σ) narrow emission feature at ~10 mega-electron volts (MeV) in the spectrum of the bright GRB 221009A. Over 80 seconds, it evolves in energy (~12 to ~6 MeV) and in luminosity (~1.1 to <0.43 × 10 50 erg second -1 ) but has a constant width of ~1 MeV. We interpret this feature as a blueshifted spectral line produced by the annihilation of electron-positron pairs, potentially in the same location responsible for emitting the brightest GRB pulses.
Databáze:	MEDLINE
Externí odkaz:	Zobrazit plný text záznamu Plný text ve formátu PDF