Perego, A. (2018)
υ-driven winds from the remnant of binary neutron star mergers.
In: Journal of Physics: Conference Series, 940 (1)
doi: 10.1088/1742-6596/940/1/012018
Artikel, Bibliographie
Dies ist die neueste Version dieses Eintrags.
Kurzbeschreibung (Abstract)
We present a 3D hydrodynamic study of the neutrino-driven winds that emerge from the remnant of a neutron star merger, represented by a thick accretion disc orbiting around a massive neutron star. This strong baryonic wind is blown out by neutrino absorption on free baryons inside the disc. It expands within a few tens of ms along the original binary rotation axis. If the central object survives for at least 200ms, the mass ejected in the wind can reach 5% of the initial mass of the accretion disc. Due to the intense neutrino irradiation, matter ejected in the wind increases its electron fraction between 0.3 and 0.4, producing weak r-process nucleosynthesis yields. We predict a distinct UV/optical transient associated with the wind ejecta that peaks from a few hours to a few days after the merger.
Typ des Eintrags: | Artikel |
---|---|
Erschienen: | 2018 |
Autor(en): | Perego, A. |
Art des Eintrags: | Bibliographie |
Titel: | υ-driven winds from the remnant of binary neutron star mergers |
Sprache: | Englisch |
Publikationsjahr: | 2018 |
Ort: | Bristol |
Verlag: | IOP Publishing |
Titel der Zeitschrift, Zeitung oder Schriftenreihe: | Journal of Physics: Conference Series |
Jahrgang/Volume einer Zeitschrift: | 940 |
(Heft-)Nummer: | 1 |
Kollation: | 4 Seiten |
DOI: | 10.1088/1742-6596/940/1/012018 |
Zugehörige Links: | |
Kurzbeschreibung (Abstract): | We present a 3D hydrodynamic study of the neutrino-driven winds that emerge from the remnant of a neutron star merger, represented by a thick accretion disc orbiting around a massive neutron star. This strong baryonic wind is blown out by neutrino absorption on free baryons inside the disc. It expands within a few tens of ms along the original binary rotation axis. If the central object survives for at least 200ms, the mass ejected in the wind can reach 5% of the initial mass of the accretion disc. Due to the intense neutrino irradiation, matter ejected in the wind increases its electron fraction between 0.3 and 0.4, producing weak r-process nucleosynthesis yields. We predict a distinct UV/optical transient associated with the wind ejecta that peaks from a few hours to a few days after the merger. |
ID-Nummer: | Artikel-ID: 012018 |
Zusätzliche Informationen: | Nuclear Physics in Astrophysics Conference (NPA VII) 18–22 May 2015, York, UK |
Sachgruppe der Dewey Dezimalklassifikatin (DDC): | 500 Naturwissenschaften und Mathematik > 530 Physik |
Fachbereich(e)/-gebiet(e): | 05 Fachbereich Physik 05 Fachbereich Physik > Institut für Kernphysik |
Hinterlegungsdatum: | 13 Mai 2024 06:05 |
Letzte Änderung: | 13 Mai 2024 06:05 |
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υ-driven winds from the remnant of binary neutron star mergers. (deposited 07 Mai 2024 13:54)
- υ-driven winds from the remnant of binary neutron star mergers. (deposited 13 Mai 2024 06:05) [Gegenwärtig angezeigt]
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