Perego, A. (2024)
υ-driven winds from the remnant of binary neutron star mergers.
In: Journal of Physics: Conference Series, 2018, 940 (1)
doi: 10.26083/tuprints-00020916
Artikel, Zweitveröffentlichung, Verlagsversion
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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: | 2024 |
| Autor(en): | Perego, A. |
| Art des Eintrags: | Zweitveröffentlichung |
| Titel: | υ-driven winds from the remnant of binary neutron star mergers |
| Sprache: | Englisch |
| Publikationsjahr: | 7 Mai 2024 |
| Ort: | Darmstadt |
| Publikationsdatum der Erstveröffentlichung: | 2018 |
| Ort der Erstveröffentlichung: | 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: | 10.26083/tuprints-00020916 |
| URL / URN: | https://tuprints.ulb.tu-darmstadt.de/20916 |
| Zugehörige Links: | |
| Herkunft: | Zweitveröffentlichung DeepGreen |
| 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 |
| Status: | Verlagsversion |
| URN: | urn:nbn:de:tuda-tuprints-209161 |
| 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: | 07 Mai 2024 13:54 |
| 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) [Gegenwärtig angezeigt]
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