Two-dimensional simulations of pulsational pair-instability supernovae

• Verfasst von: Chen, Ke-Jung [VerfasserIn]
• Verfasst von: Woosley, Stan [VerfasserIn]
• Verfasst von: Heger, Alexander [VerfasserIn]
• Verfasst von: Almgren, Ann [VerfasserIn]
• Verfasst von: Whalen, Daniel J. [VerfasserIn]
• Titel: Two-dimensional simulations of pulsational pair-instability supernovae
• Verf.angabe: Ke-Jung Chen, Stan Woosley, Alexander Heger, Ann Almgren, and Daniel J. Whalen
• E-Jahr: 2014
• Jahr: [2014 September 1]
• Umfang: 6 S.
• Illustrationen: Illustrationen, Diagramme
• Fussnoten: Gesehen am 16.09.2020
• Titel Quelle: Enthalten in: The astrophysical journal / 1
• Ort Quelle: London : Institute of Physics Publ., 1996
• Jahr Quelle: 2014
• Band/Heft Quelle: 792(2014,1) Artikel-Nummer 28, 6 Seiten
• ISSN Quelle: 1538-4357
• DOI: doi:10.1088/0004-637X/792/1/28
• Datenträger: Online-Ressource
• Sprache: eng
• K10plus-PPN: 1733114254

Abstract

Massive stars that end their lives with helium cores in the range of 35-65 M ☉ are known to produce repeated thermonuclear outbursts due to a recurring pair-instability. In some of these events, solar masses of material are ejected in repeated outbursts of several × 1050 erg each. Collisions between these shells can sometimes produce very luminous transients that are visible from the edge of the observable universe. Previous one-dimensional (1D) studies of these events produce thin, high-density shells as one ejection plows into another. Here, in the first multi-dimensional simulations of these collisions, we show that the development of a Rayleigh-Taylor instability truncates the growth of the high-density spike and drives mixing between the shells. The progenitor is a 110 M ☉ solar-metallicity star that was shown in earlier work to produce a superluminous supernova. The light curve of this more realistic model has a peak luminosity and duration that are similar to those of 1D models but a structure that is smoother.