TWO-DIMENSIONAL SIMULATIONS OF PULSATIONAL PAIR-INSTABILITY SUPERNOVAE

2014/02/28 by Ke-Jung Chen, Stan Woosley, Alexander Heger +3 · 7 citations
Physics and Astronomy · #Astronomy and Astrophysical Research #Gamma-ray bursts and supernovae #Helium #Light curve #Luminosity #Observable #Pulsars and Gravitational Waves Research #Stars #Stellar evolution #Supernova #Thermonuclear fusion #astro-ph.CO #astro-ph.HE #astro-ph.SR

paper · pdf · doi:10.1088/0004-637x/792/1/28

26 pages, 9 figures (accepted to ApJ)

arxiv created 2014/07/06 · openalex publication_date 2014/08/12 · arxiv updated 2015/06/18 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05

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 × 10 50 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.

Citations

• Pengaruh Kompensasi Finansial terhadap Loyalitas dan Kinerja Karyawan (Studi Kasus pada PT. Maya Food Industri, Pekalongan)
• The Nucleosynthetic Signature of Population III

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