Journal
ASTROPHYSICAL JOURNAL
Volume 792, Issue 1, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/792/1/28
Keywords
early universe; hydrodynamics; instabilities; shock waves; stars: massive; supernovae: general
Categories
Funding
- IAU
- DOE HEP Program [DE-SC0010676]
- National Science Foundation [AST 0909129]
- NASA Theory Program [NNX14AH34G]
- Australian Research Council [ARC FT 120100363]
- Baden-Wurttemberg-Stiftung [P-LS-SPII/18]
- DOE [DE-SC0010676, DE-AC02-05CH11231, DE-GF02-87ER40328, DE-FC02-09ER41618]
- NSF [AST-1109394, PHY02-16783]
- National Nuclear Security Administration of the US Department of Energy at Los Alamos National Laboratory [DE-AC52-06NA25396]
- U.S. Department of Energy (DOE) [DE-SC0010676] Funding Source: U.S. Department of Energy (DOE)
- NASA [683662, NNX14AH34G] Funding Source: Federal RePORTER
- Direct For Mathematical & Physical Scien
- Division Of Physics [1430152] Funding Source: National Science Foundation
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Massive stars that end their lives with helium cores in the range of 35-65 M-circle dot 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 x 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-circle dot 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.
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