Two-dimensional simulations of pulsational pair-instability supernovae
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...
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| Main Authors: | , , , , |
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| Format: | Article (Journal) |
| Language: | English |
| Published: |
[2014 September 1]
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| In: |
The astrophysical journal
Year: 2014, Volume: 792, Issue: 1 |
| ISSN: | 1538-4357 |
| DOI: | 10.1088/0004-637X/792/1/28 |
| Online Access: | Verlag, lizenzpflichtig, Volltext: https://doi.org/10.1088/0004-637X/792/1/28
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| Author Notes: | Ke-Jung Chen, Stan Woosley, Alexander Heger, Ann Almgren, and Daniel J. Whalen |
| Summary: | 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. |
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| Item Description: | Gesehen am 16.09.2020 |
| Physical Description: | Online Resource |
| ISSN: | 1538-4357 |
| DOI: | 10.1088/0004-637X/792/1/28 |