Progenitors of low-luminosity Type II-Plateau supernovae
Author
dc.contributor.author
Lisakov, Sergey M.
Author
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Dessart, Luc
Author
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Hillier, D. John
Author
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Waldman, Roni
Author
dc.contributor.author
Livne, Eli
Admission date
dc.date.accessioned
2018-07-27T19:40:42Z
Available date
dc.date.available
2018-07-27T19:40:42Z
Publication date
dc.date.issued
2018
Cita de ítem
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Monthly notices of the Royal Astronomical Society Volumen: 473 Número: 3 Páginas: 3863-3881
es_ES
Identifier
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10.1093/mnras/stx2521
Identifier
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https://repositorio.uchile.cl/handle/2250/150398
Abstract
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The progenitors of low-luminosity Type II-Plateau supernovae (SNe II-P) are believed to be red supergiant (RSG) stars, but there is much disparity in the literature concerning their mass at core collapse and therefore on the main sequence. Here, we model the SN radiation arising from the low-energy explosion of RSG stars of 12, 25 and 27M(circle dot) on the main sequence and formed through single star evolution. Despite the narrow range in ejecta kinetic energy (2.5-4.2 x 10(50) erg) in our model set, the SN observables from our three models are significantly distinct, reflecting the differences in progenitor structure (e.g. surface radius, H-rich envelope mass and He-core mass). Our higher mass RSG stars give rise to Type II SNe that tend to have bluer colours at early times, a shorter photospheric phase, and a faster declining V-band light curve (LC) more typical of Type II-linear SNe, in conflict with the LC plateau observed for low-luminosity SNe II. The complete fallback of the CO core in the low-energy explosions of our high-mass RSG stars prevents the ejection of any Ni-56 (nor any core O or Si), in contrast to low-luminosity SNe II-P, which eject at least 0.001M(circle dot) of Ni-56. In contrast to observations, Type II SN models from higher mass RSGs tend to show an H alpha absorption that remains broad at late times (due to a larger velocity at the base of the H-rich envelope). In agreement with the analyses of pre-explosion photometry, we conclude that low-luminosity SNe II-P likely arise from low-mass rather than high-mass RSG stars.
es_ES
Patrocinador
dc.description.sponsorship
Erasmus Mundus Joint Doctorate Program from the agency EACEA of the European Commission
2013-1471
STScI
HST-AR-12640.01
NASA
NNX14AB41G