2014A&A...565A..70K


Query : 2014A&A...565A..70K

2014A&A...565A..70K - Astronomy and Astrophysics, volume 565A, 70-70 (2014/5-1)

Observational properties of low-redshift pair instability supernovae.

KOZYREVA A., BLINNIKOV S., LANGER N. and YOON S.-C.

Abstract (from CDS):

So-called superluminous supernovae have been recently discovered in the local Universe. It appears possible that some of them originate in stellar explosions induced by the pair instability mechanism. Recent stellar evolution models also predict pair instability supernovae from very massive stars at fairly high metallicities (i.e., Z∼0.004). We provide supernova models and synthetic light curves for two progenitor models, a 150M red supergiant and a 250M yellow supergiant at a metallicity of Z=0.001, for which the evolution from the main sequence to collapse and the initiation of the pair instability supernova itself has been previously computed in a realistic and self-consistent way. We use the radiation hydrodynamics code STELLA to describe the supernova evolution of both models in a time frame of about 500 days. We describe the shock-breakout phases of both supernovae, which are characterized by higher luminosity, longer duration, and a lower effective temperature than those of ordinary Type IIP supernovae. We derive the bolometric, as well as the U, B, V, R, and I, light curves of our pair instability supernova models, which show a long-lasting plateau phase with maxima at Mbol≃-19.3mag and -21.3mag for our lower and higher mass models, respectively. While we do not produce synthetic spectra, we also describe the photospheric composition and velocity as a function of time. We conclude that the light curve of the explosion of our initially 150M star resembles those of relatively bright type IIP supernovae, whereas its photospheric velocity at early times is somewhat lower. Its 56Ni mass of 0.04M also falls well into the range found in ordinary core collapse supernovae. The light curve and photospheric velocity of our 250M models has a striking resemblance to that of the superluminous SN 2007bi, strengthening its interpretation as pair instability supernova. We conclude that pair instability supernovae may occur more frequently in the local universe than previously assumed.

Abstract Copyright:

Journal keyword(s): stars: massive - stars: Population II - supernovae: general - radiative transfer - hydrodynamics

Simbad objects: 14

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Number of rows : 14
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 SN 1992am SN* 01 25 02.76 -04 39 00.9   18.5 18.5     SNIIP 55 1
2 PS1-10bzj SN* 03 31 39.826 -27 47 42.17           SNIc 51 0
3 SN 1999em SN* 04 41 27.04 -02 51 45.2   13.79 13.7     SNIIP 648 1
4 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 16522 1
5 SN 1987A SN* 05 35 28.020 -69 16 11.07           SNIIpec 4783 2
6 SN 2010gx SN* 11 25 46.71 -08 49 41.4           SNIc 151 1
7 SN 2007bi SN* 13 19 20.19 +08 55 44.3       18.3   SNIcpec 206 1
8 SN 1992H SN* 13 56 22.26 +47 14 27.4     15.0     SNII 104 1
9 PTF 10nmn SN* 15 50 02.809 -07 24 42.38           SLSN-I 27 0
10 PTF 09cnd SN* 16 12 08.94 +51 29 16.1           SLSNIc 108 0
11 SN 2009kf SN* 16 12 54.00 +55 38 13.8           SNIIP 46 1
12 PS1-10ky SN* 22 13 37.851 +01 14 23.57           SNIc 45 0
13 [CSG2012] SN J2213-1745 SN* 22 13 39.9700 -17 45 24.486           SLSN-I 22 0
14 PS1-10awh SN* 22 14 29.831 -00 04 03.62           SNIc 44 0

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2023.02.02-19:59:47

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