Explosion energies, nickel masses and distances of Type II plateau supernovae

Nadyozhin, D. K.

doi:10.1046/j.1365-2966.2003.07070.x

Cited by 94 publications

(86 citation statements)

References 40 publications

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“…Li et al (2006) and by Maund et al (2005) with an inferred M ZAMS of 7-9 M  and 9 2 3 -+ M  , respectively, for an 8.4 Mpc distance to M51. Takáts & Vinkó (2006) revised the distance to M51 to 7.1 Mpc, which would reduce the above progenitor mass estimates to M 9.6 5.2 ZAMS =  M  using the formula given by Nadyozhin (2003). Similar results were obtained by Tsvetkov et al (2006) from their observations of the supernova and their use of the IIP-analytical model of Popov (1993) and the simulations of Litvinova & Nadezhin (1985).…”

Section: Observational Samplesupporting

confidence: 66%

The Development of Explosions in Axisymmetric Ab Initio Core-Collapse Supernova Simulations of 12–25 Stars

Bruenn

Lentz

Hix

et al. 2016

ApJ

203

300

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We present four ab initio axisymmetric core-collapse supernova simulations initiated from 12, 15, 20, and 25 M  zero-age main sequence progenitors. All of the simulations yield explosions and havebeen evolved for at least 1.2 s after core bounce and 1 s after material first becomes unbound. These simulations were computed with our CHIMERA code employing RbR spectral neutrino transport, special and general relativistic transport effects, and state-of-the-art neutrino interactions. Continuing the evolution beyond 1 s after core bounce allows the explosions to develop more fully and the processes involved in powering the explosions to become more clearly evident. We compute explosion energy estimates, including the negative gravitational binding energy of the stellar envelope outside the expanding shock, of 0.34, 0.88, 0.38, and 0.70 Bethe (B≡10 51 erg) and increasing at 0.03, 0.15, 0.19, and 0.52 B s 1 -, respectively, for the 12, 15, 20, and 25 M  models at the endpoint of this report. We examine the growth of the explosion energy in our models through detailed analyses of the energy sources and flows. We discuss how the explosion energies may be subject to stochastic variations as exemplfied by the effect of the explosion geometry of the 20 M  model in reducing its explosion energy. We compute the proto-neutron star masses and kick velocities. We compare our results for the explosion energies and ejected Ni 56 masses against some observational standards despite the large error bars in both models and observations.

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Section: Observational Samplesupporting

confidence: 66%

The Development of Explosions in Axisymmetric Ab Initio Core-Collapse Supernova Simulations of 12–25 Stars

Bruenn

Lentz

Hix

et al. 2016

ApJ

203

300

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“…As discussed by many modellers (e.g. Woosley and Weaver 1986, Nomoto 1987, Woosley, Heger, and Weaver 2002, Eldridge and Tout 2004) the computation of evolution, and subsequent explosion, The differences between the observed characteristics of II-P SNe in particular has previously been attributed to large differences in the progenitor mass and radii (Hamuy 2003, Nadyozhin 2003, Utrobin and Chugai 2008. However the ejecta masses have not given good agreement with the direct masses of progenitor stars.…”

Section: Supernova Progenitorsmentioning

confidence: 87%

Progenitors of Core-Collapse Supernovae

Smartt

2009

Annu. Rev. Astron. Astrophys.

1,145

1,168

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Knowledge of the progenitors of core-collapse supernovae is a fundamental component in understanding the explosions. The recent progress in finding such stars is reviewed. The minimum initial mass that can produce a supernova has converged to 8 ± 1M⊙, from direct detections of red supergiant progenitors of II-P SNe and the most massive white dwarf progenitors, although this value is model dependent. It appears that most type Ibc supernovae arise from moderate mass interacting binaries. The highly energetic, broad-lined Ic supernovae are likely produced by massive, Wolf-Rayet progenitors. There is some evidence to suggest that the majority of massive stars above ∼20M⊙ may collapse quietly to black-holes and that the explosions remain undetected. The recent discovery of a class of ultra-bright type II supernovae and the direct detection of some progenitor stars bearing luminous blue variable characteristics suggests some very massive stars do produce highly energetic explosions. The physical mechanism is open to debate and these SNe pose a challenge to stellar evolutionary theory.

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“…SN 2008ax, see Pastorello et al 2008b, and references therein), but surely less than the several solar masses estimated for a normal type IIP SN (e.g. Nadyozhin 2003). Although the ejecta mass implies a moderate mass star (8−10 M ) at explosion, the initial mass is somewhat uncertain.…”

Section: Discussionmentioning

confidence: 99%

SN 1999ga: a low-luminosity linear type II supernova?

Pastorello

Crockett

Martin

et al. 2009

A&A

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Context. Type II-linear supernovae are thought to arise from progenitors that have lost most of their H envelope by the time of the explosion, and they are poorly understood because they are only occasionally discovered. It is possible that they are intrinsically rare, but selection effects due to their rapid luminosity evolution may also play an important role in limiting the number of detections. In this context, the discovery of a subluminous type II-linear event is even more interesting. Aims. We investigate the physical properties and characterise the explosion site of the type II SN 1999ga, which exploded in the nearby spiral galaxy NGC 2442. Methods. Spectroscopic and photometric observations of SN 1999ga allow us to constrain the energetics of the explosion and to estimate the mass of the ejected material, shedding light on the nature of the progenitor star in the final stages of its life. The study of the environment in the vicinity of the explosion site provides information on a possible relation between these unusual supernovae and the properties of the galaxies hosting them. Results. Despite the lack of early-time observations, we provide reasonable evidence that SN 1999ga was probably a type II-linear supernova that ejected a few solar masses of material, with a very small amount of radioactive elements of the order of 0.01 M .

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Explosion energies, nickel masses and distances of Type II plateau supernovae

Cited by 94 publications

References 40 publications

The Development of Explosions in Axisymmetric Ab Initio Core-Collapse Supernova Simulations of 12–25 Stars

The Development of Explosions in Axisymmetric Ab Initio Core-Collapse Supernova Simulations of 12–25 Stars

Progenitors of Core-Collapse Supernovae

SN 1999ga: a low-luminosity linear type II supernova?

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