An analytical model for the plateau stage of Type II supernovae

The aim of this work is to present a semianalytical light curve model code that can be used for estimating physical properties of core collapse supernovae (SNe) in a quick and efficient way. To verify our code we fit light curves of Type II SNe and compare our best parameter estimates to those from hydrodynamical calculations. For this analysis, we use quasi-bolometric light curves of five different Type IIP SNe. In each case, we obtain appropriate results for initial pre-supernova parameters. We conclude that this semianalytical light curve model is useful to obtaining approximate physical properties of Type II SNe without using time-consuming numerical hydrodynamic simulations.

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“…Furthermore, our results show the same parameter dependence of the plateau duration as calculated by Popov (1993).…”

Section: The Effect Of Varying Input Parameterssupporting

confidence: 85%

A semianalytical light curve model and its application to type IIP supernovae

Nagy

Ordasi

Vinkó

et al. 2014

A&A

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“…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). Pastorello et al (2009) analyzed an extensive data set to estimate M 10 ZAMS » -15 M  by a semi-analytic fit of the data to the model of Zampieri et al (2003).…”

Section: Observational Samplementioning

confidence: 61%

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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“…Following the plateau luminosity relation presented by Popov (1993), L ∝ E 5/6 M −1/2 ej R 2/3 , and scaling with the radius of SN 1987A, R(87A) = 3 × 10 12 cm = 43 R (Woosley 1988), a rough estimate of the progenitor radius of SNe 2006V and 2006au can be inferred. We note that this approach has been followed by Kleiser et al (2011) for estimating the progenitor radius of SN 2000cb, although Popov (1993) developed the plateau luminosity relation for SNe whose emission was nonradioactive.…”

Section: Physical Parameters Of the Progenitorsmentioning

confidence: 67%

“…We note that this approach has been followed by Kleiser et al (2011) for estimating the progenitor radius of SN 2000cb, although Popov (1993) developed the plateau luminosity relation for SNe whose emission was nonradioactive. Such a simple scaling implies radii of 50 R for both objects, which clearly suggests a very compact progenitor for our objects.…”

Section: Physical Parameters Of the Progenitorsmentioning

confidence: 99%

The Type II supernovae 2006V and 2006au: two SN 1987A-like events

Taddia

Stritzinger

Sollerman

et al. 2012

A&A

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Context. Supernova 1987A revealed that a blue supergiant (BSG) star can end its life as a core-collapse supernova (SN). SN 1987A and other similar objects exhibit properties that distinguish them from ordinary Type II Plateau (IIP) SNe, whose progenitors are believed to be red supergiants (RSGs). Similarities among 1987A-like events include a long rise to maximum, early luminosity fainter than that of normal Type IIP SNe, and radioactivity acting as the primary source powering the light curves.

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An analytical model for the plateau stage of Type II supernovae

Cited by 247 publications

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A semianalytical light curve model and its application to type IIP supernovae

A semianalytical light curve model and its application to type IIP supernovae

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

The Type II supernovae 2006V and 2006au: two SN 1987A-like events

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