Observations and analysis of two type IIP supernovae: the intrinsically faint object SN 2005cs and the ambiguous object SN 2005ay

Tsvetkov, D. Yu.; Volnova, A.; Shulga, A. P.; Korotkiy, S.; Elmhamdi, A.; Danziger, I. J.; Ereshko, M. V.

doi:10.1051/0004-6361:20065704

Cited by 53 publications

(61 citation statements)

References 27 publications

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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: 58%

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 Samplementioning

confidence: 58%

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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“…In this regard it would be of top priority to determine independently the progenitor mass both from the pre-discovery images and from the hydrodynamic simulations. Among SNe IIP, except for SN 1987A, only SN 2004et and SN 2005cs were detected in the pre-discovery images (Li et al 2005;Li et al 2006) and have the light curves and spectra appropriate for the hydrodynamic modeling as well (Sahu et al 2006;Misra et al 2007;Pastorello et al 2006;Tsvetkov et al 2006). These two challenging cases require a detailed study.…”

Section: Discussionmentioning

confidence: 99%

Ejecta and progenitor of the low-luminosity type IIP supernova 2003Z

Utrobin

Чугай

Pastorello

2007

A&A

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Context. The origin of low-luminosity type IIP supernovae is unclear: they have been proposed to originate either from massive (∼25 M ) or low-mass (∼9 M ) stars. Aims. We wish to determine parameters of the low-luminosity type IIP supernova 2003Z, to estimate a mass-loss rate of the presupernova, and to recover a progenitor mass. Methods. We compute the hydrodynamic models of the supernova to describe the light curves and the observed expansion velocities. The wind density of the presupernova is estimated using a thin shell model for the interaction with circumstellar matter. Results. We estimate an ejecta mass of 14.0 ± 1.2 M , an explosion energy of (2.45 ± 0.18) × 10 50 erg, a presupernova radius of 229 ± 39 R , and a radioactive 56 Ni amount of 0.0063 ± 0.0006 M . The upper limit of the wind density parameter in the presupernova vicinity is 10 13 g cm −1 , and the mass lost at the red/yellow supergiant stage is ≤0.6 M assuming the constant mass-loss rate. The estimated progenitor mass is in the range of 14.4-17.4 M . The presupernova of SN 2003Z was probably a yellow supergiant at the time of the explosion. Conclusions. The progenitor mass of SN 2003Z is lower than those of SN 1987A and SN 1999em, normal type IIP supernovae, but higher than the lower limit of stars undergoing a core collapse. We propose an observational test based on the circumstellar interaction to discriminate between the massive (∼25 M ) and moderate-mass (∼16 M ) scenarios.

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“…This event was more than a magnitude fainter than an average Type IIP supernova. Nevertheless, the light curve of SN 2005cs was observed in UBVRI bands and its physical properties were calculated by Tsvetkov et al (2006) based on the hydrodynamic model of Litvinova & Nadyozhin (1985). SN 2005cs was also fitted using our code and the results can be found in Table 3.…”

Section: Sn 2005csmentioning

confidence: 99%

“…SN 2005cs was also fitted using our code and the results can be found in Table 3. For better comparison, we used d = 8.4 Mpc for the distance of M51, Tsvetkov et al (2006). Takáts et al (2014). which was adopted by Tsvetkov et al (2006).…”

Section: Sn 2005csmentioning

confidence: 99%

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

Nagy

Ordasi

Vinkó

et al. 2014

A&A

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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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Observations and analysis of two type IIP supernovae: the intrinsically faint object SN 2005cs and the ambiguous object SN 2005ay

Cited by 53 publications

References 27 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

Ejecta and progenitor of the low-luminosity type IIP supernova 2003Z

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

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