Parameters of the classical type-IIP supernova SN 1999em

Бакланов, П. В.; Блинников, С. И.; Pavlyuk, N. N.

doi:10.1134/1.1958107

Cited by 82 publications

(95 citation statements)

References 19 publications

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“…Utrobin (2007) found that both this one-group approach and the multi-group approach of Baklanov et al (2005) measured similar ejecta mass and explosion energy for SN 1999em. The basic equations and details of the input physics, including calculations of mean opacities, are described in Utrobin (2004).…”

Section: Model Overviewmentioning

confidence: 99%

“…At present, we can only state firmly that the multi-group treatment of radiation transfer cannot notably change the inferred SN parameters. This conclusion is based on the comparison between the multigroup (Baklanov et al 2005) and one-group (Utrobin 2007) approaches to the SN 1999em modeling. A major drawback of our model may be its one-dimensional approximation.…”

Section: Could Explosion Asymmetry Be a Crucial Missing Factor?mentioning

confidence: 99%

“…Our non-evolutionary pre-SN qualitatively takes this multi-dimensional effect into account, which ensures that the non-evolutionary model describes the light curve shape more successfully. A non-evolutionary pre-SN is also preferred by Baklanov et al (2005) in their modeling of SN 1999em.…”

Section: Explosion Of Evolutionary Presupernovamentioning

confidence: 99%

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High mass of the type IIP supernova 2004et inferred from hydrodynamic modeling

Utrobin

Чугай

2009

A&A

110

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Context. Previous studies of type IIP supernovae have inferred that progenitor masses recovered from hydrodynamic models are higher than 15 M . Aims. To verify the progenitor mass of this supernova category, we attempt a parameter determination of the well-observed luminous type IIP supernova 2004et. Methods. We model the bolometric light curve and the photospheric velocities of SN 2004et by means of hydrodynamic simulations in an extended parameter space. Results. From hydrodynamic simulations and observational data, we infer a presupernova radius of 1500 ± 140 R , an ejecta mass of 24.5 ± 1 M , an explosion energy of (2.3 ± 0.3) × 10 51 erg, and a radioactive 56 Ni mass of 0.068 ± 0.009 M . The estimated progenitor mass on the main sequence is in the range of 25−29 M . In addition, we find clear signatures of the explosion asymmetry in the nebular spectra of SN 2004et. Conclusions. The measured progenitor mass of SN 2004et is significantly higher than the progenitor mass suggested by the preexplosion images. We speculate that the mass inferred from hydrodynamic modeling is overestimated and crucial missing factors are multi-dimensional effects.

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Section: Model Overviewmentioning

confidence: 99%

Section: Could Explosion Asymmetry Be a Crucial Missing Factor?mentioning

confidence: 99%

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High mass of the type IIP supernova 2004et inferred from hydrodynamic modeling

Utrobin

Чугай

2009

A&A

110

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“…Synthetic LCs were numerically obtained using the onedimensional multi-group radiation hydrodynamics code STELLA (Blinnikov & Bartunov 1993;Blinnikov et al 1998;Blinnikov & Sorokina 2004;Blinnikov et al 2006;Baklanov, Blinnikov, & Pavlyuk 2005;Sorokina et al 2015). STELLA has been used to model SN LCs of various kinds, including ultra-stripped SNe (Tauris et al 2013).…”

Section: Explosive Hydrodynamics and Light Curvesmentioning

confidence: 99%

Light-curve and spectral properties of ultrastripped core-collapse supernovae leading to binary neutron stars

Moriya

Mazzali

Tominaga

et al. 2016

Mon. Not. R. Astron. Soc.

105

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We investigate light-curve and spectral properties of ultra-stripped core-collapse supernovae. Ultra-stripped supernovae are the explosions of heavily stripped massive stars which lost their envelopes via binary interactions with a compact companion star. They eject only ∼ 0.1 M ⊙ and may be the main way to form double neutronstar systems which eventually merge emitting strong gravitational waves. We follow the evolution of an ultra-stripped supernova progenitor until iron core collapse and perform explosive nucleosynthesis calculations. We then synthesize light curves and spectra of ultra-stripped supernovae using the nucleosynthesis results and present their expected properties. Ultra-stripped supernovae synthesize ∼ 0.01 M ⊙ of radioactive 56 Ni, and their typical peak luminosity is around 10 42 erg s −1 or −16 mag. Their typical rise time is 5 − 10 days. Comparing synthesized and observed spectra, we find that SN 2005ek, some of the so-called calcium-rich gap transients, and SN 2010X may be related to ultra-stripped supernovae. If these supernovae are actually ultra-stripped supernovae, their event rate is expected to be about 1 per cent of core-collapse supernovae. Comparing the double neutron-star merger rate obtained by future gravitational-wave observations and the ultra-stripped supernova rate obtained by optical transient surveys identified with our synthesized light-curve and spectral models, we will be able to judge whether ultra-stripped supernovae are actually a major contributor to the binary neutron star population and provide constraints on binary stellar evolution.

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“…This requires corrections for estimated mass loss during progenitor evolution and a compact remnant mass estimate. Since this method requires high-quality photometric and spectroscopic data, it has only been applied to a handful of events where such data are available (e.g., Zampieri et al 2003;Baklanov et al 2005;Utrobin 2007;Utrobin & Chugai 2008, 2009Pastorello et al 2009;Dall'Ora et al 2014). Typically, these models of explosions in RSGs predict significantly higher ZAMS masses than those obtained by direct imaging.…”

Section: Introductionmentioning

confidence: 99%

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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Parameters of the classical type-IIP supernova SN 1999em

Cited by 82 publications

References 19 publications

High mass of the type IIP supernova 2004et inferred from hydrodynamic modeling

High mass of the type IIP supernova 2004et inferred from hydrodynamic modeling

Light-curve and spectral properties of ultrastripped core-collapse supernovae leading to binary neutron stars

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

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