Progenitor mass of the type IIP supernova 2005cs

Utrobin, V. P.; Чугай, Н. Н.

doi:10.1051/0004-6361:200810272

Cited by 92 publications

(158 citation statements)

References 34 publications

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“…7a) and the total 56 Ni mass versus the progenitor mass (Fig. 7b) strengthens the correlations recovered earlier for the SNe IIP studied hydrodynamically (Utrobin & Chugai 2008). We note that these correlations also infer the correlation between the explosion energy and the total 56 Ni mass, which was found and discussed earlier by Nadyozhin (2003).…”

Section: Progenitor Masssupporting

confidence: 90%

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

Utrobin

Чугай

2009

A&A

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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: Progenitor Masssupporting

confidence: 90%

“…We adopt the pre-SN model with an envelope mass of 15.9 M and a density distribution that closely resembles that of the evolutionary model (Utrobin & Chugai 2008). The hydrogen and helium are assumed to be mixed along the mass coordinate in a similar way to the optimal model (Fig.…”

Section: Explosion Of Evolutionary Presupernovamentioning

confidence: 99%

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

Utrobin

Чугай

2009

A&A

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110

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“…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). Finally, Utrobin & Chugai (2008), with radiation-hydrodynamics modeling, obtain a larger M ZAMS of 17.2-19.2 M  . Interestingly, if this latter estimate is correct there would be a strong implication that sub-luminous SNe II arise from two distinct progenitor populations, a low-mass (∼7-10 M  ) population and a relatively high-mass (20 M  ) population.…”

Section: Observational Samplementioning

confidence: 99%

“…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

205

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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“…SN 2005cs seems to belong to the subtype of low-luminosity, 56 Ni-poor, low-velocity SNe II-P, as shown also by long-term studies of Tsvetkov et al (2006;optical photometry), Gnedin et al (2007; R-band photometry and polarimetry), and Pastorello et al (2009;optical and near-IR photometry, optical spectroscopy). Extensive studies of the first-year data and pre-explosion images resulted in a progenitor mass of 7−13 M (Maund et al 2005;Li et al 2006;Takáts & Vinkó 2006;Eldridge et al 2007), while Utrobin & Chugai (2008) determined a significantly higher value (17−19 M ). In their more recent work Pastorello et al (2009) concluded that the progenitor mass should be in the range of 10−15 M .…”

Section: Supernova Sample Observed By Spitzermentioning

confidence: 99%

Twelve type II-P supernovae seen with the eyes ofSpitzer

Szalai

Vinkó

2012

A&A

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Context. Core-collapse supernovae (CC SNe), especially those of type II-plateau (II-P), are thought to be important contributors to cosmic dust production. The most obvious indicator of newly-formed and/or pre-existing dust is the time-dependent mid-infrared (MIR) excess coming from the environment of SNe. In the past few years several CC SNe were monitored by the Spitzer Space Telescope in the nebular phase, hundreds of days after explosion. On the other hand, only a few of these objects have been analyzed and published to date. Aims. Our goal was to collect publicly available, previously unpublished measurements on type II-P (or peculiar IIP) SNe from the Spitzer database. The most important aspect was to find SNe observed with the Infrared Array Camera (IRAC) on at least two epochs. The temporal changes of the observed fluxes may be indicative of the underlying supernova, while spectral energy distribution (SED) fitting to the fluxes in different IRAC channels may reveal the physical parameters of the mid-IR radiation, which is presumably caused by warm dust. Methods. The IRS spectra were extracted and calibrated with SPICE, while photometric SEDs were assembled using IRAF and MOPEX. Calculated SEDs from observed fluxes were fit with simple dust models to obtain basic information on the dust presumed as the source of MIR radiation. Results. We found twelve SNe that satisfied the criterion above, observed at late-time epochs (typically after +300 days). In three cases we could not identify any point source at the SN position on late-time IRAC images. We found two SNe, 2005ad and 2005af, which likely have newly formed dust in their environment, while in the other seven cases the observed MIR flux may originate from pre-existing circumstellar or interstellar dust. Our results support the previous observational conclusions that warm new dust in the environment of SNe contributes only marginally to the cosmic dust content.

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Progenitor mass of the type IIP supernova 2005cs

Cited by 92 publications

References 34 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

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

Twelve type II-P supernovae seen with the eyes ofSpitzer

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