- and Oxygen-Burning Stars and Pre-Supernova Models

Rakavy, G.; Shaviv, G.; Zinamon, Z.

doi:10.1086/149318

Cited by 116 publications

(59 citation statements)

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“…The large 16 O mass fraction, coupled with 16 O+ 16 O being a true fusion reaction and not a photodisintegration driven event like Ne-burning or Si-burning, ensures that O-burning is a key energetic and nucleosynthesis stage in the late phases of massive star evolution (Rakavy et al 1967;Arnett 1972b;Woosley et al 1972;El Eid et al 2004;Sukhbold et al 2016).…”

Section: O-burningmentioning

confidence: 99%

On Variations of Pre-Supernova Model Properties

Farmer¹,

Fields²,

Petermann³

et al. 2016

ApJS

132

166

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We explore the variation in single star 15-30 M , non-rotating, solar metallicity, pre-supernova MESA models due to changes in the number of isotopes in a fully-coupled nuclear reaction network and adjustments in the mass resolution. Within this two-dimensional plane we quantitatively detail the range of core masses at various stages of evolution, mass locations of the main nuclear burning shells, electron fraction profiles, mass fraction profiles, burning lifetimes, stellar lifetimes, and compactness parameter at core-collapse for models with and without mass loss. Up to carbon burning we generally find mass resolution has a larger impact on the variations than the number of isotopes, while the number of isotopes plays a more significant role in determining the span of the variations for neon, oxygen and silicon burning. Choice of mass resolution dominates the variations in the structure of the intermediate convection zone and secondary convection zone during core and shell hydrogen burning respectively, where we find a minimum mass resolution of ≈0.01 M is necessary to achieve convergence in the helium core mass at the ≈5% level. On the other hand, at the onset of core-collapse we find ≈30% variations in the central electron fraction and mass locations of the main nuclear burning shells, a minimum of ≈127 isotopes is needed to attain convergence of these values at the ≈10% level.

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Section: O-burningmentioning

confidence: 99%

On Variations of Pre-Supernova Model Properties

Farmer¹,

Fields²,

Petermann³

et al. 2016

ApJS

132

166

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“…The combination of the remarkable luminosity, the broad peak and large amount of 56 Ni synthesised in the explosion could be explained with the model of a pair-instability supernova (Barkat et al 1967;Rakavy et al 1967;Bond et al 1984). These events are thought to occur when the temperature in the core of a very massive stars exceeds temperatures of ∼10 9 K allowing electron-positron pair production to occur.…”

Section: Sn 2007bi: Pair-instability or Massive Core Collapse?mentioning

confidence: 99%

Two type Ic supernovae in low-metallicity, dwarf galaxies: diversity of explosions

Young¹,

Smartt²,

Valenti³

et al. 2010

A&A

137

132

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Aims. The aim of this paper is to discuss the nature of two type Ic supernovae SN 2007bg and SN 2007bi and their host galaxies. Both supernovae were discovered in wide-field, non-targeted surveys and are found to be associated with sub-luminous blue dwarf galaxies identified in SDSS images. Methods. We present BVRI photometry and optical spectroscopy of SN 2007bg and SN 2007bi and their host galaxies. Their lightcurves and spectra are compared to those of other type Ic SNe and analysis of these data provides estimates of the energetics, total ejected masses and synthesised mass of 56 Ni. Detection of the host galaxy emission lines allows for metallicity measurements. Results. Neither SNe 2007bg nor 2007bi were found in association with an observed GRB, but from estimates of the metallicities of their host-galaxies they are found to inhabit similar low-metallicity environments as GRB associated supernovae. The radio-bright SN 2007bg is hosted by an extremely sub-luminous galaxy of magnitude M B = −12.4 ± 0.6 mag and an estimated oxygen abundance of 12 + log(O/H) = 8.18 ± 0.17 (on the Pettini & Pagel 2004 scale). The early lightcurve evolution of SN 2007bg matches the fastpace decline of SN 1994I giving it one of the fastest post-maximum decline rates of all broad-lined type Ic supernovae known to date and, when combined with its high expansion velocities, a high kinetic energy to ejected mass ratio (E K /M ej ∼ 2.7). We also show that SN 2007bi is possibly the most luminous type Ic known, reaching a peak magnitude of M R ∼ −21.3 mag and displays a remarkably slow decline, following the radioactive decay rate of 56 Co to 56 Fe throughout the course of its observed lifetime. SN 2007bi also displays an extreme longevity in its spectral evolution and is still not fully nebular at approximately one year post-maximum brightness. From a simple model of the bolometric light curve of SN 2007bi we estimate a total ejected 56 Ni mass of M Ni = 3.5−4.5 M , the largest 56 Ni mass measured in the ejecta of a supernova to date. There are two models that could explain the high luminosity and large ejected 56 Ni mass. One is a pair-instability supernova (PISN) which has been predicted to occur for massive stars at low metallicities. We measure the host galaxy metallicity of SN 2007bi to be 12 + log(O/H) = 8.15 ± 0.15 (on the McGaugh 1991 scale) which is somewhat high to be consistent with the PISN model. An alternative is the core-collapse of a C+O star of 20−40 M which is the core of a star of originally 50−100 M .

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“…Their emission lines likely originate from relatively abundant circumstellar material (CSM) around the SN progenitor star (e.g., Chevalier & Fransson 1994;Chugai & Danziger 1994;Chugai et al 2003;Ofek et al 2007Ofek et al , 2010Ofek et al , 2014bSmith et al 2008Smith et al , 2009), ejected only a short time (on the order of months to decades) prior to the SN explosion (Dessart et al 2009;Gal-Yam & Leonard 2009;Ofek et al 2010Ofek et al , 2013b. Several theoretical mechanisms have been suggested to explain this high mass loss in the final stages of stellar evolution (e.g., Rakavy et al 1967;Woosley et al 2007;Yoon & Cantiello 2010;Arnett & Meakin 2011;Chevalier 2012;Quataert & Shiode 2012;Shiode & Quataert 2014;Soker & Kashi 2013).…”

Section: Introductionmentioning

confidence: 99%

PRECURSORS PRIOR TO TYPE IIn SUPERNOVA EXPLOSIONS ARE COMMON: PRECURSOR RATES, PROPERTIES, AND CORRELATIONS

Ofek

Sullivan

Shaviv

et al. 2014

ApJ

239

264

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There is a growing number of Type IIn supernovae (SNe) which present an outburst prior to their presumably final explosion. These precursors may affect the SN display, and are likely related to poorly charted phenomena in the final stages of stellar evolution. By coadding Palomar Transient Factory (PTF) images taken prior to the explosion, here we present a search for precursors in a sample of 16 Type IIn SNe. We find five SNe IIn that likely have at least one possible precursor event (PTF 10bjb, SN 2010mc, PTF 10weh, SN 2011ht, and PTF 12cxj), three of which are reported here for the first time. For each SN we calculate the control time. We find that precursor events among SNe IIn are common: at the one-sided 99% confidence level, >50% of SNe IIn have at least one pre-explosion outburst that is brighter than 3 × 10 7 L taking place up to 1/3 yr prior to the SN explosion. The average rate of such precursor events during the year prior to the SN explosion is likely 1 yr −1 , and fainter precursors are possibly even more common. Ignoring the two weakest precursors in our sample, the precursors rate we find is still on the order of one per year. We also find possible correlations between the integrated luminosity of the precursor and the SN total radiated energy, peak luminosity, and rise time. These correlations are expected if the precursors are mass-ejection events, and the early-time light curve of these SNe is powered by interaction of the SN shock and ejecta with optically thick circumstellar material.

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- and Oxygen-Burning Stars and Pre-Supernova Models

Cited by 116 publications

References 0 publications

On Variations of Pre-Supernova Model Properties

On Variations of Pre-Supernova Model Properties

Two type Ic supernovae in low-metallicity, dwarf galaxies: diversity of explosions

PRECURSORS PRIOR TO TYPE IIn SUPERNOVA EXPLOSIONS ARE COMMON: PRECURSOR RATES, PROPERTIES, AND CORRELATIONS

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