Bursting SN 1996cr's bubble: hydrodynamic and X-ray modelling of its circumstellar medium

Dwarkadas, Vikram V.; Dewey, Daniel; Bauer, F. E.

doi:10.1111/j.1365-2966.2010.16966.x

Cited by 56 publications

(97 citation statements)

References 77 publications

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“…Examples include the type-IIn SNe 1996cr (Dwarkadas et al 2010;Dewey et al 2011), 2006jd (Chandra et al 2012, and SN 2009ip (Margutti et al 2014a). In all cases, the excess has been interpreted as originating from H-and He-like transitions of collisionally ionized Fe atoms.…”

Section: Clumpy Structure Of the Csmmentioning

confidence: 99%

Ejection of the Massive Hydrogen-rich Envelope Timed with the Collapse of the Stripped SN 2014C

Margutti

Kamble

Milisavljevic

et al. 2017

ApJ

171

269

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We present multi-wavelength observations of SN 2014C during the first 500 days. These observations represent the first solid detection of a young extragalactic stripped-envelope SN out to high-energy X-rays ∼40 keV. SN 2014C shows ordinary explosion parameters (E k ∼1.8×10 51 erg and M ej ∼1.7 M e ). However, over an ∼1 year timescale, SN 2014C evolved from an ordinary hydrogen-poor supernova into a strongly interacting, hydrogen-rich supernova, violating the traditional classification scheme of type-I versus type-II SNe. Signatures of the SN shock interaction with a dense medium are observed across the spectrum, from radio to hard X-rays, and revealed the presence of a massive shell of ∼1 M e of hydrogen-rich material at ∼6×10 16 cm. The shell was ejected by the progenitor star in the decades to centuries before collapse. This result challenges current theories of massive star evolution, as it requires a physical mechanism responsible for the ejection of the deepest hydrogen layer of H-poor SN progenitors synchronized with the onset of stellar collapse. Theoretical investigations point at binary interactions and/or instabilities during the last nuclear burning stages as potential triggers of the highly time-dependent mass loss. We constrain these scenarios utilizing the sample of 183 SNe Ib/c with public radio observations. Our analysis identifies SN 2014C-like signatures in ∼10% of SNe. This fraction is reasonably consistent with the expectation from the theory of recent envelope ejection due to binary evolution if the ejected material can survive in the close environment for 10 3 -10 4 years. Alternatively, nuclear burning instabilities extending to core C-burning might play a critical role.

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Section: Clumpy Structure Of the Csmmentioning

confidence: 99%

Ejection of the Massive Hydrogen-rich Envelope Timed with the Collapse of the Stripped SN 2014C

Margutti

Kamble

Milisavljevic

et al. 2017

ApJ

171

269

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“…The time t shj is stored in an additional passive tracer added to the model equations. To estimate the deviations from equilibrium of ionization of the most abundant ions, we adopted the approach suggested by Dwarkadas et al (2010). In fact, this approach ensures high efficiency in the calculation (expecially in the case of 3D simulations as in our case) as well as a reasonable accuracy in the evaluation of the nonequilibrium of ionization effects.…”

Section: Modeling the Evolution Of The Snrmentioning

confidence: 99%

Modeling SNR Cassiopeia a From the Supernova Explosion to Its Current Age: The Role of Post-Explosion Anisotropies of Ejecta

Orlando

Miceli

Pumo

et al. 2016

ApJ

115

138

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The remnants of core-collapse supernovae (SNe) have complex morphologies that may reflect asymmetries and structures developed during the progenitor SN explosion. Here we investigate how the morphology of the supernova remnant Cassiopeia A (Cas A) reflects the characteristics of the progenitor SN with the aim of deriving the energies and masses of the post-explosion anisotropies responsible for the observed spatial distribution of Fe and Si/S. We model the evolution of Cas A from the immediate aftermath of the progenitor SN to the three-dimensional interaction of the remnant with the surrounding medium. The post-explosion structure of the ejecta is described by small-scale clumping of material and larger-scale anisotropies. The hydrodynamic multi-species simulations consider an appropriate post-explosion isotopic composition of the ejecta. The observed average expansion rate and shock velocities can be well reproduced by models with ejecta mass M ej ≈4M e and explosion energy E SN ≈2.3×10 51 erg. The post-explosion anisotropies (pistons) reproduce the observed distributions of Fe and Si/ S if they had a total mass of ≈0.25 M e and a total kinetic energy of ≈1.5×10 50 erg. The pistons produce a spatial inversion of ejecta layers at the epoch of Cas A, leading to the Si/S-rich ejecta physically interior to the Fe-rich ejecta. The pistons are also responsible for the development of the bright rings of Si/S-rich material which form at the intersection between the reverse shock and the material accumulated around the pistons during their propagation. Our result supports the idea that the bulk of asymmetries observed in Cas A are intrinsic to the explosion.

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“…For example SN 1996cr 8 was missed at a distance of 3.8 Mpc (Bauer et al 2008;Dwarkadas et al 2010).…”

Section: Control Timementioning

confidence: 99%

A comparison between star formation rate diagnostics and rate of core collapse supernovae within 11 Mpc

Botticella

Smartt

Kennicutt

et al. 2012

A&A

123

135

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Aims. The core collapse supernova rate provides a strong lower limit for the star formation rate (SFR). Progress in using it as a cosmic SFR tracer requires some confidence that it is consistent with more conventional SFR diagnostics in the nearby Universe. This paper compares standard SFR measurements based on Hα, far ultraviolet (FUV) and total infrared (TIR) galaxy luminosities with the observed core collapse supernova rate in the same galaxy sample. The comparison can be viewed from two perspectives. Firstly, by adopting an estimate of the minimum stellar mass to produce a core collapse supernova one can determine a SFR from supernova numbers. Secondly, the radiative SFR can be assumed to be robust and then the supernova statistics provide a constrain on the minimum stellar mass for core collapse supernova progenitors. Methods. The novel aspect of this study is that Hα, FUV and TIR luminosities are now available for a complete galaxy sample within the local 11 Mpc volume and the number of discovered supernovae in this sample within the last 13 years is high enough to perform a meaningful statistical comparison. We exploit the multi-wavelength dataset from 11 HUGS, a volume-limited survey designed to provide a census of SFR in the Local Volume. There are 14 supernovae discovered in this sample of galaxies within the last 13 years. Although one could argue that this may not be complete, it is certainly a robust lower limit. Results. Assuming a lower limit for core collapse of 8 M (as proposed by direct detections of SN progenitor stars and white dwarf progenitors), the core-collapse supernova rate matches the SFR from the FUV luminosity. However, the SFR based on Hα luminosity is lower than these two estimates by a factor of nearly 2. If we assume that the FUV or Hα based luminosities are a true reflection of the SFR, we find that the minimum mass for core collapse supernova progenitors is 8 ± 1 M and 6 ± 1 M , respectively. Conclusions. The estimate of the minimum mass for core collapse supernova progenitors obtained exploiting FUV data is in good agreement with that from the direct detection of supernova progenitors. The concordant results by these independent methods point toward a constraint of 8 ± 1 M on the lower mass limit for progenitor stars of core collapse supernovae.

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Bursting SN 1996cr's bubble: hydrodynamic and X-ray modelling of its circumstellar medium

Cited by 56 publications

References 77 publications

Ejection of the Massive Hydrogen-rich Envelope Timed with the Collapse of the Stripped SN 2014C

Ejection of the Massive Hydrogen-rich Envelope Timed with the Collapse of the Stripped SN 2014C

Modeling SNR Cassiopeia a From the Supernova Explosion to Its Current Age: The Role of Post-Explosion Anisotropies of Ejecta

A comparison between star formation rate diagnostics and rate of core collapse supernovae within 11 Mpc

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