The rise-time of Type II supernovae

González–Gaitán, S.; Tominaga, Nozomu; Molina, Juan; Galbany, L.; Bufano, F.; Anderson, J. P.; Gutiérrez, C. P.; Förster, F.; Pignata, G.; Bersten, Melina C.; Howell, D. A.; Sullivan, M.; Carlberg, R. G.; Jaeger, Thomas de; Hamuy, M.; Бакланов, П. В.; Блинников, С. И.

doi:10.1093/mnras/stv1097

Cited by 135 publications

(172 citation statements)

References 130 publications

(167 reference statements)

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“…The results of Gonzalez-Gaitan et al (2015), based on comparisons with the analytical models of Nakar & Sari (2010) and hydrodynamical models of Tominaga et al (2009), are in agreement with the above, i.e., that the progenitor radii are too small when compared with the expected radii of Type II-P/L SNe. On this basis, Gonzalez-Gaitan et al (2015) conclude that temperatures of red supergiant stars are underestimated, or that mixing length prescriptions used in stellar evolution models are to blame.…”

Section: Rise Times Of Sne With Direct Progenitor Detectionssupporting

confidence: 77%

“…On this basis, Gonzalez-Gaitan et al (2015) conclude that temperatures of red supergiant stars are underestimated, or that mixing length prescriptions used in stellar evolution models are to blame. While this may indeed be the case, we emphasize that the very useful, but still simplistic framework considered both here and in Gonzalez-Gaitan et al (2015), serve mainly to indicate relevant trends, and that factors such as the explosion energy to ejecta mass ratio will strongly influence the actual rise time.…”

Section: Rise Times Of Sne With Direct Progenitor Detectionsmentioning

confidence: 99%

See 1 more Smart Citation

A comparative study of Type II-P and II-L supernova rise times as exemplified by the case of LSQ13cuw

Gáll

Polshaw

Kotak

et al. 2015

A&A

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We report on our findings based on the analysis of observations of the Type II-L supernova LSQ13cuw within the framework of currently accepted physical predictions of core-collapse supernova explosions. LSQ13cuw was discovered within a day of explosion, hitherto unprecedented for Type II-L supernovae. This motivated a comparative study of Type II-P and II-L supernovae with relatively well-constrained explosion epochs and rise times to maximum (optical) light. From our sample of twenty such events, we find evidence of a positive correlation between the duration of the rise and the peak brightness. On average, SNe II-L tend to have brighter peak magnitudes and longer rise times than SNe II-P. However, this difference is clearest only at the extreme ends of the rise time versus peak brightness relation. Using two different analytical models, we performed a parameter study to investigate the physical parameters that control the rise time behaviour. In general, the models qualitatively reproduce aspects of the observed trends. We find that the brightness of the optical peak increases for larger progenitor radii and explosion energies, and decreases for larger masses. The dependence of the rise time on mass and explosion energy is smaller than the dependence on the progenitor radius. We find no evidence that the progenitors of SNe II-L have significantly smaller radii than those of SNe II-P.

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Section: Rise Times Of Sne With Direct Progenitor Detectionssupporting

confidence: 77%

Section: Rise Times Of Sne With Direct Progenitor Detectionsmentioning

confidence: 99%

A comparative study of Type II-P and II-L supernova rise times as exemplified by the case of LSQ13cuw

Gáll

Polshaw

Kotak

et al. 2015

A&A

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“…Barbon, Ciatti & Rosino 1979), types II-P and II-L are now more commonly thought to occupy a continuum of different levels of mass loss primarily influenced by the initial mass of the progenitor (e.g. Anderson et al 2014;Sanders et al 2015;González-Gaitán et al 2015). Type IIn ('narrow lines') SNe are characterized by the presence of a dense circumstellar medium (CSM) at the time of explosion, resulting in strong interaction between the SN ejecta and the CSM (e.g.…”

Section: Introductionmentioning

confidence: 99%

Core-collapse supernova progenitor constraints using the spatial distributions of massive stars in local galaxies

Kangas

Portinari

Mattila

et al. 2017

A&A

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We study the spatial correlations between the H α emission and different types of massive stars in two local galaxies, the Large Magellanic Cloud (LMC) and Messier 33. We compare these to correlations derived for core-collapse supernovae (CCSNe) in the literature to connect CCSNe of different types with the initial masses of their progenitors and to test the validity of progenitor mass estimates which use the pixel statistics method. We obtain samples of evolved massive stars in both galaxies from catalogues with good spatial coverage and/or completeness, and combine them with coordinates of main-sequence stars in the LMC from the SIMBAD database. We calculate the spatial correlation of stars of different classes and spectral types with H α emission. We also investigate the effects of distance, noise and positional errors on the pixel statistics method. A higher correlation with H α emission is found to correspond to a shorter stellar lifespan, and we conclude that the method can be used as an indicator of the ages, and therefore initial masses, of SN progenitors. We find that the spatial distributions of type II-P SNe and red supergiants of appropriate initial mass ( 9 M ) are consistent with each other. We also find the distributions of type Ic SNe and WN stars with initial masses 20 M consistent, while supergiants with initial masses around 15 M are a better match for type IIb and II-L SNe. The type Ib distribution corresponds to the same stellar types as type II-P, which suggests an origin in interacting binaries. On the other hand, we find that luminous blue variable stars show a much stronger correlation with H α emission than do type IIn SNe.

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“…Despite the recent availability of large samples of SN II light curves (e.g., Arcavi et al 2012;Anderson et al 2014;Faran et al 2014aFaran et al , 2014bGonzález-Gaitán et al 2015;Sanders et al 2015), there is little high-quality data in the literature against which to test predictions (e.g., Nakar & Sari 2010;Rabinak & Waxman 2011, NS10, RW11) regarding early-time light curve behavior in the ultraviolet (UV) and optical bands. Rabinak & Waxman (2011) showed that it is possible to deduce the progenitor star radius (R * ) and energy per unit mass (E/M) from the early UV light curve.…”

Section: Introductionmentioning

confidence: 99%

“…Recently, Gall et al (2015) and González-Gaitán et al (2015) compared large samples of SNII light curves to RW11/NS10 shock-cooling models. Both papers compared SN rise times to rise times derived from shock-cooling models: Gall et al (2015) used r-band data, while González-Gaitán et al (2015) compared multi-band photometry.…”

Section: Introductionmentioning

confidence: 99%

Type Ii Supernova Energetics and Comparison of Light Curves to Shock-Cooling Models

Rubin

Gal‐Yam

et al. 2016

ApJ

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During the first few days after explosion, Type II supernovae (SNe) are dominated by relatively simple physics. Theoretical predictions regarding early-time SN light curves in the ultraviolet (UV) and optical bands are thus quite robust. We present, for the first time, a sample of 57 R-band SN II light curves that are well-monitored during their rise, with 5 > detections during the first 10 days after discovery, and a well-constrained time of explosion to within 1-3 days. We show that the energy per unit mass (E/M) can be deduced to roughly a factor of five by comparing early-time optical data to the 2011 model of Rabinak & Waxman, while the progenitor radius cannot be determined based on R-band data alone. We find that SN II explosion energies span a range of E/M=(0.2-20)×10 51 erg/ (10 M  ), and have a mean energy per unit mass of E M 0.85 10 51 á ñ =´erg/(10 M  ), corrected for Malmquist bias. Assuming a small spread in progenitor masses, this indicates a large intrinsic diversity in explosion energy. Moreover, E/M is positively correlated with the amount of 56 Ni produced in the explosion, as predicted by some recent models of core-collapse SNe. We further present several empirical correlations. The peak magnitude is correlated with the decline rate ( m 15 D ), the decline rate is weakly correlated with the rise time, and the rise time is not significantly correlated with the peak magnitude. Faster declining SNe are more luminous and have longer rise times. This limits the possible power sources for such events.

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The rise-time of Type II supernovae

Cited by 135 publications

References 130 publications

A comparative study of Type II-P and II-L supernova rise times as exemplified by the case of LSQ13cuw

A comparative study of Type II-P and II-L supernova rise times as exemplified by the case of LSQ13cuw

Core-collapse supernova progenitor constraints using the spatial distributions of massive stars in local galaxies

Type Ii Supernova Energetics and Comparison of Light Curves to Shock-Cooling Models

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