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

Gáll, Erwin; Polshaw, J.; Kotak, R.; Jerkstrand, A.; Leibundgut, B.; Rabinowitz, D.; Sollerman, J.; Sullivan, M.; Smartt, S. J.; Anderson, J. P.; Benetti, S.; Baltay, C.; Feindt, U.; Fraser, M.; González–Gaitán, S.; Inserra, C.; Maguire, K.; McKinnon, R.; Valenti, S.; Young, D. R.

doi:10.1051/0004-6361/201525868

Cited by 61 publications

(89 citation statements)

References 114 publications

(202 reference statements)

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“…Valenti et al (2014) suggested that slowly rising SNe IIP have higher maximum luminosities (see also Gal-Yam et al 2011). The same trend was found in Gall et al (2015). At the same time, Faran et al (2014b) and Rubin et al (2016) do not find this correlation in their samples, and only a weak correlation is found in the sample of Valenti et al (2016).…”

Section: The Rise Times Of Sne Iipsupporting

confidence: 65%

“…Being more robust and easier to measure than the power-law exponent of the bolometric light curve, the rise time can still give us important information on the progenitor characteristics. Our work is also motivated by a number of recent works considering large sets of early SNIIP light curves and focusing on their rise times (e.g., Gall et al 2015;González-Gaitán et al 2015;Rubin et al 2016). Figure 5 shows g-band light curves for a representative set of models from Figure 2 for a final energy = E 10 erg fin 51…”

Section: The Rise Times Of Sne Iipmentioning

confidence: 99%

“…In addition, based on the results of our numerical models, we derive a relation for the rise time t rise of SN IIP light curves in the g band as a function of the radius R of the progenitor. This relation may be useful in future analyses of observed early rises, especially when comparing large samples of events (e.g., Gall et al 2015;González-Gaitán et al 2015;Rubin et al 2016;Valenti et al 2016). Our results show that the observed rise times are in agreement with the observed red supergiant (RSG) radii from Levesque et al (2005Levesque et al ( , 2006, and there is no need to restrict the progenitor models to small radii   R 500 , as was suggested in some previous studies (see, e.g., Dessart et al 2013;Shussman et al 2016).…”

Section: Introductionmentioning

confidence: 99%

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Numerical Modeling of the Early Light Curves of Type Iip Supernovae

Morozova

Piro

Renzo

et al. 2016

ApJ

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The early rise of Type IIP supernovae (SN IIP) provides important information for constraining the properties of their progenitors. This can, in turn, be compared to pre-explosion imaging constraints and stellar models to develop a more complete picture of how massive stars evolve and end their lives. Using the SuperNova Explosion Code (SNEC), we model the first 40 days of SNe IIP to better understand what constraints can be derived from their early light curves. We use two sets of red supergiant (RSG) progenitor models with zero-age main sequence masses in the range between. We find that the early properties of the light curve depend most sensitively on the radius of the progenitor, and thus provide a relation between the g-band rise time and the radius at the time of explosion. This relation will be useful for deriving constraints on progenitors from future observations, especially in cases where detailed modeling of the entire rise is not practical. When comparing to observed rise times, the radii we find are a factor of a few larger than previous semi-analytic derivations and are generally in better agreement with what is found with current stellar evolution calculations as well as direct observations of RSGs.

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Section: The Rise Times Of Sne Iipsupporting

confidence: 65%

Section: The Rise Times Of Sne Iipmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Numerical Modeling of the Early Light Curves of Type Iip Supernovae

Morozova

Piro

Renzo

et al. 2016

ApJ

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“…Up to now, pre-explosion imaging has not revealed any clear distinction between the progenitors of Type IIP and Type IIL SNe neither in radius (Gall et al 2015) nor in mass ). Since our winds are optically thick, the radius we are finding R ext would act as a "pseudo-photosphere," making the progenitors much redder and potentially dimmer if dust formation occurs.…”

Section: Implications For the Stellar Progenitors Of Sne Iilmentioning

confidence: 89%

Unifying Type II Supernova Light Curves with Dense Circumstellar Material

Morozova

Piro

Valenti

2017

ApJ

178

247

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A longstanding problem in the study of supernovae (SNe) has been the relationship between the TypeIIP and TypeIIL subclasses. Whether they come from distinct progenitors or they are from similar stars with some property that smoothly transitions from one class to another has been the subject of much debate. Here,using onedimensional radiation-hydrodynamic SN models, we showthat the multi-band light curves of SNe IIL are well fit by ordinary red supergiants surrounded by dense circumstellar material (CSM). The inferred extent of this material, coupled with a typical wind velocity of 10 100 km s 1 --, suggests enhanced activity by these stars during the last months to ∼years of their lives, which may be connected with advanced stages of nuclear burning. Furthermore, we find that,even for more plateau-like SNe,dense CSM provides a better fit to the first 20 days of their light curves, indicating that the presence of such material may be more widespread than previously appreciated. Here we choose to model the CSM with a wind-like density profile, but it is unclear whether this just generally represents some other mass distribution, such as a recent mass ejection, thick disk, or even inflated envelope material. Better understanding the exact geometry and density distribution of this material will be an important question for future studies.

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“…Depending on the decline in the light curve, SNeII can be further subclassified as SNIIL for a linear decline and SNIIP for sustained brightness before an eventual decline. However, drawing distinctions between SNIILandIIP is less obvious considering an existing continuum of observed properties (Faran et al 2014;Sanders et al 2015;Chakraborti et al 2016;Gall et al 2015;Pejcha & Prieto 2015).…”

Section: Introductionmentioning

confidence: 99%

LINE IDENTIFICATIONS OF TYPE I SUPERNOVAE: ON THE DETECTION OF Si II FOR THESE HYDROGEN-POOR EVENTS

Parrent

Milisavljević

Söderberg

et al. 2016

ApJ

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Here we revisit line identifications of type I supernovae (SNe I) and highlight trace amounts of unburned hydrogen as an important free parameter for the composition of the progenitor. Most one-dimensional stripped-envelope models of supernovae indicate that observed features near 6000-6400 Å in typeI spectra are due to more than Si IIλ6355. However, while an interpretation of conspicuous Si IIλ6355 can approximate 6150 Å absorption features for all SNe Ia during the first month of free expansion, similar identifications applied to 6250 Å features of SNe Ib and Ic have not been as successful. When the corresponding synthetic spectra are compared with highquality timeseries observations, the computed spectra are frequently too blue in wavelength. Some improvement can be achieved with Fe II lines that contribute redward of 6150 Å; however, the computed spectra either remain too blue or the spectrum only reaches a fair agreement when the rise-time to peak brightness of the model conflicts with observations by a factor of two. This degree of disagreement brings into question the proposed explosion scenario. Similarly, a detection of strong Si IIλ6355 in the spectra of broadlined Ic and super-luminous events of type I/R is less convincing despite numerous model spectra used to show otherwise. Alternatively, we suggest 6000-6400 Å features are possibly influenced by either trace amounts of hydrogen or blueshifted absorption and emission in Hα, the latter being an effect which is frequently observed in the spectra of hydrogen-rich, SNe II.

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

Cited by 61 publications

References 114 publications

Numerical Modeling of the Early Light Curves of Type Iip Supernovae

Numerical Modeling of the Early Light Curves of Type Iip Supernovae

Unifying Type II Supernova Light Curves with Dense Circumstellar Material

LINE IDENTIFICATIONS OF TYPE I SUPERNOVAE: ON THE DETECTION OF Si II FOR THESE HYDROGEN-POOR EVENTS

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