On the theory of the light curves of supernovae

Grassberg, E. K.; Imshennik, V. S.; Nadyozhin, D. K.

doi:10.1007/bf00654604

Cited by 184 publications

(187 citation statements)

References 18 publications

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“…This phase is better understood theoretically (e.g., Grassberg et al 1971;Chevalier 1976Chevalier , 1992Chevalier & Fransson 2008) and has been observed in a few cases (by GALEX, Gezari et al 2008;Schawinski et al 2008;and by Swift, Soderberg et al 2008; data shown as red and black circles in Figure 1). The shockcooling phase is longer and more luminous in larger stars.…”

mentioning

confidence: 57%

The Detection Rate of Early Uv Emission From Supernovae: A Dedicated Galex/PTF Survey and Calibrated Theoretical Estimates

Ganot

Gal‐Yam

Ofek

et al. 2016

ApJ

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The radius and surface composition of an exploding massive star, as well as the explosion energy per unit mass, can be measured using early UV observations of core-collapse supernovae (SNe). We present the first results from a simultaneous GALEX/PTF search for early ultraviolet (UV) emission from SNe. Six SNe II and one Type II superluminous SN (SLSN-II) are clearly detected in the GALEX near-UV (NUV) data. We compare our detection rate with theoretical estimates based on early, shock-cooling UV light curves calculated from models that fit existing Swift and GALEX observations well, combined with volumetric SN rates. We find that our observations are in good agreement with calculated rates assuming that red supergiants (RSGs) explode with fiducial radii of 500 R e , explosion energies of 10 51 erg, and ejecta masses of 10 M e . Exploding blue supergiants and Wolf-Rayet stars are poorly constrained. We describe how such observations can be used to derive the progenitor radius, surface composition, and explosion energy per unit mass of such SN events, and we demonstrate why UV observations are critical for such measurements. We use the fiducial RSG parameters to estimate the detection rate of SNe during the shock-cooling phase (<1 day after explosion) for several ground-based surveys (PTF, ZTF, and LSST). We show that the proposed wide-field UV explorer ULTRASAT mission is expected to find >85 SNe per year (∼0.5 SN per deg 2 ), independent of host galaxy extinction, down to an NUV detection limit of 21.5 mag AB. Our pilot GALEX/PTF project thus convincingly demonstrates that a dedicated, systematic SN survey at the NUV band is a compelling method to study how massive stars end their life.

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confidence: 57%

The Detection Rate of Early Uv Emission From Supernovae: A Dedicated Galex/PTF Survey and Calibrated Theoretical Estimates

Ganot

Gal‐Yam

Ofek

et al. 2016

ApJ

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“…Radiation hydrodynamic calculations of the explosion and evolution of Type II SNe have been presented by Grassberg et al (1971), Falk & Arnett (1977), Falk (1978), Klein & Chevalier (1978), Hillebrandt & Müller (1981), and Litvinova & Nadezhin (1983, 1985, as well as more specifically for SNe II-P by Young (2004), Utrobin (2007), Utrobin & Chugai (2009), Bersten et al (2011), and Dessart & Hillier (2011), for SNe II-L by Swartz et al (1991) and Blinnikov & Bartunov (1993) and for the peculiar Type II-P SN 1987A by Blinnikov et al (2000), Dessart & Hillier (2010) and Pumo & Zampieri (2011). Here we give a summary view of the physical processes at play and the various evolutionary stages seen in these simulations.…”

Section: Appendix A: Light Curve Modelsmentioning

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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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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“…For this reason, features of the early light curves can be especially helpful in constraining progenitor properties. Emission dominated by shock cooling should reflect the radius and the density profile of the exploding star (see, e.g., Grassberg et al 1971;Falk & Arnett 1977;Soderberg et al 2008;Nakar & Sari 2010, hereafter NS10;Rabinak & Waxman 2011;Bersten et al 2013). The presence of extended material around the progenitor influences both the photometry and spectroscopy of the early SN light curve (see, e.g., Chevalier & Irwin 2011;Moriya et al 2011;Ginzburg & Balberg 2014;Nakar & Piro 2014;Svirski & Nakar 2014;Piro 2015 for the theoretical view and Ofek et al 2010;Garnavich et al 2016;Khazov et al 2016 for observational evidence).…”

Section: Introductionmentioning

confidence: 99%

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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On the theory of the light curves of supernovae

Cited by 184 publications

References 18 publications

The Detection Rate of Early Uv Emission From Supernovae: A Dedicated Galex/PTF Survey and Calibrated Theoretical Estimates

The Detection Rate of Early Uv Emission From Supernovae: A Dedicated Galex/PTF Survey and Calibrated Theoretical Estimates

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

Numerical Modeling of the Early Light Curves of Type Iip Supernovae

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