Observed and Physical Properties of Core-Collapse Supernovae

By M. Hamuy. 2002

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I use photometry and spectroscopy data for 24 Type II plateau supernovae (SNe IIP) to examine their observed and physical properties. This data set shows that these objects encompass a wide range of ~5 mag in their plateau luminosities, their expansion velocities vary by a factor of 5, and the nickel masses produced in these explosions go from 0.0016 to 0.26 M☉. From a subset of 16 objects I find that the explosion energies vary between 0.6 × 1051 and 5.5 × 1051 ergs, the ejected masses encompass the range 14-56 M☉, and the progenitors' radii go from 80 to 600 R☉. Despite this great diversity, several regularities emerge, which reveal that there is a continuum in the properties of these objects from the faint, low-energy, nickel-poor SNe 1997D and 1999br, to the bright, high-energy, nickel-rich SN 1992am. This study provides evidence that more massive progenitors produce more energetic explosions, thus suggesting that the outcome of the core collapse is somewhat determined by the envelope mass. I also find that SNe with greater energies produce more nickel. Similar relationships appear to hold for SNe Ib/c, which suggests that both SNe II and SNe Ib/c share the same core physics. When the whole sample of core-collapse objects is considered, there is a continuous distribution of energies below 8 × 1051 ergs. Far above in energy scale and nickel production lies the extreme hypernova 1998bw, the only SN firmly associated with a gamma-ray burst.

Subfields: Astronomy and Astrophysics, Molecular Biology, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/456c990bbf6811da690425e463d653409b4eb400

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Citations in the corpus

TOWARD CHARACTERIZATION OF THE TYPE IIP SUPERNOVA PROGENITOR POPULATION: A STATISTICAL SAMPLE OF LIGHT CURVES FROM Pan-STARRS1 (2014, methodology): “Several authors have argued for a single parameter source of variation among SNe IIP light curves (Hamuy 2003; Poznanski 2013), particularly with respect to the luminosity– velocity relation applied in the standardizable candle method (Hamuy & Pinto 2002; Olivares 2008; D’Andrea et al. 2010).”
THE DEVELOPMENT OF EXPLOSIONS IN AXISYMMETRIC AB INITIO CORE-COLLAPSE SUPERNOVA SIMULATIONS OF 12–25 M ⊙ ?> STARS (2012, methodology): “Hamuy (2003) applied the fitting formulae of Litvinova & Nadezhin (1983, 1985) to a sample of 13 SNe IIP that had sufficient data for the needed observational parameters to be derived.”
Young Core-Collapse Supernova Remnants and Their Supernovae (2004, background): “Results for seven SNe Ib and Ic indicate MNi ¼ 0:07–0.15 M except for the highly energetic SN1998bw withMNi 0:5 M (summarized by Hamuy 2003).”
A double stellar generation in the globular cluster NGC 6656 (M 22): Two stellar groups with different iron and s-process element abundances (2009, background): “Each CCSN on average produces ∼0.07 M of iron (Hamuy 2003), therefore about twenty SNe are needed to produce the fresh iron in the second stellar population.”
Hot Gas In and Around Elliptical Galaxies (2003, methodology): “Yields from Type II supernovae yII (expressed in M⊙) vary with initial main sequence stellar mass (e.g. Hamuy 2003) and must be averaged over the initial mass function.”
Bolometric light curves and explosion parameters of 38 stripped-envelope core-collapse supernovae (2014, methodology): “Hamuy (2003) show a correlation of increasing EK with MNi for SNe IIP and to a weaker extent this is also found for SE SNe.”
Non-spherical core collapse supernovae. I. Neutrino-driven convection, Rayleigh-Taylor instabilities, and the formation and propagation of metal clumps (2003, background): “Photospheric velocities, as those published recently by Hamuy (2003), are not very helpful in this respect because they only probe the outer, faster expanding layers of the ejecta.”
Optical and near infrared coverage of SN 2004et: physical parameters and comparison with other type IIP supernovae (2009, methodology): “If these estimates of progenitor masses are accurate, it means long plateau phases are produced by ejected envelope masses as low as 6–7 M⊙, which are in some cases much lower values than those calculated from light curve modelling (Hamuy 2003; Nadëzhin 2003).”
Measuring the Progenitor Masses and Dense Circumstellar Material of Type II Supernovae (2017, background): “This general correlation was to be expected, since recent studies confirm that SNeIIL have somewhat higher explosion energies per unit ejecta mass than SNeIIP (see, e.g., Faran et al. 2014a; Gall et al. 2015) and the steeper decline of SNeIIL is due to a larger amount of dense CSM (Morozova et al. 2”
Origin of multiple stellar populations in globular clusters and their helium enrichment (2008, positive): “On average, each CCSN produces ∼0.07 M of iron (Hamuy 2003), roughly 10 times less than each SNIa.”
THE LANDSCAPE OF THE NEUTRINO MECHANISM OF CORE-COLLAPSE SUPERNOVAE: NEUTRON STAR AND BLACK HOLE MASS FUNCTIONS, EXPLOSION ENERGIES, AND NICKEL YIELDS (2014, methodology): “In the left panel of Figure 23, we show theoretical results from our work and Ugliano et al. (2012) with observations of explosion energies and nickel masses from Hamuy (2003).”
SUPER-LUMINOUS TYPE Ic SUPERNOVAE: CATCHING A MAGNETAR BY THE TAIL (2013, methodology): “The 56Ni masses can thus be estimated using the formula M(56Ni)SN = 7.87× 10 −44Lte [ (t−t0)/(1+z)−6.10 111.26 ] M⊙, (1) (e.g. as employed by Hamuy 2003), where t0 is the explosion epoch, 6.1 d is the half-life of 56Ni and 111.26 d is the e-folding time of the 56Co decay, which release 1.71 MeV and…”
SN 2008S: An electron-capture SN from a super-AGB progenitor? (2009, methodology): “We estimated the56Ni mass also using the method of Hamuy (2003) assuming that all theγ−rays resulting from the decay of56Co into 56Fe are fully thermalized: M(56Ni)08S = 7.866×10−44Lexp[ (t − t0)/(1 + z) − τNi τCo ]M⊙(2) where t0 is the explosion epoch,τNi = 8.76 days the life time of 56Ni and τCo…”
Progenitors of Core-Collapse Supernovae (2009, background): “The differences between the observed characteristics of II-P SNe in particular has previously been attributed to large differences in the progenitor mass and radii (Hamuy 2003, Nadyozhin 2003, Utrobin and Chugai 2008).”
THE COSMIC CORE-COLLAPSE SUPERNOVA RATE DOES NOT MATCH THE MASSIVE-STAR FORMATION RATE (2011, background): “Type IIP SNe are the most common type of CC SNe and also the most varied in terms of luminosity (e.g., Richardson et al. 2002; Hamuy 2003).”
DUST AND THE TYPE II-PLATEAU SUPERNOVA 2004dj (2009, methodology): “Kotak et al. (2005) used the V band exponential tail method of Hamuy (2003) to derive a 56Ni mass of ∼ 0.022M⊙.”
A simple approach to the supernova progenitor–explosion connection (2016, background): “The picture is similar for the nickel mass and its correlation to the explosion energy that has already been noted by Hamuy (2003).”
CHARACTERIZING THE V-BAND LIGHT-CURVES OF HYDROGEN-RICH TYPE II SUPERNOVAE (2014, methodology): “Given that peak epochs of SNe II are often hard to define, literature measurements of SN II brightness have generally concentrated on some epoch during the ‘plateau’ (e.g. Hamuy 2003a; Nugent et al. 2006).”
Low‐luminosity Type II supernovae: spectroscopic and photometric evolution (2003, methodology): “Comparison with a sequence of more normal Type II SNe (Hamuy 2003; Zampieri et al., in preparation) suggests that this group of SNe represent the extreme low-luminosity tail of a single continuous distribution.”