Progenitors of Core-Collapse Supernovae

By S. Smartt. 2009

884 citations recorded by the source corpus.

Knowledge of the progenitors of core-collapse supernovae is a fundamental component in understanding the explosions. The recent progress in finding such stars is reviewed. The minimum initial mass that can produce a supernova (SN) has converged to 8 ± 1 M⊙ from direct detections of red supergiant progenitors of II-P SNe and the most massive white dwarf progenitors, although this value is model dependent. It appears that most type Ibc SNe arise from moderate mass interacting binaries. The highly energetic, broad-lined Ic SNe are likely produced by massive, Wolf-Rayet progenitors. There is some evidence to suggest that the majority of massive stars above ∼20 M⊙ may collapse quietly to black holes and that the explosions remain undetected. The recent discovery of a class of ultrabright type II SNe and the direct detection of some progenitor stars bearing luminous blue variable characteristics suggest some very massive stars do produce highly energetic explosions. The physical mechanism is under debate, and t...

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/30bca72925fe18c90a1bb205a4d41b3a22e7ad40

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Instrumentation

Citations in the corpus

TOWARD CHARACTERIZATION OF THE TYPE IIP SUPERNOVA PROGENITOR POPULATION: A STATISTICAL SAMPLE OF LIGHT CURVES FROM Pan-STARRS1 (2014, background): “However, even accounting for IMF prescriptions of varying steepness, Smartt (2009) reported an upper limit for the SN IIP progenitor mass of 16.5 M based on their direct progenitor detection search.”
THE BLACK HOLE MASS DISTRIBUTION IN THE GALAXY (2010, background): “Observations of mass losing evolved stars are one of the direct ways of studying the end stages of stellar evolution (Smartt 2009).”
THE FIRST SYSTEMATIC STUDY OF TYPE Ibc SUPERNOVA MULTI-BAND LIGHT CURVES (2010, background): “Unlike other core-collapse SNe, however, the progenitor systems of SNe Ibc have yet to be directly identified in preexplosion images (see Smartt 2009 for a review).”
Bolometric light curves and explosion parameters of 38 stripped-envelope core-collapse supernovae (2014, background): “Observationally, SNe II are seen to be explosions from stars at the lower end of the massive star range (∼8–16 M ; see Smartt 2009, for a review),2 which have not suffered sufficient mass-loss to remove their hydrogen envelopes.”
Progenitor mass constraints for core-collapse supernovae from correlations with host galaxy star formation⋆ (2012, background): “Unfortunately, we are still awaiting a direct detection of an SNIbc (Smartt 2009).”
The death of massive stars – I. Observational constraints on the progenitors of Type II-P supernovae (2008, background): “The lower initial mass limit for an SN progenitor in such a system is uncertain, but is probably around the limit for single stars to produce Fe cores, or O–Mg–Ne cores, around 8 M (Smartt 2009).”
Supernova remnants: the X-ray perspective (2011, background): “…supernovae, and optical studies of potential progenitor stars confirm that their progenitors have initial masses in the ∼ 8− 17 M⊙ range, and that they explode in the red supergiant phase, while still having a substantial hydrogen envelope (see the discussions in Smartt, 2009; Chevalier, 2005).”
The Origin of Elements from Carbon to Uranium (2020, background): “In searching for the progenitor stars at the locations of nearby SNe II-P, no progenitor stars have been found with initial masses M>30Me (Smartt 2009).”
THE LANDSCAPE OF THE NEUTRINO MECHANISM OF CORE-COLLAPSE SUPERNOVAE: NEUTRON STAR AND BLACK HOLE MASS FUNCTIONS, EXPLOSION ENERGIES, AND NICKEL YIELDS (2014, background): “…& 0.5 based on direct supernova detection, estimates of supernova production in the Galaxy, star formation rate or diffuse neutrino background (e.g. Kochanek et al. 2008; Kochanek 2014b; Smartt 2009; Horiuchi et al. 2011; Adams et al. 2013; Nakazato 2013; Clausen et al. 2014; Mathews et al. 2014).”
First results from the IllustrisTNG simulations: a tale of two elements - chemical evolution of magnesium and europium (2017, background): “The assumed lower mass limit for corecollapse supernovae in IllustrisTNG is 8 M , a generous lower limit for the progenitors of a SNII (Smartt 2009; Ibeling & Heger 2013; Woosley & Heger 2015; Sukhbold et al. 2016).”
How much H and He is ‘hidden’ in SNe Ib/c? – I. Low-mass objects (2012, background): “2007) and the progenitor stars (Georgy et al. 2009; Smartt 2009; Yoon et al. 2010) are progressively being resolved.”
PREPARING FOR AN EXPLOSION: HYDRODYNAMIC INSTABILITIES AND TURBULENCE IN PRESUPERNOVAE (2013, background): “Woosley et al. (2007) suggested that the precursor outburst of SN 2006jc might have been a pulsational pair instability eruption. four cases suggest progenitor stars that are much more massive than the typical red supergiant progenitors of SNe II-P (Smartt 2009).”
On the nature of supernovae Ib and Ic (2012, background): “This difficulty to make SNe Ib might be reflected by the 2:1 occurrence rates of SNe Ic:Ib (Smartt 2009).”
Grids of stellar models with rotation - II. WR populations and supernovae/GRB progenitors at Z = 0.014 (2012, background): “…the hypothesis that the progenitor population of all Ibc SNe are massive WR stars, the probability that they did not detect any of the 10 progenitors by chance would then be only 11%, assuming that the Ib progenitors are WN stars and Ic progenitors are WC/WO stars (see more detail in Smartt 2009).”
Dawes Review 6: The Impact of Companions on Stellar Evolution (2016, background): “The modern consensus is that the type Ia supernovae are thermal runaway explosions of carbon–oxygen WD (e.g., Hillebrandt & Niemeyer, 2000), whilst Ib and Ic supernovae are helium stars that undergo core collapse (e.g., Smartt, 2009).”
Supernovae from red supergiants with extensive mass loss (2010, methodology): “…get information about the progenitors of CCSNe by directly getting images of the SN progenitors by looking into the archival images of the SN site (Smartt 2009, and the references therein) or statistically analysing the number of ⋆ takashi.moriya@ipmu.jp SNe appeared (e.g., Smith et al. 2010;…”
The progenitor mass of the Type IIP supernova SN 2004et from late-time spectral modeling (2012, methodology): “Such identifications have now been made for the Type IIP SNe SN 2003gd, SN 2004A, SN 2004et, SN 2005cs, SN 2008bk, SN 2008cn, and SN 2009md (Smartt 2009; Elias-Rosa et al. 2009; Fraser et al. 2011, and references therein).”
EVLA OBSERVATIONS CONSTRAIN THE ENVIRONMENT AND PROGENITOR SYSTEM OF Type Ia SUPERNOVA 2011fe (2012, methodology): “10 Mpc) core-collapse SNe (Weiler et al. 2002)— explosions that mark the death of massive stars, M & 8 M⊙ (Smartt 2009).”