The progenitors of core-collapse supernovae

By John J. Eldridge. 2004

313 citations recorded by the source corpus.

We present maps of the nature of single star progenitors of supernovae and their remnants in mass and metallicity space. We find our results are similar to others but we have gone further in varying the amount of mixing and using various mass-loss schemes to see how the maps change. We find that extra mixing, in the form of convective overshooting, moves boundaries such as the minimum mass for a supernova or Wolf-Rayet (WR) star to lower masses. We also find that the pre-WR mass loss determines the shape of our maps. We find that different mass-loss rates lead to quite different results. We find that the rise in luminosity at second dredge-up places quite tight constraints on the masses of some progenitors and in particular the progenitor of supernova 2003gd.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/fb1a099756020c1d3e118f391bc99232bcefcb97

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

1. S. Smartt
2. Stan Woosley
3. N. Smith
4. N. Langer
5. Robert G. Izzard
6. Michela Mapelli
7. A. Karakas
8. J. Eldridge

In Instrumentation

1. N. Smith
2. S. Smartt
3. N. Langer
4. Stan Woosley
5. Robert G. Izzard
6. A. Karakas
7. G. Meynet
8. R. Hirschi

Citations in the corpus

• Progenitors of Core-Collapse Supernovae (2009, methodology): “Also the observed mass-loss rate of 16-20M⊙ stars would be somewhat too low to produce WR stars in evolutionary models which adopt these Ṁ values (see Heger et al. 2003, Hirschi, Meynet, and Maeder 2004, Eldridge and Tout 2004, Crowther 2007).”
• THE YELLOW SUPERGIANT PROGENITOR OF THE TYPE II SUPERNOVA 2011dh IN M51 (2011, background): “4 and compared with stars stellar evolution tracks (Eldridge & Tout 2004).”
• On the birthrates of Galactic neutron stars (2008, unknown): “While stellar modelling results (Eldridge & Tout 2004; Podsiadlowski et al. 2004) had seen electron-capture SNe only possible in close binary systems,3 some very recent work has examined this process in isolated stars (Prelarends et al 2008).”
• COMPACT REMNANT MASS FUNCTION: DEPENDENCE ON THE EXPLOSION MECHANISM AND METALLICITY (2011, methodology): “Later calculations with an updated evolutionary code (Eldridge & Tout 2004a, 2004b) indicated that ECS may occur for higher initial masses (Mzams 7.5 M ).”
• The death of massive stars – I. Observational constraints on the progenitors of Type II-P supernovae (2008, methodology): “The precise configuration of a star at the moment of core-collapse and how this determines the resulting SN type are still quite uncertain (e.g. Heger et al. 2003; Eldridge & Tout 2004).”
• The Dawes Review 2: Nucleosynthesis and Stellar Yields of Low- and Intermediate-Mass Single Stars (2014, background): “Stars with more massive cores will undergo off-centre Ne ignition with convective flashes (Ritossa et al. 1999; Eldridge & Tout 2004).”
• What can be learned from a future supernova neutrino detection (2017, methodology): “[69] S. J. Smartt, “Progenitors of Core-Collapse Supernovae,” Ann.”
• Evolution of massive AGB stars - II. model properties at non-solar metallicity and the fate of Super-AGB stars (2007, background): “The fraction of stars with initial mass between Mup and Mmas which evolve into the ONe WD and electron capture supernova (EC-SN) channels is largely uncertain and very dependent on composition, mass loss rate or internal mixing (Eldridge & Tout 2004).”
• The Effect of Massive Binaries on Stellar Populations and Supernova Progenitors (2007, methodology): “We have constructed a set of binary stellar models covering a wide range of binary parameter space using a detailed stellar evolution code (Eldridge & Tout 2004a).”
• BPASS predictions for binary black hole mergers (2016, methodology): “However at higher initial masses, mass-loss can still lead to the formation of neutron stars (e.g. Eldridge & Tout 2004; Heger et al. 2003; Ugliano et al. 2012; Sukhbold et al. 2016).”
• The great escape: how exoplanets and smaller bodies desert dying stars (2011, background): “Additionally, lower metallicity stars can begin neutron star formation and black hole formation at different values; the representative ones might be 6 and 18 M , respectively (Heger et al. 2003; Eldridge & Tout 2004; Belczynski et al. 2010).”
• Massive stars exploding in a He-rich circumstellar medium. I. Type Ibn (SN 2006jc-like) events (2008, background): “At the time of explosion, which is expected to occur a few× 105 years after the last major LBV outburst (see e.g. Heger et al. 2003; Eldridge & Tout 2004), the mass ofthe WR star is expected to be of the order of 15-20M⊙.”
• Super and massive AGB stars - IV. Final fates - Initial to final mass relation (2014, background): “Analogously to carbon burning in super-AGB stars, models with very massive cores MC & 1.35M⊙ ignite neon off-center, under degenerate conditions with associated convective flashes (Ritossa et al. 1999; Eldridge & Tout 2004).”
• The Supernova Channel of Super-AGB Stars (2007, background): “Eldridge & Tout (2004b) determine a minimum mass for supernova explosion around 7 M (with overshooting), or around 9 M (without overshooting), again without being able to calculate the stellar evolution models through the final phases.”
• Optical and near infrared coverage of SN 2004et: physical parameters and comparison with other type IIP supernovae (2009, methodology): “Stellar evolutionary models predict that most single stars with masses in the range∼ 8–30 M⊙ should end their lives as red supergiants and produce type II SNe (Eldridge & Tout 2004; Heger et al. 2003; Hirschi et al. 2004; Limongi & Chieffi 2003).”
• Early and late time VLT spectroscopy of SN 2001el - Progenitor constraints for a type Ia supernova (2005, background): “2003; Eldridge & Tout 2004), similar constraints are still missing for the progenitors of thermonuclear (type Ia) supernovae Send offprint requests to: S. Mattila; e-mail: seppo@astro.su.se ⋆ Based on observations collected at the European Southern Observatory, Paranal, Chile (ESO Programmes 67.”
• Binary Population and Spectral Synthesis Version 2.1: Construction, Observational Verification, and New Results (2017, methodology): “The opacity tables are described in Eldridge & Tout (2004a) and are based on the OPAL (Iglesias & Rogers 1996) and Ferguson et al. (2005) opacities.”
• Double neutron stars: merger rates revisited (2017, methodology): “In StarTrack we follow the study of Hurley, Pols & Tout (2000) (with the updated mass range based on the results of Eldridge & Tout 2004a,b, see 3.2 for details) and use the mass of the core at this stage to decide whether a star will develop a degenerate ONeMg core and thus whether at some point…”
• Observed Fractions of Core-Collapse Supernova Types and Initial Masses of their Single and Binary Progenitor Stars (2010, background): “Single-star evolution models adopt simple prescriptions for these steady winds (Meynet et al. 1994), and aim to predict the fates of massive stars as functions of initial mass and metallicity (e.g. Heger et al. 2003; Eldridge & Tout 2004).”