Core-collapse Supernovae: From Neutrino-driven 1D Explosions to Light Curves and Spectra

Curtis, Sanjana; E., Wolfe, Noah; Fröhlich, C.; Miller, Jonah; Wollaeger, Ryan; Ebinger, Kevin

doi:10.3847/1538-4357/ac0dc5

Cited by 14 publications

(16 citation statements)

References 114 publications

Supporting

Mentioning

Contrasting

Unclassified

Order By: Relevance

“…The explosion energies, explodability, and the shape of each as a function of ZAMS mass differ nontrivially for STIR and PUSH (see Couch et al 2020;Ebinger et al 2019), and this could impact global trends in explosion properties. On the other hand, Curtis et al (2020) obtained their 56 Ni distributions using a nuclear reaction network in conjunction with their CCSN simulations. As aforementioned, we estimated 56 Ni mass from the explosion energy, informed by KEPLER yields.…”

Section: Discussionmentioning

confidence: 99%

Connecting the Light Curves of Type IIP Supernovae to the Properties of Their Progenitors

Barker

Harris

Warren³

et al. 2022

ApJ

View full text Add to dashboard Cite

Observations of core-collapse supernovae (CCSNe) reveal a wealth of information about the dynamics of the supernova ejecta and its composition but very little direct information about the progenitor. Constraining properties of the progenitor and the explosion requires coupling the observations with a theoretical model of the explosion. Here we begin with the CCSN simulations of Couch et al., which use a nonparametric treatment of the neutrino transport while also accounting for turbulence and convection. In this work we use the SuperNova Explosion Code to evolve the CCSN hydrodynamics to later times and compute bolometric light curves. Focusing on Type IIP SNe (SNe IIP), we then (1) directly compare the theoretical STIR explosions to observations and (2) assess how properties of the progenitor’s core can be estimated from optical photometry in the plateau phase alone. First, the distribution of plateau luminosities (L 50) and ejecta velocities achieved by our simulations is similar to the observed distributions. Second, we fit our models to the light curves and velocity evolution of some well-observed SNe. Third, we recover well-known correlations, as well as the difficulty of connecting any one SN property to zero-age main-sequence mass. Finally, we show that there is a usable, linear correlation between iron core mass and L 50 such that optical photometry alone of SNe IIP can give us insights into the cores of massive stars. Illustrating this by application to a few SNe, we find iron core masses of 1.3–1.5 M ⊙ with typical errors of 0.05 M ⊙. Data are publicly available online on Zenodo: doi:10.5281/zenodo.6631964.

show abstract

Section: Discussionmentioning

confidence: 99%

Connecting the Light Curves of Type IIP Supernovae to the Properties of Their Progenitors

Barker

Harris

Warren³

et al. 2022

ApJ

View full text Add to dashboard Cite

show abstract

“…Our framework ("PUSH") mimics the netenhanced energy deposition expected from multidimensional fluid motion in a spherically symmetric simulation. Due to the physical coupling of core and outer layers, and the computational efficiency of PUSH, observable quantities such as remnant masses, nucleosynthetic yields, and electromagnetic signals can be generated self-consistently for a wide variety of models (Ebinger et al 2020;Curtis et al 2021) in a fraction of the time of full 3D first-principle models.…”

Section: Simulationsmentioning

confidence: 99%

A New Constraint on the Nuclear Equation of State from Statistical Distributions of Compact Remnants of Supernovae

Meskhi

Dai

et al. 2022

ApJL

Self Cite

View full text Add to dashboard Cite

Understanding how matter behaves at the highest densities and temperatures is a major open problem in both nuclear physics and relativistic astrophysics. Our understanding of such behavior is often encapsulated in the so-called high-temperature nuclear equation of state (EOS), which influences compact binary mergers, core-collapse supernovae, and other phenomena. Our focus is on the type (either black hole or neutron star) and mass of the remnant of the core collapse of a massive star. For each six candidates of equations of state, we use a very large suite of spherically symmetric supernova models to generate a sample of synthetic populations of such remnants. We then compare these synthetic populations to the observed remnant population. Our study provides a novel constraint on the high-temperature nuclear EOS and describes which EOS candidates are more or less favored by an information-theoretic metric.

show abstract

“…These calculations simulate the collapse and explosion, but they need alternative codes to reproduce SN observables. Recent efforts have been made in this direction (Sukhbold et al 2016;Curtis et al 2021;Barker et al 2021), where multi-dimensional explosions are sometimes mimicked in 1D models and mapped to different codes to further obtain SN observables. While this methodology is more consistent (given that it only needs the progenitor structure as input), sometimes it cannot reproduce the observations and is restricted to a limited parameter space.…”

Section: Introductionmentioning

confidence: 99%

Type II supernovae from the Carnegie Supernova Project-I

Martínez

Bersten

Anderson

et al. 2022

A&A

View full text Add to dashboard Cite

Linking supernovae to their progenitors is a powerful method for furthering our understanding of the physical origin of their observed differences while at the same time testing stellar evolution theory. In this second study of a series of three papers where we characterise type II supernovae (SNe II) to understand their diversity, we derive progenitor properties (initial and ejecta masses and radius), explosion energy, and 56Ni mass and its degree of mixing within the ejecta for a large sample of SNe II. This dataset was obtained by the Carnegie Supernova Project-I and is characterised by a high cadence of SNe II optical and near-infrared light curves and optical spectra that were homogeneously observed and processed. A large grid of hydrodynamical models and a fitting procedure based on Markov chain Monte Carlo methods were used to fit the bolometric light curve and the evolution of the photospheric velocity of 53 SNe II. We infer ejecta masses of between 7.9 and 14.8 M⊙, explosion energies between 0.15 and 1.40 foe, and 56Ni masses between 0.006 and 0.069 M⊙. We define a subset of 24 SNe (the ‘gold sample’) with well-sampled bolometric light curves and expansion velocities for which we consider the results more robust. Most SNe II in the gold sample (∼88%) are found with ejecta masses in the range of ∼8−10 M⊙, coming from low zero-age main-sequence masses (9−12 M⊙). The modelling of the initial-mass distribution of the gold sample gives an upper mass limit of 21.3$ ^{+3.8}_{-0.4} $ M⊙ and a much steeper distribution than that for a Salpeter massive-star initial mass function (IMF). This IMF incompatibility is due to the large number of low-mass progenitors found – when assuming standard stellar evolution. This may imply that high-mass progenitors lose more mass during their lives than predicted. However, a deeper analysis of all stellar evolution assumptions is required to test this hypothesis.

show abstract

Core-collapse Supernovae: From Neutrino-driven 1D Explosions to Light Curves and Spectra

Cited by 14 publications

References 114 publications

Connecting the Light Curves of Type IIP Supernovae to the Properties of Their Progenitors

Connecting the Light Curves of Type IIP Supernovae to the Properties of Their Progenitors

A New Constraint on the Nuclear Equation of State from Statistical Distributions of Compact Remnants of Supernovae

Type II supernovae from the Carnegie Supernova Project-I

Contact Info

Product

Resources

About