THE COMPACTNESS OF PRESUPERNOVA STELLAR CORES

By T. Sukhbold, Stan Woosley. 2013

168 citations recorded by the source corpus.

The success or failure of the neutrino-transport mechanism for producing a supernova in an evolved massive star is known to be sensitive not only to the mass of the iron core that collapses, but also to the density gradient in the silicon and oxygen shells surrounding that core. Here we study the systematics of a presupernova core's “compactness” as a function of the mass of the star and the physics used in its calculation. Fine-meshed surveys of presupernova evolution are calculated for stars from 15 to 65 M☉. The metallicity and the efficiency of semiconvection and overshoot mixing are both varied and bare carbon-oxygen cores are explored as well as full hydrogenic stars. Two different codes, KEPLER and MESA, are used for the study. A complex interplay of carbon and oxygen burning, especially in shells, can cause rapid variations in the compactness for stars of very nearly the same mass. On larger scales, the distribution of compactness with main sequence mass is found to be robustly non-monotonic, implying islands of “explodabilty,” particularly around 8–20 M☉ and 25–30 M☉. The carbon-oxygen (CO) core mass of a presupernova star is a better, (though still ambiguous) discriminant of its core structure than the main sequence mass.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/152962e22b64b6bd2f0fba01b9f6832f4aa3632d

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Citations in the corpus

CORE-COLLAPSE SUPERNOVAE FROM 9 TO 120 SOLAR MASSES BASED ON NEUTRINO-POWERED EXPLOSIONS (2015, methodology): “The nonmonotonic nature of compactness is due to the migration of the location of carbon- and oxygen-burning shells with changing mass (Sukhbold & Woosley 2014).”
Exploring Fundamentally Three-dimensional Phenomena in High-fidelity Simulations of Core-collapse Supernovae (2018, background): “…is typically silicon shell that is undergoing nuclear burning that may or may not be convective at the point of core collapse, depending on the preceding evolution (cf., Chieffi & Limongi 2013; Sukhbold & Woosley 2014), above this silicon shell is an oxygen shell that is also typically convective.”
THE REMARKABLE DEATHS OF 9–11 SOLAR MASS STARS (2015, methodology): “There is considerable variation for this quantity in the literature though (Eldridge & Tout 2004; Sukhbold & Woosley 2014), and our core masses are within previously published ranges.”
Formation of Double Neutron Star Systems (2017, background): “Sukhbold & Woosley (2014) argued that ξ at bounce is correlated with ξ at the onset of core collapse, and hence the calculated pre-SN density structures can help in forecasting the mapping between pre-SN (ideally even ZAMS for single stars) parameters and the outcome of a core collapse.”
What can be learned from a future supernova neutrino detection (2017, background): “range depending how the simulation was done [170].”
The search for failed supernovae with the Large Binocular Telescope: confirmation of a disappearing star (2016, background): “…et al. 2009; Smartt 2015) and corresponds to a progenitor with a high “compactness” parameter that is considered most likely to result in a failed supernova (O’Connor & Ott 2011; Ugliano et al. 2012; Horiuchi et al. 2014; Sukhbold & Woosley 2014; Pejcha & Thompson 2015; Sukhbold et al. 2016).”
Unifying Type II Supernova Light Curves with Dense Circumstellar Material (2016, methodology): “We use non-rotating solar-metallicity RSG models from the stellar evolution code KEPLER (Weaver et al. 1978; Woosley & Heger 2007, 2015; Sukhbold & Woosley 2014; Sukhbold et al. 2016) with ZAMS masses in the range between 9M and 16.5M .”
THE LANDSCAPE OF THE NEUTRINO MECHANISM OF CORE-COLLAPSE SUPERNOVAE: NEUTRON STAR AND BLACK HOLE MASS FUNCTIONS, EXPLOSION ENERGIES, AND NICKEL YIELDS (2014, background): “This is the result of variations in progenitor structure, which originate in the latest stages of stellar evolution and even similar CO core masses might lead to different outcomes as measured by the compactness Sukhbold & Woosley (2014).”
A High-resolution Study of Presupernova Core Structure (2017, methodology): “Because some of the models from Sukhbold & Woosley (2014) were used by Sukhbold et al. (2016), it also affected the outcome of that work for masses larger than 14 M .”
Observational Constraints on the Progenitors of Core-Collapse Supernovae: The Case for Missing High-Mass Stars (2015, methodology): “As discussed in the introduction in Sukhbold & Woosley (2014), the density gradient in more massive stars is relatively shallow, which will likely lead to higher accretion rates onto the compact object created at the point of collapse.”
Measuring the Progenitor Masses and Dense Circumstellar Material of Type II Supernovae (2017, methodology): “As in our previous work (Morozova et al. 2017), we use the non-rotating solar-metallicity RSG models from the stellar evolution code KEPLER (Weaver et al. 1978; Woosley & Heger 2007, 2015; Sukhbold & Woosley 2014; Sukhbold et al. 2016).”
A TWO-PARAMETER CRITERION FOR CLASSIFYING THE EXPLODABILITY OF MASSIVE STARS BY THE NEUTRINO-DRIVEN MECHANISM (2015, methodology): “…(Heger 2003, private communication); the solar-metallicity s2013 (151 models, 15.0–30.0 M ) and sh2013 series (15 models, 30.0–60.0 M , no mass loss) of Sukhbold & Woosley (2014), supplemented by additional 36 models with 9.0–14.9 M ; the solar-metallicity s2007 series (32 models, 12.0–120.0 M )…”
MESA ISOCHRONES AND STELLAR TRACKS (MIST). I. SOLAR-SCALED MODELS (2016, background): “Additionally, the resulting core mass has significant implications for the supernova progenitors, from their ability to undergo a successful explosion (e.g., Sukhbold & Woosley 2014) to the actual nucleosynthetic yields (e.g., Langer et al. 1989; Heger & Woosley 2002; Rauscher et al. 2002).”
Binary Population and Spectral Synthesis Version 2.1: Construction, Observational Verification, and New Results (2017, result): “Ours is a relatively simple method but does produce similar island of stability to that found by other authors (Ugliano et al. 2012; Sukhbold & Woosley 2014; Ertl et al. 2016).”