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Equation of state effects in the core collapse of a 20-M-circle dot star
Stockholm University, Faculty of Science, Department of Astronomy. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC). California Institute of Technology, USA.
Stockholm University, Faculty of Science, Department of Astronomy. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
Number of Authors: 42019 (English)In: Physical Review C: Covering Nuclear Physics, ISSN 2469-9985, E-ISSN 2469-9993, Vol. 100, no 5, article id 055802Article in journal (Refereed) Published
Abstract [en]

Uncertainties in our knowledge of the properties of dense matter near and above nuclear saturation density are among the main sources of variations in multimessenger signatures predicted for core-collapse supernovae (CCSNe) and the properties of neutron stars (NSs). We construct 97 new finite-temperature equations of state (EOSs) of dense matter that obey current experimental, observational, and theoretical constraints and discuss how systematic variations in the EOS parameters affect the properties of cold nonrotating NSs and the core collapse of a 20-M-circle dot progenitor star. The core collapse of the 20-M-circle dot progenitor star is simulated in spherical symmetry using the general-relativistic radiation-hydrodynamics code GRID where neutrino interactions are computed for each EOS using the NULIB library. We conclude that the effective mass of nucleons at densities above nuclear saturation density is the largest source of uncertainty in the CCSN neutrino signal and dynamics even though it plays a subdominant role in most properties of cold NS matter. Meanwhile, changes in other observables affect the properties of cold NSs, while having little effect in CCSNe. To strengthen our conclusions, we perform six octant three-dimensional CCSN simulations varying the effective mass of nucleons at nuclear saturation density. We conclude that neutrino heating and, thus, the likelihood of explosion is significantly increased for EOSs where the effective mass of nucleons at nuclear saturation density is large.

Place, publisher, year, edition, pages
2019. Vol. 100, no 5, article id 055802
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
URN: urn:nbn:se:su:diva-176614DOI: 10.1103/PhysRevC.100.055802ISI: 000495064700005OAI: oai:DiVA.org:su-176614DiVA, id: diva2:1381931
Available from: 2019-12-30 Created: 2019-12-30 Last updated: 2019-12-30Bibliographically approved

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Schneider, Andre S.O'connor, Evan
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