The State of Matter in Simulations of Core-Collapse supernovae—Reflections and Recent Developments

Fischer, Tobias; Bastian, Niels-Uwe F.; Blaschke, D.; Cierniak, Mateusz; Hempel, Matthias; Klähn, T.; Martı́nez-Pinedo, G.; Newton, William; Röpke, G.; Typel, S.

doi:10.1017/pasa.2017.63

Cited by 48 publications

(57 citation statements)

References 181 publications

(310 reference statements)

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“…The NSE conditions found in the collapsing stellar core feature a broad distribution of nuclei with a pronounced peak around the iron-group, at low densities (see Figure 2 of Ref. [58]). In simulations of supernovae, this nuclear distribution is classified by the NSE average, including nuclear shell effects as discussed [75], which extends beyond the commonly used single-nucleus approximation.…”

Section: Heavy Nuclear Clusters With a 56mentioning

confidence: 96%

“…This applies equally for light and heavy nuclear clusters. In comparison with the state-of-the-art quantum statistical approach [86,87] the deficits of NSE are revealed [58], while the cluster-virial EOS can provide the constraint at low densities [16]. It relates to the overestimation of the abundance of light clusters and in particular the too late dissolving of clusters into homogeneous matter.…”

Section: Light Nuclear Clusters With a ≤mentioning

confidence: 96%

“…Figure 1a of Ref. [58]). At T ≤ 0.5 MeV, time-dependent processes determine the nuclear composition, where heavy nuclei dominate.…”

Section: Applications In Core-collapse Supernovae and Neutron Starsmentioning

confidence: 97%

“…However, the ν e charged-current opacity is dominated by absorption on free neutrons. The situation is different forν e , since it was shown that protons and light clusters have similar abundances [58,85]. Taking properly into medium modifications for the cross sections and the proper phase-space of the contributing particles, the final rates are generally small.…”

Section: Light Nuclear Clusters With a ≤mentioning

confidence: 99%

“…It leads to an overestimate of the abundances of the unbound baryons and 4 He. This has important consequences for the supernova results, since such simplistic approach overestimates the neutrino response with the neutrons and protons, which in turn changes the supernova neutrino fluxes and spectra, however, with only a mild impact on the overall supernova dynamics [58].…”

Section: Light Nuclear Clusters With a ≤mentioning

confidence: 99%

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Towards a Unified Quark-Hadron-Matter Equation of State for Applications in Astrophysics and Heavy-Ion Collisions

et al. 2018

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Abstract:We outline an approach to a unified equation of state for quark-hadron matter on the basis of a Φ−derivable approach to the generalized Beth-Uhlenbeck equation of state for a cluster decomposition of thermodynamic quantities like the density. To this end we summarize the cluster virial expansion for nuclear matter and demonstrate the equivalence of the Green's function approach and the Φ−derivable formulation. As an example, the formation and dissociation of deuterons in nuclear matter is discussed. We formulate the cluster Φ−derivable approach to quark-hadron matter which allows to take into account the specifics of chiral symmetry restoration and deconfinement in triggering the Mott-dissociation of hadrons. This approach unifies the description of a strongly coupled quark-gluon plasma with that of a medium-modified hadron resonance gas description which are contained as limiting cases. The developed formalism shall replace the common two-phase approach to the description of the deconfinement and chiral phase transition that requires a phase transition construction between separately developed equations of state for hadronic and quark matter phases. Applications to the phenomenology of heavy-ion collisions and astrophysics are outlined.

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Section: Heavy Nuclear Clusters With a 56mentioning

confidence: 96%

Section: Light Nuclear Clusters With a ≤mentioning

confidence: 96%

“…Figure 1a of Ref. [58]). At T ≤ 0.5 MeV, time-dependent processes determine the nuclear composition, where heavy nuclei dominate.…”

Section: Applications In Core-collapse Supernovae and Neutron Starsmentioning

confidence: 97%

Section: Light Nuclear Clusters With a ≤mentioning

confidence: 99%

Section: Light Nuclear Clusters With a ≤mentioning

confidence: 99%

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Towards a Unified Quark-Hadron-Matter Equation of State for Applications in Astrophysics and Heavy-Ion Collisions

et al. 2018

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Phases of Dense Matter in Compact Stars

Blaschke

Chamel

2018

The Physics and Astrophysics of Neutron Stars

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Formed in the aftermath of gravitational core-collapse supernova explosions, neutron stars are unique cosmic laboratories for probing the properties of matter under extreme conditions that cannot be reproduced in terrestrial laboratories. The interior of a neutron star, endowed with the highest magnetic fields known and with densities spanning about ten orders of magnitude from the surface to the centre, is predicted to exhibit various phases of dense strongly interacting matter, whose physics is reviewed in this chapter. The outer layers of a neutron star consist of a solid nuclear crust, permeated by a neutron ocean in its densest region, possibly on top of a nuclear "pasta" mantle. The properties of these layers and of the homogeneous isospin asymmetric nuclear matter beneath constituting the outer core may still be constrained by terrestrial experiments. The inner core of highly degenerate, strongly interacting matter poses a few puzzles and questions which are reviewed here together with perspectives for their resolution. Consequences of the dense-matter phases for observables such the neutron-star mass-radius relationship and the prospects to uncover their structure with modern observational programmes are touched upon.

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Hydrodynamics of core-collapse supernovae and their progenitors

Müller¹

2020

Living Rev Comput Astrophys

161

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Multi-dimensional fluid flow plays a paramount role in the explosions of massive stars as core-collapse supernovae. In recent years, three-dimensional (3D) simulations of these phenomena have matured significantly. Considerable progress has been made towards identifying the ingredients for shock revival by the neutrino-driven mechanism, and successful explosions have already been obtained in a number of selfconsistent 3D models. These advances also bring new challenges, however. Prompted by a need for increased physical realism and meaningful model validation, supernova theory is now moving towards a more integrated view that connects multi-dimensional phenomena in the late convective burning stages prior to collapse, the explosion engine, and mixing instabilities in the supernova envelope. Here we review our current understanding of multi-D fluid flow in core-collapse supernovae and their progenitors. We start by outlining specific challenges faced by hydrodynamic simulations of core-collapse supernovae and of the late convective burning stages. We then discuss recent advances and open questions in theory and simulations.

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The State of Matter in Simulations of Core-Collapse supernovae—Reflections and Recent Developments

Cited by 48 publications

References 181 publications

Towards a Unified Quark-Hadron-Matter Equation of State for Applications in Astrophysics and Heavy-Ion Collisions

Towards a Unified Quark-Hadron-Matter Equation of State for Applications in Astrophysics and Heavy-Ion Collisions

Phases of Dense Matter in Compact Stars

Hydrodynamics of core-collapse supernovae and their progenitors

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