Nuclear input for core-collapse models

Martı́nez-Pinedo, G.; Liebendörfer, M.; Frekers, D.

doi:10.1016/j.nuclphysa.2006.02.014

Cited by 39 publications

(47 citation statements)

References 143 publications

(284 reference statements)

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“…Electron capture on free protons and heavy nuclei during collapse reduces Y e (i.e., "deleptonizes" the collapsing core) and consequently decreases the size of the homologously collapsing inner core that depends on the average value of Y e in a roughly quadratic way (see, e.g., [56]). The material of the inner core is in sonic contact and determines the dynamics and the gravitational wave signal at core bounce and in the early postbounce phases.…”

Section: Deleptonization and Neutrino Pressurementioning

confidence: 99%

Gravitational wave burst signal from core collapse of rotating stars

et al. 2008

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We present results from detailed general relativistic simulations of stellar core collapse to a protoneutron star, using two different microphysical nonzero-temperature nuclear equations of state as well as an approximate description of deleptonization during the collapse phase. Investigating a wide variety of rotation rates and profiles as well as masses of the progenitor stars and both equations of state, we confirm in this very general setup the recent finding that a generic gravitational wave burst signal is associated with core bounce, already known as type I in the literature. The previously suggested type II (or "multiple-bounce") waveform morphology does not occur. Despite this reduction to a single waveform type, we demonstrate that it is still possible to constrain the progenitor and postbounce rotation based on a combination of the maximum signal amplitude and the peak frequency of the emitted gravitational wave burst. Our models include to sufficient accuracy the currently known necessary physics for the collapse and bounce phase of core-collapse supernovae, yielding accurate and reliable gravitational wave signal templates for gravitational wave data analysis. In addition, we assess the possiblity of nonaxisymmetric instabilities in rotating nascent proto-neutron stars. We find strong evidence that in an iron core-collapse event the postbounce core cannot reach sufficiently rapid rotation to become subject to a classical bar-mode instability. However, many of our postbounce core models exhibit sufficiently rapid and differential rotation to become subject to the recently discovered dynamical instability at low rotation rates.

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Section: Deleptonization and Neutrino Pressurementioning

confidence: 99%

Gravitational wave burst signal from core collapse of rotating stars

et al. 2008

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“…However, the input physics relevant during the collapse of the stellar core is very rich on the microscopic level (Martínez-Pinedo et al 2006), and this dynamical phase is very sensitive to small perturbations. The evolution of the collapsing core depends significantly on the adiabatic index of the equation of state, general relativistic effects, the electron capture rates on free protons and nuclei, and the coherent scattering opacities of neutrinos off the different nuclei.…”

Section: Core-collapse and Bouncementioning

confidence: 99%

Gravitational waves from 3D MHD core collapse simulations

Scheidegger

Fischer

Whitehouse

et al. 2008

A&A

112

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We present the gravitational wave analyses from rotating (model s15g) and nearly non-rotating (model s15h) 3D MHD core collapse supernova simulations at bounce and during the first couple of ten milliseconds afterwards. The simulations are launched from 15 M progenitor models stemming from stellar-evolution calculations. Gravity is implemented by a spherically symmetric effective general relativistic potential. The input physics uses the Lattimer-Swesty equation of state for hot, dense matter and a neutrino parametrisation scheme that is accurate until the first few ms after bounce. The 3D simulations allow us to study features already known from 2D simulations, as well as nonaxisymmetric effects. In agreement with recent results, we find only type I gravitational wave signals at core bounce. In the later stage of the simulations, one of our models (s15g) shows nonaxisymmetric gravitational wave emission caused by a low T/|W| dynamical instability, while the other model radiates gravitational waves due to a convective instability in the protoneutron star. The total energy released in gravitational waves within the considered time intervals is 1.52 × 10 −7 M (s15g) and 4.72 × 10 −10 M (s15h). Both core collapse simulations indicate that corresponding events in our Galaxy would be detectable either by the LIGO or Advanced LIGO detector.

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“…5, which shows the cluster distribution for a chosen thermodynamic condition ( temperature T = 1.6 MeV, baryonic density ρ = 3.3 · 10 11 gcm −3 , proton fraction Y p = 0.41) which is typical for the dynamics of supernova matter after the bounce and before the propagation of the shock wave [11,12]. We can see that the dominant cluster size is around A = 60, which is a particularly important size in the process of electron capture which determines the composition of the resulting neutron star [42][43][44][45][46][47]. It is clear that it is very important to correctly compute the abundances of such nuclei.…”

Section: Phenomenological Consequences Of Ensemble In-equivalencementioning

confidence: 99%

Ensemble inequivalence in supernova matter within a simple model

Gulminelli

Raduta²

2012

Phys. Rev. C

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A simple, exactly solvable statistical model is presented for the description of baryonic matter in the thermodynamic conditions associated to the evolution of core-collapsing supernova. It is shown that the model presents a first order phase transition in the grandcanonical ensemble which is not observed in the canonical ensemble. Similar to other model systems studied in condensed matter physics, this ensemble in-equivalence is accompanied by negative susceptibility and discontinuities in the intensive observables conjugated to the order parameter. This peculiar behavior originates from the fact that baryonic matter is subject to attractive short range strong forces as well as repulsive long range electromagnetic interactions, partially screened by a background of electrons. As such, it is expected in any theoretical treatment of nuclear matter in the stellar environement. Consequences for the phenomenology of supernova dynamics are drawn.

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Nuclear input for core-collapse models

Cited by 39 publications

References 143 publications

Gravitational wave burst signal from core collapse of rotating stars

Gravitational wave burst signal from core collapse of rotating stars

Gravitational waves from 3D MHD core collapse simulations

Ensemble inequivalence in supernova matter within a simple model

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