0000000000880994

AUTHOR

Bruno Peres

showing 2 related works from this author

General relativistic neutrino transport using spectral methods

2014

We present a new code, Lorene's Ghost (for Lorene's gravitational handling of spectral transport) developed to treat the problem of neutrino transport in supernovae with the use of spectral methods. First, we derive the expression for the nonrelativistic Liouville operator in doubly spherical coordinates (r, theta, phi, epsilon, Theta, Phi)$, and further its general relativistic counterpart. We use the 3 + 1 formalism with the conformally flat approximation for the spatial metric, to express the Liouville operator in the Eulerian frame. Our formulation does not use any approximations when dealing with the angular arguments (theta, phi, Theta, Phi), and is fully energy-dependent. This approa…

PhysicsHigh Energy Astrophysical Phenomena (astro-ph.HE)[PHYS]Physics [physics]Chebyshev polynomialsPhysics and Astronomy (miscellaneous)010308 nuclear & particles physicsSpherical coordinate systemFOS: Physical sciences01 natural sciencesGravitation0103 physical sciencesSchwarzschild metricNeutrinoAstrophysics - High Energy Astrophysical PhenomenaSpectral methodRelativistic quantum chemistry[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]010303 astronomy & astrophysicsFourier seriesComputingMilieux_MISCELLANEOUSMathematical physics
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Influence of pions and hyperons on stellar black hole formation

2013

We present numerical simulations of stellar core-collapse with spherically symmetric, general relativistic hydrodynamics up to black hole formation. Using the CoCoNuT code, with a newly developed grey leakage scheme for the neutrino treatment, we investigate the effects of including pions and \Lambda-hyperons into the equation of state at high densities and temperatures on the black hole formation process. Results show non-negligible differences between the models with reference equation of state without any additional particles and models with the extended ones. For the latter, the maximum masses supported by the proto-neutron star are smaller and the collapse to a black hole occurs earlie…

High Energy Astrophysical Phenomena (astro-ph.HE)Physics[PHYS]Physics [physics]Nuclear and High Energy PhysicsNuclear Theory010308 nuclear & particles physicsAstrophysics::High Energy Astrophysical PhenomenaFOS: Physical sciencesPrimordial black holeAstrophysics01 natural sciencesNuclear Theory (nucl-th)Black holeBinary black holeRotating black holeIntermediate-mass black hole0103 physical sciencesExtremal black holeStellar black holeQ starAstrophysics - High Energy Astrophysical Phenomena[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]010303 astronomy & astrophysicsComputingMilieux_MISCELLANEOUSPhys. Rev. D., 87, id.043006 (2013)
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