Conservative special relativistic radiative transfer for multidimensional astrophysical simulations: motivation and elaboration

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dc.creatorCardall, Christian Y.
dc.creatorLentz, Eric J.
dc.creatorMezzacappa, Anthony
dc.date2005-10-25
dc.date.accessioned2026-07-07T06:44:01Z
dc.date.available2026-07-07T06:44:01Z
dc.descriptionMany astrophysical phenomena exhibit relativistic radiative flows. While velocities in excess of $v \sim 0.1c$ can occur in these systems, it has been common practice to approximate radiative transfer to $\cO(v/c)$. In the case of neutrino transport in core-collapse supernovae, this approximation gives rise to an inconsistency between the lepton number transfer and lab frame energy transfer, which have different $\cO(v/c)$ limits. A solution used in spherically symmetric $\cO(v/c)$ simulations has been to retain, for energy accounting purposes, the $\cO(v^2/c^2)$ terms in the lab frame energy transfer equation that arise from the $\cO(v/c)$ neutrino number transport equation. Avoiding the proliferation of such ``extra'' $\cO(v^2/c^2)$ terms in the absence of spherical symmetry motivates a special relativistic formalism, which we exhibit in coordinates sufficiently general to encompass Cartesian, spherical, and cylindrical coordinate systems.
dc.description9 pages
dc.identifierhttps://arxiv.org/abs/astro-ph/0510702
dc.identifierhttp://arxiv.org/abs/astro-ph/0510702
dc.identifierPhys. Rev. D 72, 043007 (2005)
dc.identifierdoi:10.1103/PhysRevD.72.043007
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/102633
dc.subjectAstrophysics
dc.titleConservative special relativistic radiative transfer for multidimensional astrophysical simulations: motivation and elaboration
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