REVIEW 4 cited by
Boltzmann equations for neutrinos with flavor mixings
Not yet reviewed by Pith; the record is open.
This paper has not been read by Pith yet. Machine review is queued; the pith claim, tier, and objections will appear here once it completes.
SPECIMEN: schema-true, not a live event
T0 review · schema-true
One-sentence machine reading of the paper's core claim.
pith:XXXXXXXX · record.json · timestamp
Signed reviews
read the original abstract
With a view of applications to the simulations of supernova explosion and proto neutron star cooling, we derive the Boltzmann equations for the neutrino transport with the flavor mixing based on the real time formalism of the nonequilibrium field theory and the gradient expansion of the Green function. The relativistic kinematics is properly taken into account. The advection terms are derived in the mean field approximation for the neutrino self-energy whiles the collision terms are obtained in the Born approximation. The resulting equations take the familiar form of the Boltzmann equation with corrections due to the mixing both in the advection part and in the collision part. These corrections are essentially the same as those derived by Sirera et al. for the advection terms and those by Raffelt et al. for the collision terms, respectively, though the formalism employed here is different from theirs. The derived equations will be easily implemented in numerical codes employed in the simulations of supernova explosions and proto neutron star cooling.
Forward citations
Cited by 4 Pith papers
-
Collective flavor conversions are interactions of neutrinos with quantized flavor waves
Neutrino fast flavor instabilities are equivalent to stimulated emission of flavomons, quantum flavor waves, whose kinetic equations reproduce the linear growth rate and extend naturally beyond it.
-
Theory of neutrino slow flavor evolution. Part I. Homogeneous medium
Slow neutrino flavor instabilities split into a new resonant small-scale branch with growth rate ~omega_E/epsilon and the familiar non-resonant branch with the traditional scale 1/sqrt(omega_E mu).
-
Theory of neutrino slow flavor evolution. Part II. Space-time evolution of linear instabilities
All weak fast and slow neutrino flavor instabilities are convective, so they grow spatially along neutrino directions rather than locally in time.
-
Fast Flavor Pendulum: Instability Condition
The Nyquist criterion for homogeneous fast flavor instability is corrected to N = W - Ns/2, where W is the subluminal winding number and Ns counts real superluminal solutions.
Discussion (0). Continue with ORCID to comment.