J. C. D’Olivo

Bound on the neutrino magnetic moment from chirality flip in supernovae

For neutrinos with a magnetic moment, we show that the collisions in a hot and dense plasma act as an efficient mechanism for the conversion of

Neutrino oscillation mechanism for pulsar kicks reexamined

\nu_L

UHE neutrino damping in a thermal gas of relic neutrinos

into

First Direct-Detection Constraints on eV-Scale Hidden-Photon Dark Matter with DAMIC at SNOLAB

\nu_R

Nucleon contribution to the neutrino electromagnetic vertex in matter

. The production rate for right-handed neutrinos is computed in terms of a resummed photon propagator which consistently incorporates the background effects. Assuming that the entire energy in a supernova collapse is not carried away by the

Damping rate of a fermion in a medium

\nu_R

Neutrinos in a gravitational background: A test for the universality of the gravitational interaction

, our results can be used to place an upper limit on the neutrino magnetic moment

Violation of the equivalence principle oscillation solutions to the solar neutrino problem

\mu_\nu < (0.1-0.4)\times 10^{-11}\mu_B

Neutrino damping rate at finite temperature and density

Anisotropic neutrino emission during the neutron star formation can be the origin of the observed proper motions of pulsars. We derive a general expression for the momentum asymmetry in terms of the neutrino energy flux gradient, and show that a nonvanishing effect is induced at the lowest order by a deformed neutrinosphere. In particular, this result is valid for a neutrino flux transported through a spherical atmosphere with constant luminosity.