Resonant Neutrino Spin-Flavor Precession and Supernova Nucleosynthesis and Dynamics

Details Resonant Neutrino Spin-Flavor Precession and Supernova Nucleosynthesis and Dynamics Resonant Neutrino Spin-Flavor Precession and Supernova Nucleosynthesis and Dynamics

1996-10-25

arxiv.org/abs/astro-ph/9610209v2

Phys.Rev. D55 (1997) 3265-3275

Astronomy and Astrophysics

Astrophysics

Latex file, 33 pages including 11 figures, uses psfig.sty, minor changes about wording and clarification of the text, to be pu

Scientific paper

10.1103/PhysRevD.55.3265

We discuss the effects of resonant spin-flavor precession (RSFP) of Majorana neutrinos on heavy element nucleosynthesis in neutrino-heated supernova ejecta and the dynamics of supernovae. In assessing the effects of RSFP, we explicitly include matter-enhanced (MSW) resonant neutrino flavor conversion effects where appropriate. We point out that for plausible ranges of neutrino magnetic moments and proto-neutron star magnetic fields, spin-flavor conversion of $\nu_\tau$ (or $\nu_\mu$) with a cosmologically significant mass (1--100 eV) into a light $\bar \nu_e$ could lead to an enhanced neutron excess in neutrino-heated supernova ejecta. This could be beneficial for models of $r$-process nucleosynthesis associated with late-time neutrino-heated ejecta from supernovae. Similar spin-flavor conversion of neutrinos at earlier epochs could lead to an increased shock reheating rate and, concomitantly, a larger supernova explosion energy. We show, however, that such increased neutrino heating likely will be accompanied by an enhanced neutron excess which could exacerbate the problem of the overproduction of the neutron number $N = 50$ nuclei in the supernova ejecta from this stage. In all of these scenarios, the average $\bar\nu_e$ energy will be increased over those predicted by supernova models with no neutrino mixings. This may allow the SN1987a data to constrain RSFP-based schemes.

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