Medium modification of the charged current neutrino opacity and its implications - INSPIRE

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Medium modification of the charged current neutrino opacity and its implications

L.F. Roberts
(
- UC, Santa Cruz and
- Caltech
)
,
Sanjay Reddy
(
- Washington U., Seattle
)
,
Gang Shen
(
- Washington U., Seattle
)

May, 2012

8 pages

Published in:

Phys.Rev.C 86 (2012) 065803

e-Print:

1205.4066 [astro-ph.HE]

DOI:

10.1103/PhysRevC.86.065803

Report number:

INT-PUB-12-024

View in:

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Abstract: (arXiv)

Previous work on neutrino emission from proto-neutron stars which employed full solutions of the Boltzmann equation showed that the average energies of emitted electron neutrinos and antineutrinos are closer to one another than predicted by older, more approximate work. This in turn implied that the neutrino driven wind is proton rich during its entire life, precluding

r

-process nucleosynthesis and the synthesis of Sr, Y, and Zr. This work relied on charged current neutrino interaction rates that are appropriate for a free nucleon gas. Here, it is shown in detail that the inclusion of the nucleon potential energies and collisional broadening of the response significantly alters this conclusion. Iso-vector interactions, which give rise to the nuclear symmetry energy, produce a difference between the neutron and proton single-particle energies

\Delta U=U_n-U_p

and alter the kinematics of the charged current reactions. In neutron-rich matter, and for a given neutrino/antineutrino energy, the rate for

\nu_e+n\rightarrow e^-+p

is enhanced while

\bar{\nu}_e+p\rightarrow n+e^+

is suppressed because the

Q

value for these reactions is altered by

\pm\Delta U

, respectively. In the neutrino decoupling region, collisional broadening acts to enhance both

\nu_e

and

\bar{\nu}_e

cross-sections and RPA corrections decrease the

\nu_e

cross-section and increase the

\bar \nu_e

cross-section, but mean field shifts have a larger effect. Therefore, electron neutrinos decouple at lower temperature than when the nucleons are assumed to be free and have lower average energies. The change is large enough to allow for a reasonable period of time when the neutrino driven wind is predicted to be neutron rich. It is also shown that the electron fraction in the wind is influenced by the nuclear symmetry energy.

Note:

Version submitted to PRC, 10 pages, 6 figures (Additional discussion of RPA effects added)

26.50.+x
21.65.Mn
26.60.-c
95.85.Ry
energy: symmetry
neutrino: interaction
antineutrino: energy
neutrino: decoupling
neutrino: opacity
potential: energy

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