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Beta equilibrium in neutron star mergers

Mar 1, 2018

12 pages

Published in:

Phys.Rev.C 98 (2018) 6, 065806

Published: Dec 28, 2018

e-Print:

1803.00662 [nucl-th]

DOI:

10.1103/PhysRevC.98.065806

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Abstract: (APS)

We show that the commonly used criterion for β equilibrium in neutrino-transparent dense nuclear matter becomes invalid as temperatures rise above 1 MeV. Such temperatures are attained in neutron-star mergers. By numerically computing the relevant weak-interaction rates we find that the correct criterion for β equilibrium requires an isospin chemical potential that can be as large as 10–20 MeV, depending on the temperature at which neutrinos become trapped.

Note:

Section on neutrino mean free paths added. Discussion and plot of effect of isospin chemical potential on beta-equilibrium proton fraction added

Nuclear Astrophysics
potential: chemical
neutron star
weak interaction
nuclear matter: equation of state
Fermi surface
temperature: low
baryon: density
neutrino: production
Urca process

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Figures(8)

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