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opacityκ p,i for neutrinoνas κp,i = R dϵ ϵ 2+iκp(ϵ)feq ν (ϵ, T, ην)R dϵ ϵ 2+ifeq ν (ϵ, T, ην) = 4π (hc)3 1 Bi(T, ην) Z dϵ ϵ 2+iκp(ϵ)feq ν (ϵ, T, ην), (A7) which automatically satisfies the Kirchhoff’s law for number, energy emission rate · 2018

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astro-ph.HE 1

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2026 1

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UNVERDICTED 1

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Consistent Treatment of Muons in Binary Neutron Star Mergers

astro-ph.HE · 2026-04-14 · unverdicted · novelty 5.0

Binary neutron star merger simulations with consistent muon treatment show ejecta masses reduced by at most 17% while average electron fractions, velocities, and temperatures differ by less than 6% from non-muonic cases.

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  • Consistent Treatment of Muons in Binary Neutron Star Mergers astro-ph.HE · 2026-04-14 · unverdicted · none · ref 11

    Binary neutron star merger simulations with consistent muon treatment show ejecta masses reduced by at most 17% while average electron fractions, velocities, and temperatures differ by less than 6% from non-muonic cases.