Vertex renormalization of weak interactions in compact stars: beyond leading order

TL;DR

This paper calculates the neutrino emission rate in neutron stars considering higher-order effects in weak interactions, revealing a modest enhancement over previous estimates.

Contribution

It introduces a vertex renormalization approach to compute neutrino emissivity beyond leading order in Fermi velocity in neutron star matter.

Findings

Neutrino emissivity is increased by up to 10% at v_F<0.4.

Full vertex calculations include resummed series in particle-hole channels.

Higher-order corrections are significant for accurate modeling of neutron star cooling.

Abstract

Neutrino emission rate from baryonic matter in neutron stars via weak neutral vector interaction is computed up to order O(v_F^6), where v_F is the Fermi velocity in units of speed of light. The vector current polarization tensors are evaluated with full vertices which include resummed series in the particle-hole channel. The neutrino emissivity is enhanced compared to the O(v_F^4) order up of 10% for values v_F< 0.4 characteristic to baryons in compact stars.