Constraining Neutron Superfluidity with R -Mode Physics

Superfluidity in relativistic neutron stars

The purpose of these notes is to give a brief review of superfluidity in neutron stars. After a short presentation explaining why and how superfluidity is expected in the crust and core of neutron stars, consequences on thermal evolution and rotational dynamics are discussed. The second part summarizes a formalism that has been recently developped to describe the hydrodynamics of superfluids or...

Superfluidity in Neutron Star Matter

Constraining Electroweak Physics

The most fundamental observable related to the weak interaction is the muon lifetime, τμ. With the electromagnetic two-loop contribution known1, τμ can be used unambiguously to extract the Fermi constant, GF = 1.16637(1)× 10 −5 GeV, where the uncertainty is completely dominated by experiment. Adding the fine structure constant, α, one can obtain two relations between the intermediate gauge boso...

Constraining New Physics with Vertex Corrections

We discuss how new physics not encompassed within the STU oblique correction framework can be constrained from precision electroweak measurements via vertex corrections to Z–pole observables. 1. Limitations of the Oblique Correction Analysis In constructing models beyond the Standard Model (SM) such as technicolor or supersymmetric theories, it is important to test their viability by looking fo...

Proton and Neutron Superfluidity in β-stable Neutron Star Matter

We investigate the effect of a microscopic three-body force on the proton and neutron superfluidity in the 1S0 channel in β-stable neutron star matter. It is found that the three-body force has only a small effect on the neutron 1S0 pairing gap, but it suppresses strongly the proton 1S0 superfluidity in β-stable neutron star matter. PACS numbers: 26.60.+c,21.65.+f, 21.30.Fe