CONSTRAINING NEUTRON STAR MATTER WITH QUANTUM CHROMODYNAMICS

Superfluidity in Neutron Star Matter

Baryon Asymmetry, Dark Matter and Quantum Chromodynamics

We propose a new scenario to explain the observed cosmological asymmetry between matter and antimatter, based on nonperturbative physics at the QCD scale. Our scenario relies on a mechanism of separation of matter and antimatter which would be in two different phases: conventional hadronic phase and novel, color superconducting phase. We argue that chunks of quarks or antiquarks in condensed co...

Constraining the neutron star equation of state using XMM - Newton

We have identified three possible ways in which future XMM-Newton observations can provide significant constraints on the equation of state of neutron stars. First, using a long observation of the neutron star X-ray transient Cen X–4 in quiescence one can use the RGS spectrum to constrain the interstellar extinction to the source. This removes this parameter from the X-ray spectral fitting of t...

Constraining Population Synthesis Models via the Binary Neutron Star Population

The observed sample of double neutron-star (NS-NS) binaries presents a challenge to populationsynthesis models of compact object formation: the parameters entering into these models must be carefully chosen so as to match (i) the observed star formation rate and (ii) the formation rate of NS-NS binaries, which can be estimated from the observed sample and the selection effects related to the di...

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