Neutrino Interactions in Octet Baryon Matter

Neutrino processes caused by the neutral current are studied in octet baryon matter. Previous confusion about the baryonic matrix elements of the neutral current interaction is excluded, and a correct table for them improved by consideration of the proton spin problem is presented instead.Comment: 6 page

Occurrence of Hyperon Superfluidity in Neutron Star Cores

Superfluidity of $\Lambda$ and $\Sigma^-$ admixed in neutron star (NS) cores is investigated realistically for hyperon ($Y$)-mixed NS models obtained using a $G$-matrix-based effective interaction approach. Numerical results for the equation of state (EOS) with the mixing ratios of the respective components and the hyperon energy gaps including the temperature dependence are presented. These are meant to serve as physical inputs for $Y$-cooling calculations of NSs. By paying attention to the uncertainties of the EOS and the $YY$ interactions, it is shown that both $\Lambda$ and $\Sigma^-$ are superfluid as soon as they appear although the magnitude of the critical temperature and the density region where superfluidity exists depend considerably on the $YY$ pairing potential. Considering momentum triangle condition and the occurrence of superfluidity, it is found that a so-called `` hyperon cooling\rq\rq~(neutrino-emission from direct Urca process including $Y$) combined with $Y$-superfluidity may be able to account for observations of the colder class of NSs. It is remarked that $\Lambda$-hyperons play a decisive role in the hyperon cooling scenario. Some comments are given regarding the consequences of the less attractive $\Lambda\Lambda$ interaction recently suggested by the `` NAGARA event\rq\rq~$^6_{\Lambda\Lambda}$He.Comment: 25 pages, 12figures; final version; will appear in Prog. THeor. Phys. Vol.115, No.

Neutrino emission due to Cooper pairing of protons in cooling neutron stars: Collective effects

The process of neutrino-pair radiation due to formation and breaking of Cooper pairs of protons in superconducting cores of neutron stars is considered with taking into account of the electromagnetic coupling of protons to ambient electrons. It is shown that plasma polarization strongly modifies the effective vector weak current of protons. Collective response of ambient electrons to the proton quantum transition contributes coherently to the complete interaction with the neutrino field and enhances the rate of neutrino-pair production by two orders of magnitude.Comment: 11 pages, 2 figure

Quark description of the Nambu-Goldstone bosons in the color-flavor locked phase

We investigate the color-singlet order parameters and the quark description of the Nambu-Goldstone (NG) bosons in the color-flavor locked (CFL) phase. We put emphasis on the NG boson (phason) called ``H'' associated with the $\mathrm{U_B(1)}$ symmetry breaking. We qualitatively argue the nature of H as the second sound in the hydrodynamic regime. We articulate, based on a diquark picture, how the structural change of the condensates and the associated NG bosons occurs continuously from hadronic to CFL quark matter if the quark-hadron continuity is realized. We sharpen the qualitative difference between the flavor octet pions and the singlet phason. We propose a conjecture that superfluid H matter undergoes a crossover to a superconductor with tightly-bound diquarks, and then a crossover to superconducting matter with diquarks dissociated.Comment: 14 pages, 1 table, 1 figure and confusing statements are correcte

Neutrino Emission from Superfluid Neutron-Star Cores: Various Types of Neutron Pairing

We calculate and provide analytic fits of the factors which describe the reduction of the neutrino emissivity of modified Urca and nucleon-nucleon bremsstrahlung processes by superfluidity of neutrons and protons in neutron-star cores. We consider $^1$S$_0$ pairing of protons and either $^1$S$_0$ or $^3$P$_2$ pairing of neutrons. We analyze two types of $^3$P$_2$ pairing: the familiar pairing with zero projection of the total angular momentum of neutron pairs onto quantization axis, $m_J=0$; and the pairing with $|m_J|=2$ which leads to the gap with nodes at the neutron Fermi surface. Combining the new data with those available in the literature we fully describe neutrino emission by nucleons from neutron star cores to be used in simulations of cooling of superfluid neutron stars.Comment: 14 pages, 6 figures, A&A, accepte

Confronting Neutron Star Cooling Theories with New Observations

With the successful launch of Chandra and XMM/Newton X-ray space missions combined with the lower-energy band observations, we are in the position where careful comparison of neutron star cooling theories with observations will make it possible to distinguish among various competing theories. For instance, the latest theoretical and observational developments already exclude both nucleon and kaon direct URCA cooling. In this way we can now have realistic hope for determining various important properties, such as the composition, degree of superfluidity, the equation of state and steller radius. These developments should help us obtain better insight into the properties of dense matter.Comment: 11 pages, 1 figur

Baryon superfluidity and neutrino emissivity of neutron stars

For neutron stars with hyperon-mixed core, neutrino emissivity is studied under the equation of state, obtained by introducing repulsive three-body force universal for all baryons so as to assure the maximum mass compatible with the observation. By paying attention to the density-dependence of critical temperatures of baryon superfluids, which reflect the nature of baryon-baryon interaction and control neutron star cooling, we show what neutrino emission processes are efficient in the regions with and without hyperon mixing and remark its implications related to neutron star cooling.Comment: 5pages, 4 figure