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The Structure and Signals of Neutron Stars, from Birth to Death

24–28 Mar 2014
Europe/Rome timezone

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Session

Afternoon session - Parallel A

25 Mar 2014, 14:30

Conveners

Afternoon session - Parallel A

  • Dmitry Yakovlev (IOFFE Inst., San Petersburg)

Presentation materials

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  1. 75. Transport coefficients of nuclear matter in neutron star cores in the BHF framework
    Peter Shternin
    25/03/2014, 14:30
    We calculate shear viscosity and thermal conductivity of dense asymmetric nuclear matter in the neutron star cores. Nuclear interaction is treated in the framework of non-relativistic Brueckner-Hartree-Fock formalism. The full Argonne v18 potential with addition of the Urbana IX effective three-body forces is used. In general, in-medium effects at two-body level lead to increase of the...
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  2. 0. Transport coefficients in superfluid neutron stars
    Dr Laura Tolos (ICE (CSIC-IEEC))
    25/03/2014, 14:50
    We study the shear and bulk viscosity coefficients as well as the thermal conductivity as arising from the collisions among phonons in superfluid neutron stars. We use effective field theory techniques to extract the allowed phonon collisional processes, written as a function of the equation of state of the system. We analyze the shear viscosity taking into account the contribution of...
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  3. 22. Tests of the nuclear equation of state and superfluid and superconducting gaps using the Cassiopeia A neutron star
    Wynn Ho (U)
    25/03/2014, 15:10
    The observed rapid cooling of the Cassiopeia A neutron star can be interpreted as being caused by neutron and proton transitions from normal to superfluid/superconducting states in the stellar core. Here we present measurements of the neutron star mass and radius found from consistent fitting of both the Chandra X-ray spectra and cooling behavior; this comparison is only possible for...
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  4. 41. The neutron star in Cassiopeia A: equation of state, superfluidity, and Joule heating
    Dr Alfio Bonanno (INAF-Catania)
    25/03/2014, 15:30
    The thermomagnetic evolution of the young neutron star in Cassiopea A is studied by considering fast neutrino emission processes. In particular, we consider neutron star models obtained from the equation of state computed in the framework of the Brueckner-Bethe-Goldstone many-body theory and variational methods, and models obtained with the Akmal-Pandharipande-Ravenhall equation of state. It...
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  5. 100. Effects of superfluidity on cooling of compact stars
    Armen Sedrakian (Frankfurt University)
    25/03/2014, 15:50
    I will discuss the recent work on the effects of superfluidity of baryonic and quark matter on the cooling of compact stars. In particular I will focus on the effects of (1) pair-breaking processes on the cooling; (2) color superconductivity; and (3) the problem of the fitting of Cas A data with different models.
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  6. 53. Thermal Evolution of Compact Stars with Color Superconducting Quark Matter
    Dr Tsuneo Noda (Kurume Institute of Technology)
    25/03/2014, 16:10
    The observations of the central source of Cassiopeia A (Cas A) indicates that the compact star has large mass and high effective temperature, and suggests that its location on the cooling diagram is in the standard cooling region. There are some other compact stars which have low effective temperature, and they require an exotic phase which appears at high density, for large neutrino...
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