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XQCD 2019 (The 17th International Conference on QCD in Extreme Conditions)

24–26 Jun 2019
Bunkyo School Building, Tokyo Campus, University of Tsukuba
Japan timezone

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Session

Session 2

24 Jun 2019, 11:05
122, 134 (Bunkyo School Building, Tokyo Campus, University of Tsukuba)

122, 134

Bunkyo School Building, Tokyo Campus, University of Tsukuba

3-29-1 Otsuka Bunkyo-ku Tokyo 112-0012 Japan

Conveners

Session 2

  • Muneto Nitta (Keio University)

Presentation materials

There are no materials yet.

  1. 51. The interpolation approach to dense QCD and neutron-star phenomenology
    Dr Tyler Gorda (University of Virginia)
    24/06/2019, 11:05
    Invited talk
    Neutron stars (NSs) contain the densest observable matter in the universe. Within their cores lies QCD matter compressed to multiple times the density of common nuclei. Unfortunately, this matter is too dense to be studied from first-principles nuclear-physics calculations, and not dense enough to be studied using first-principles perturbative-QCD calculations. In this talk, I will detail a...
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  2. 11. Neutron star equations of state and quark-hadron continuity
    Prof. Toru Kojo (Central China Normal University)
    24/06/2019, 11:50
    Oral talk
    The properties of dense QCD matter are delineated through the construction of equations of state which should be consistent with QCD calculations in the low and high density limits, nuclear laboratory experiments, and the neutron star observations. These constraints, together with the causality condition of the sound velocity, are used to develop the picture of hadron-quark continuity in which...
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  3. 25. Rotating neutron star in strong magnetic fields and the MR relations
    Ms Chinatsu Watanabe (Saitama University)
    24/06/2019, 12:15
    Oral talk
    Neutron stars are highly magnetized rotating compact stars. In 2010, a neutron star named PSR J1614-2230 has a mass of twice the solar mass (1.97$\pm$0.04M$\odot$). In 2013, a neutron star named PSR J0348+0432 with a mass of 2.01$\pm$0.04M$\odot$ was observed. Such massive neutron stars give strong constraints on the equation of state (EoS) of neutron star matter. In this study, we calculate...
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