Constraining quark-hadron interface tension in the multi-messenger era. (arXiv:1902.08766v1 [hep-ph])
<a href="http://arxiv.org/find/hep-ph/1/au:+Xia_C/0/1/0/all/0/1">Cheng-Jun Xia</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Maruyama_T/0/1/0/all/0/1">Toshiki Maruyama</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Yasutake_N/0/1/0/all/0/1">Nobutoshi Yasutake</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Tatsumi_T/0/1/0/all/0/1">Toshitaka Tatsumi</a>
We study the interface effects of quark-hadron mixed phase in compact stars.
The properties of nuclear matter are obtained based on the
relativistic-mean-field model. For the quark phase, we adopt perturbation model
with running quark masses and coupling constant. At certain choices of
parameter sets, it is found that varying the quark-hadron interface tension
will have sizable effects on the radii ($Delta R approx 600$ m) and tidal
deformabilities ($Delta Lambda/Lambda approx 50%$) of hybrid stars. These
provide possibilities for us to constrain the quark-hadron interface tension
with future gravitational wave observations as well as the ongoing NICER
mission.
We study the interface effects of quark-hadron mixed phase in compact stars.
The properties of nuclear matter are obtained based on the
relativistic-mean-field model. For the quark phase, we adopt perturbation model
with running quark masses and coupling constant. At certain choices of
parameter sets, it is found that varying the quark-hadron interface tension
will have sizable effects on the radii ($Delta R approx 600$ m) and tidal
deformabilities ($Delta Lambda/Lambda approx 50%$) of hybrid stars. These
provide possibilities for us to constrain the quark-hadron interface tension
with future gravitational wave observations as well as the ongoing NICER
mission.
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