2015/03/13 by N. Yasutake, Yasutake, N., S. Benic +7
Physics and Astronomy · #FOS: Physical sciences #High Energy Astrophysical Phenomena (astro-ph.HE) #Nuclear Theory (nucl-th) #astro-ph.HE #nucl-th
paper · pdf · doi:10.48550/arxiv.1503.03933
3 pages, 1 figure. Proceeding of "Quarks and Compact Stars 2014 Beijing"
arxiv created 2015/03/23 · arxiv updated 2015/03/24
We study the quark-hadron phase transition with the finite-size effects in neutron stars. The finite-size effects should be, generally, taken into account in the phase transition of multi-component system. The behavior of the phase transition, however, strongly depends on the models for quark and hadron matter, surface tension, neutrino fraction, and temperature. We find that, if the surface tension is strong, the EOS becomes similar to the case of a Maxwell construction for any hadron and/or quark model, though we adopt the Gibbs conditions. We also find that the mass-radius relations for that EOS are consistent with the observations, and our model is then applicable to realistic astrophysical phenomena such as the thermal evolution of compact stars.