2001/11/21 by P. K. Sahu, G. F. Burgio, M. Baldo
Engineering · Physics and Astronomy · #Astrophysical Phenomena and Observations #Geophysics and Sensor Technology #Pulsars and Gravitational Waves Research #astro-ph #hep-ph #nucl-th
paper · pdf · doi:10.1086/339510
published as Astrophys.J. 566 (2002) L89-L92 · 10 pages, TeX, submitted to Astrophysical Journal Letters
arxiv created 2001/11/21 · openalex publication_date 2002/02/20 · arxiv updated 2009/11/30 · openalex created_date 2016/06/24 · openalex updated_date 2026/07/31
We make a first calculation of eigenfrequencies of radial pulsations of neutron stars with quark cores in a general relativistic formalism given by Chandrasekhar. The equations of state used to estimate such eigenfrequencies have been derived by taking proper care of the hadron-quark phase transition. The hadronic equations of state have been obtained in the framework of the Brueckner-Hartree-Fock and relativistic mean field theories, whereas the quark equation of state has been derived within the MIT bag model. We find that the periods of oscillation of neutron stars with quark cores show a kink that is associated with the presence of a mixed phase region. Also, the oscillation periods show significant differences between ordinary neutron stars and neutron stars with dynamical quark phases.