Article

Relativistic hybrid stars with super-strong toroidal magnetic fields: An evolutionary track with QCD phase transition

10/2009; DOI:abs/0910.0327
Source: arXiv

ABSTRACT We investigate structures of hybrid stars, which feature quark core surrounded by a hadronic matter mantle, with super-strong toroidal magnetic fields in full general relativity. Modeling the equation of state (EOS) with a first order transition by bridging the MIT bag model for the description of quark matter and the nuclear EOS by Shen et al., we numerically construct thousands of the equilibrium configurations to study the effects of the phase transition. It is found that the appearance of the quark phase can affect distributions of the magnetic fields inside the hybrid stars, making the maximum field strength about up to 30 % larger than for the normal neutron stars. Using the equilibrium configurations, we explore the possible evolutionary paths to the formation of hybrid stars due to the spin-down of magnetized rotating neutron stars. We find that the energy release by the phase transition to the hybrid stars is quite large ($\la 10^{52} \rm erg$) even for super strongly magnetized compact stars. Our results suggest that the strong gravitational-wave emission and the sudden spin-up signature could be observable signals of the QCD phase transition, possibly for a source out to Megaparsec distances. Comment: 17 pages, 10 figures. accepted to MNRAS

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Keywords

10 figures

compact stars

energy release

feature quark core

first order transition

full general relativity

hybrid stars

magnetic fields

Megaparsec distances

MIT bag model

normal neutron stars

nuclear EOS

phase transition

possible evolutionary paths

QCD phase transition

quark phase

rotating neutron stars

strong gravitational-wave emission

super-strong toroidal magnetic fields