Rotating hybrid stars with the Dyson-Schwinger quark model

Abstract

We study rapidly rotating hybrid stars with the Dyson-Schwinger model for quark matter and the Brueckner-Hartree-Fock many-body theory with realistic two-body and three-body forces for nuclear matter. We determine the maximum gravitational mass, equatorial radius, and rotation frequency of stable stellar configurations by considering the constraints of the Keplerian limit and the secular axisymmetric instability, and compare with observational data. We also discuss the rotational evolution for constant baryonic mass, and find a spinup phenomenon for supramassive stars before they collapse to black holes.

9 pages,9 figures

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Cited by in corpus (10)

• GW190814's secondary component with mass $(2.50-2.67)$ M${}_{\odot }$ as a super-fast pulsar
• Neutron star universal relations with microscopic equations of state
• The application of the Quark-Hadron Chiral Parity-Doublet Model to neutron star matter
• Effects of $\varphi$-meson on properties of hyperon stars in density dependent relativistic mean field model
• Strange quark stars within proper time regularized (2+1)-flavor NJL model
• The equation of state and radial oscillations of neutron stars
• Effects of hadron-quark phase transition on properties of Neutron Stars
• Non-radial oscillations and gravitational wave emission of hybrid neutron stars
• Rotating Neutron Stars with the Relativistic Ab Initio Calculations
• Influence of light quark loops on the Wigner phase with Dyson-Schwinger equations approach