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Astron. Astrophys. 357, 968-976 (2000)

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Deconfinement transition in rotating compact stars

E. Chubarian 1, H. Grigorian 1,2, G. Poghosyan 1 and D. Blaschke 2

1 Yerevan State University, Department of Physics, Alex Manoogian Str. 1, 375025 Yerevan, Armenia
2 Universität Rostock, Fachbereich Physik, Universitätsplatz 1, 18051 Rostock, Germany (blaschke@darss.mpg.uni-rostock.de)

Received 1 February 2000 / Accepted 15 February 2000


Using the formalism of general relativity for axially symmetric gravitational fields and their sources - rotating compact stars - a perturbation theory with respect to angular velocity is developed and physical quantities such as mass, shape, momentum of inertia and total energy of the star are defined. The change of the internal structure of the star due to rotation has been investigated and the different contributions to the moment of inertia have been evaluated separately. Numerical solutions have been performed using a two-flavor model equation of state describing the deconfinement phase transition as constrained by the conservation of total baryon number and electric charge. During the spin down evolution of the rotating neutron star, below critical values of angular velocity a quark matter core can appear which might be detected as a characteristic signal in the pulsar timing. Within the spin-down scenario due to magnetic dipole radiation it is shown that the deviation of the braking index from [FORMULA] could signal not only the occurrence but also the size of a quark core in the pulsar. A new scenario is proposed where, due to mass accretion onto the rapidly rotating compact star, a spin-down to spin-up transition might signal a deconfinement transition in its interior.

Key words: dense matter – stars: evolution – stars: interiors – stars: neutron – stars: rotation

Send offprint requests to: D. Blaschke

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© European Southern Observatory (ESO) 2000

Online publication: June 5, 2000