Volume 372, Number 2, June III 2001
|Page(s)||535 - 543|
|Section||Interstellar and circumstellar matter|
|Published online||15 June 2001|
The crust of rotating strange quark stars
N. Copernicus Astronomical Center, Polish Academy of Sciences, Bartycka 18, 00-716 Warszawa, Poland
2 Département d'Astrophysique Relativiste et de Cosmologie -UMR 8629 du CNRS, Observatoire de Paris, 92195 Meudon Cedex, France e-mail: email@example.com; firstname.lastname@example.org; Eric.Gourgoulhon@obspm.fr
Corresponding author: J. L. Zdunik, email@example.com
Accepted: 9 March 2001
Calculations of the properties of rotating strange stars with crusts are performed within the framework of general relativity. We employ an equation of state (EOS) of strange quark matter based on the MIT Bag Model with massive strange quarks and lowest order QCD interactions. The crust is described by the BPS equation of state. A significant increase of the stellar radius is found close to the Keplerian (mass-shedding limit) configuration. This leads to the disappearance of the gap between the stellar surface and the innermost stable circular orbit (ISCO) at very high rotation rates, for a rather broad range of stellar masses. The Keplerian configuration for the strange star with crust corresponds to values of J, , which are about 20% smaller than in the case of bare strange stars. Because the Keplerian configuration is achieved due to the increase of the stellar oblateness, the Keplerian frequency (of the rotation) remains almost unaltered. The lack of the gap close to the Keplerian rotation could imply a more stringent limit on , if the existence of such a gap is supported by observations, as in the source 4U 1820-30 with the upper QPO frequency 1.07 kHz. If such a constraint is taken into account (mandatory existence of a gap) the minimum is about 1 kHz even with the extreme fine tuning of strange quark matter parameters. The minimum is then obtained for the non-rotating configuration with maximum allowable mass. The maximum frequency in the stable circular orbit around the strange star with a crust is smaller by about 100 Hz than in the case of a bare strange star. During the spin-down of a magnetized strange quark star with crust, the crust matter is absorbed in the equatorial region by the strange matter core. The deconfinement of absorbed crust matter is a strongly exothermic process, which would influence the cooling curve of this compact object.
Key words: dense matter / equation of state / stars: neutron / stars: rotation / stars: binaries: general
© ESO, 2001
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