Strange stars with realistic quark vector interaction and phenomenological density-dependent scalar potential

Dey, Mira; Bombaci, Ignazio; Dey, Jishnu; Ray, Subharthi; Samanta, B.C.

doi:10.1016/s0370-2693(98)00935-6

Cited by 324 publications

(387 citation statements)

References 21 publications

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“…In this model the quark interaction is described by an interquark vector potential originating from gluon exchange and by a density-dependent scalar potential that restores the chiral symmetry at high density. Using the same model (with the parameterization [Dey et al 1998, erratum] denoted as SS1 and SS2), 8 we calculated the M-R relations, which are also shown by solid curves labeled SS1 and SS2 in Figure 1, corresponding to strange stars with maximum masses of 1.44 and 1.32 M , and radii of 7.07 and 6.53 7 There are actually two solutions of eq. (7) with given I and M; one serves as the upper limit of R and the other the lower limit of R. But the former solution gives an unphysically small radius and is rejected.…”

Section: The Mass-radius Relation For 4u 1728ϫ34mentioning

confidence: 99%

“…Recently, Dey et al (1998) derived an EOS for strange matter that has asymptotic freedom built in, shows confinement at zero baryon density and deconfinement at high density, and gives a stable configuration for chargeless, b-stable strange matter. In this model the quark interaction is described by an interquark vector potential originating from gluon exchange and by a density-dependent scalar potential that restores the chiral symmetry at high density.…”

Section: The Mass-radius Relation For 4u 1728ϫ34mentioning

confidence: 99%

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On the Nature of the Compact Star in 4U 1728−34

Ray

Dey

et al. 1999

The Astrophysical Journal

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The discovery of kilohertz quasi-periodic oscillations (kHz QPOs) in low-mass X-ray binaries (LMXBs) with the Rossi X-Ray Timing Explorer has stimulated extensive studies of these sources. Recently, Osherovich & Titarchuk suggested a new model for kHz QPOs and the related correlations between kHz QPOs and lowfrequency features in LMXBs. Here we use their results to study the mass-radius relation for the atoll source 4U 1728Ϫ34. We find that, if this model is correct, 4U 1728Ϫ34 is possibly a strange star rather than a neutron star.

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Section: The Mass-radius Relation For 4u 1728ϫ34mentioning

confidence: 99%

Section: The Mass-radius Relation For 4u 1728ϫ34mentioning

confidence: 99%

On the Nature of the Compact Star in 4U 1728−34

Ray

Dey

et al. 1999

The Astrophysical Journal

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“…The two curves SSI and SS2 in Fig. 1 give the MR relation for strange stars calculated with the EOS by Dey et al (1998). Figure 1 clearly demonstrates that a strange star model is more compatible with SAX J 1808.4-3658 than a neutron star one.…”

Section: Strange Star Candidatesmentioning

confidence: 74%

“…4-3658 (Li et al 1999a), the atoll X-ray source 4U 1728-34 (Li et al 1999b), the X-ray burster 4U 1820-30 (Bombaci 1997), the X-ray pulsar Her X-l (Dey et al 1998), and the hard X-ray burster GRO J1744-28 (Cheng et al 1998) are good strange star candidates. If the compact objects in these X-ray sources are really strange stars, then there will be very deep consequences for both astrophysics and the physics of strong interactions.…”

Section: Strange Star Candidatesmentioning

confidence: 99%

Are there Strange Stars in the Universe?

Bombaci

2000

International Astronomical Union Colloquium

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A b s t r a c t . Strange stars could represent a new class of stellar compact objects, where a new phase of dense matter (deconfined strange quark matter) comes into play. Here, we discuss some possible observational evidence for their existence. IntroductionStrange stars (SS) are hypothetical astrophysical compact objects which are made entirely of deconfined u,d,s quark matter (strange quark matter). The possible existence of SS is a direct consequence of the conjecture (Bodmer 1971, Witten 1984) that strange quark matter may be the absolute ground state of strong interacting matter rather than 5 6 Fe. Since this hypothesis was formulated, strange stars have been studied by many authors, but they remained purely theoretical entities. Strange star candidatesRecent studies have shown that the compact objects associated with the transient X-ray burster SAX J1808. 4-3658 (Li et al. 1999a), the atoll X-ray source 4U 1728-34 (Li et al. 1999b), the X-ray burster 4U 1820-30 (Bombaci 1997), the X-ray pulsar Her X-l (Dey et al. 1998), and the hard X-ray burster GRO J1744-28 (Cheng et al. 1998) are good strange star candidates. If the compact objects in these X-ray sources are really strange stars, then there will be very deep consequences for both astrophysics and the physics of strong interactions.As a particular example here we consider the case of the transient X-ray burst source SAX J1808.4-3658. This source contains a millisecond X-ray pulsar with a period of 2.49 milliseconds.Using the observed X-ray luminosities, Li et al. (1999a) derived a firm upper limit on the radius R of the compact object in SAX J 1808.4-3658 given by the dashed curve in the mass-radius (MR) plane in Fig. 1. The dotted curve in Fig. 1 represents the Schwarzschild radius 2GM/c 2 , which is a lower limit of the stellar radius to prevent the star collapsing to a black hole. Thus the allowed range of the mass and radius of SAX J1808.4-3658 is the region confined by the dashed and dotted curves in Fig. 1. In the same figure, we report the theoretical MR relations (solid curves) for neutron stars given by five recent realistic models for the EOS of dense matter. Models UU, BBBl and BBB2 are relative to 659 terms of use, available at https://www.cambridge.org/core/terms. https://doi

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“…Equations of state N1, N2, and PC are not modern (i.e., not fitted to the most current nuclear scattering data), but are included for easy comparison to previous work on equation of state constraints. Curve S1 is for a compact strange star (Dey et al 1998), whereas curve S2 is for a more standard strange star equation of state (Zdunik 2000). Curve Q is a quark matter equation of state with a Gaussian form factor and a diquark condensate (kindly provided by David Blaschke and Hovik Gregorian).…”

Section: Results: Vela X-1mentioning

confidence: 99%

Constraints on Superdensematter From X-Ray Binaries

Miller

2006

NATO Science Series II: Mathematics, Physics and Chemistry

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From the earliest measurements of the masses of binary pulsars, observations of neutron stars have placed interesting constraints on the properties of high-density matter. The last few years have seen a number of observational developments that could place strong new restrictions on the equilibrium state of cold matter at supranuclear densities. We review these astronomical constraints and their context, and speculate on future prospects.

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Strange stars with realistic quark vector interaction and phenomenological density-dependent scalar potential

Cited by 324 publications

References 21 publications

On the Nature of the Compact Star in 4U 1728−34

On the Nature of the Compact Star in 4U 1728−34

Are there Strange Stars in the Universe?

Constraints on Superdensematter From X-Ray Binaries

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