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Strange stars (ReSS) calculated from a realistic equation of state (EOS), that incorporate chiral symmetry restoration as well as deconfinement at high density [Phys. Lett. B 438 (1998) 123; Phys. Lett. B 447 (1999) 352, Addendum; Phys. Lett. B 467 (1999) 303, Erratum; Indian J. Phys. B 73 (1999) 377] show compact objects in the mass radius curve. We compare our calculations of incompressibility for this EOS with that of nuclear matter. One of the nuclear matter EOS has a continuous transition to ud-matter at about five times normal density. Another nuclear matter EOS incorporates density dependent coupling constants. From a look at the consequent velocity of sound, it is found that the transition to ud-matter seems necessary. © 2004 Elsevier B.V. All rights reserved.

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Physics Letters, Section B: Nuclear, Elementary Particle and High-Energy Physics

Incompressibility of strange matter

Recently the μΔ++ was found from a fit to π+p scattering [G.L. Castro, A. Mariano, Phys. Lett. B 517 (2002) 339] 3391. This enable us to pinpoint condensate parameters more precisely in the context of QCD sum rules (QCDSR). In the octet sector, the Coleman-Glashow sum rule (CGSR) [S. Coleman, S.L. Glashow, Phys. Rev. Lett. 6 (1961) 423] is violated by the experimental μ-s. QCDSR allows us to write down two sum rules similar to the CGSR, which are obeyed by the experimental magnetic moments, whereas they rule out a specific model using the Wilson loop approach and a particular chiral quark model. It is amusing to note that the QCDSR allows us to write down the quark and gluon condensates in terms of measurables like the μ-s of the nucleons and the Σ±. © 2003 Published by Elsevier Science B.V.

Two new sum rules for octet-baryon magnetic moments (μ) and constraints on QCD sum rules from new experimental determination of μ-s for the decuplet

Skin vibration of ReSS and consequent resonance absorption can account for the absorption lines in the spectrum of X-ray emission from many compact stellar objects and in particular, the stars J1210-5226 and RXJ1856-3754. Observations of the X-ray spectrum of these stars is difficult to explain, if they are neutron stars.

Modern Physics Letters A

Have we observed the skin vibration of realistic strange stars (ReSS)?

X-ray bursts from compact stars are believed to be a result of Type I thermonuclear processes which are short-lived, typically ∼10 to 100 s. There are some low mass X-ray binaries, such as 4U 1820-30, 4U 1636-53, KS1731-260 and Serpens X-1, known as super bursters (SBs) which emit X-rays close to the Eddington luminosity limit for long periods of several hours. Recently, there have been reports of some long bursters (LBs), which have bursts lasting 6-25 min, whereas 4U 1735-44 has a burst period of 86 min. We suggest that these bursts from SBs and LBs may be a result of breaking and re-formation of diquark pairs, on the surface of realistic strange quark stars. We use the beta equilibrated u, d and s quark model of Dey et al. and Li et al. and allow for spin-dependent hyperfine interaction between quarks. The interaction produces pairing of specific colour-spin diquarks, leading to further lowering of energy by several MeV for each pair, on average. Diquarks are expected to break up because of the explosion and shock of the thermonuclear process. The subsequent production of copious diquark pairing may produce sufficient energy to produce the very long bursts seen in SBs or LBs. We do not claim to be able to model the complicated process fully. However, the estimated total energy liberated, 1042 erg, can be explained in our model with the calculated pair density ∼0.275 fm-3 and a surface thickness of only half a μm, if the entire surface is involved. The depth of the surface involved in the process may be only few μm if the process is restricted to a small part of the surface near the equator, as suggested by Bildsten. If SBs and LBs are surface phenomena, then recurrent super bursts, found near 4U 1636-53 by Wijnands at an interval of 4.7 yr, and the quick cooling of KS 1731-260 could be natural in this model.

Monthly Notices of the Royal Astronomical Society

Super bursts and long bursts as surface phenomena of compact objects

A realistic EOS (equation of state) leads to strange stars (ReSS) which are compact in the mass-radius (M-R) plot, close to the Schwarzschild limiting line. Many of the observed stars fit in with this kind of compactness, irrespective of whether they are X-ray pulsars, bursters or soft γ repeaters or even radio pulsars. We point out that a change in the radius of a star can be small or large, when its mass is increasing and this depends on the position of a particular star on the M-R curve. We carry out a stability analysis against radial oscillations and compare with the EOS of other SS models. We find that the ReSS is stable and an M-R region can be identified to that effect.