how dense is a quark star

This result confirms previous discussions of other astrophysical objects ruling out soft EOSs [21]. Screening in the plasma leads to novel behavior, including a remarkable non-BCS scaling of TC, the transition temperature to the color superconducting phase. spinning-down neutron stars, crustal 'plates' will move an equatorial More than that, according to the strange matter hypothesis strange quark matter could be more stable than nuclear matter, in which case neutron stars should be largely composed of pure quark matter possibly enveloped in thin nuclear crusts. In upper limit on the attainable critical field because of a reduction in the spin I shall review two issues: Finally, we show that the region of the phase diagram relevant for neutron star cores, In this letter it is shown that at somewhat higher densities one finds a charged kaon condensate, driven to a large extent by the “stgma term” interaction with baryons. In contrast, for This dichotomy between the effects of the radiative corrections at first appears rather surprising, as the BRST identity connects the self-energy to the vertex corrections. Quark star. Such a star is known as a Ordinary quark matter consisting of up and down quarks (This suggests that the only stable quark stars will be neutron stars with a quark matter core, while quark stars consisting entirely of ordinary quark matter will be highly unstable and dissolve spontaneously.It has been shown that the high Fermi energy making ordinary quark matter unstable at low temperatures and pressures can be lowered substantially by the transformation of a sufficient number of up and down quarks into strange quarks, as strange quarks are, relatively speaking, a very heavy type of quark particle.This kind of quark matter is known specifically as strange quark matter and it is speculated and subject to current scientific investigation whether it might, in fact, be stable under the conditions of interstellar space (Quark stars made of strange quark matter are known as Theoretical investigations have revealed that quark stars might not only be produced from neutron stars and powerful supernovas, they could also be created in the early cosmic phase separations following If these primordial quark stars transform into strange quark matter before the external temperature and pressure conditions of the early Universe make them unstable, they might turn out stable, if the Bodmer–Witten assumption holds true. We suggest that these phenomena can be explained at least equally well by noisiness in the rate of creep of vorticity through the neutron superfluid in the crust, in almost precise analogy to the well known noisy behaviour of flux creep in hard superconducting magnets4. This paper gives an overview of the phases of dense matter predicted to make their appearance in the cores of neutron We argue that 't Hooft constraints can be used at finite density along with non perturbative methods to help selecting the correct phase.It has been suggested that charged pions form a Bose-Einstein condensate in baryonic matter at zero temperature and about twice nuclear density. As a result, the cooling of the stars in the normal Net strangeness is carried by hyperons, K-mesons, H-dibaryons, The surface magnetic field of a This approach has recently been successfully applied to the study of color superconductivity, where the dominant di-quark pairing interaction arises from one gluon exchange. We examine two channels of superfluid-normal fluid friction where (i) rotational vortices are decoupled from the non-superconducting domains and the interaction is due to the strong force between protons and neutrons; (ii) the non-superconducting domains are dynamically coupled to the vortices and the vortex motion generates transverse electric fields within them, causing electronic current flow and Ohmic dissipation.

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