Stable quark stars beyond neutran stars : can they account for the missing matter ?

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dc.creatorMinkowski, Peter
dc.creatorKabana, Sonja
dc.date2002-04-09
dc.date.accessioned2026-07-07T11:09:14Z
dc.date.available2026-07-07T11:09:14Z
dc.descriptionThe structure of a spherically symmetric stable dark 'star' is discussed, at zero temperature, containing 1) a core of quarks in the deconfined phase and antileptons 2) a shell of hadrons in particular $n$, $p$, $Λ$ and $Σ^-$ and leptons or antileptons and 3) a shell of hydrogen in the superfluid phase. If the superfluid hydrogen phase goes over into the electromagnetic plasma phase at densities well below one atom / $(10 fm)^{3}$, as is usually assumed, the hydrogen shell is insignificant for the mass and the radius of the 'star'. These quantities are then determined approximatively : mass = 1.8 solar masses and radius = 9.2 km. On the contrary if densities of the order of one atom / $(10 fm)^{3}$ do form a stable hydrogen superfluid phase, we find a large range of possible masses from 1.8 to 375 solar masses. The radii vary accordingly from 9 to 1200 km.
dc.description5 pages, 2 figures, contribution to Strange Quark Matter conference, Frankfurt, Germany, Sept. 2001
dc.identifierhttps://arxiv.org/abs/hep-ph/0204103
dc.identifierhttp://arxiv.org/abs/hep-ph/0204103
dc.identifierJ.Phys.G28:2063-2068,2002
dc.identifierdoi:10.1088/0954-3899/28/7/372
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/190398
dc.subjectHigh Energy Physics - Phenomenology
dc.titleStable quark stars beyond neutran stars : can they account for the missing matter ?
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