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- W3158620309 abstract "”Old” questions of relativistic astrophysics, like the internal structure of compact stars, have received a lot of attention recently since they are very important for a solid knowledge of the QCD diagram in the low-T , high μ region as discussed along this Workshop. Among the most simple forms of investigating (indirectly) the nature of high-density matter, more precisely of the equation of state connecting the pressure and the energy density; is by obtaining accurate determinations of masses and radii. A comparison of the static models generated by integration of the Tolman-OppenheimerVolkoff equations with observed data should reveal a great deal of information about the equation of state. While astronomers and physicists alike have longely dreamed of such determinations we have only recently achieved sufficient accuracy to perform some key tests on selected objects, although it should be acknowledged that three decades of compact star astrophysics had produced quite clever arguments to determine masses and radii, even in the cases in which they proved to be wrong. A paradigmatic example of the above assertions is the celebrated determination of the binary pulsar mass PSR 1913+16, believed to be accurate to the fourth decimal place [7]. Methods based on combinations of spectroscopic and photometric techniques have been recently perfectioned, and have confirmed that at least one X-ray source is significantly above the ”canonical” 1.44 M⊙; namely Vela X-1 for which a value of 1.87 −0.17M⊙ has been obtained [7]. It is also possible that at least some compact stars are extremely compact, or in other words, that their radii are ∼ 30 − 40% less than the cherished 10 km for M ∼ 1M⊙. Indeed, this is the claim of the analysis of [4] of the binary Her X-1 (M = 0.98 ± 0.12M⊙ and R = 6.7 ± 1.2 km) and [11] in the case of the isolated nearby RX J1856-37 (M = 0.9±0.2 M⊙ and R = 6 −1 +2 km). In fact, such compactness" @default.
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- W3158620309 date "2001-12-06" @default.
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- W3158620309 title "Diquarks degrees of freedom in the EOS and the compactness of compact stars" @default.
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