Abstract
The 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, radius = 9.2 km.
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Alford, M., Rajagopal, K., Reddy S. and Wilczek, F.: 2001a, ‘The Minimal CFL-Nuclear Interface’ hep-ph/0105009.
Alford, M., Bowers, J.A. and Rajagopal, K.: 2001, ‘Color Superconductivity in Compact Stars’ J. Phys. G27, 541.
Ambrosini, G. et al.: 1996, (NA52 coll.), Heavy Ion Phys. 4, 429.
Armstrong. T.A. et al.: 2001, (E864 coll.), ‘Search for Strange Quark Matter Produced in Relativistic Heavy Ion Collisions’ Phys. Rev. C63, 054903.
Arsenescu, R. et al.: 1997, (NA52 coll.), J. Phys. G23, 2135.
Bogolubov, N.N.: 1947, J. Phys. USSR XI, 23.
Glendenning, N.K.: 1997, Compact Stars, Nuclear Physics, Particle Physics and General Relativity, Springer-Verlag, New York.
Huber, H., Weber, F. and Weigel, M.K.: 1998, ‘Symmetric and Asymmetric Nuclear Matter in the Relativsitic Approach at Finite Temperatures’ Phys. Rev. C57, 3484.
Jetzer, P.: 1998, Proceedings of EC-TMR Euroconference on 3 K Cosmology, Rome, Italy, 5–10 Oct 1998, astro-ph/9901058.
Kabana, S. and Minkowski, P.: 2001, New J. Phys. 3, 4.
Kabana, S. et al.: 1997, (NA52 coll.), J. Phys. G23, 2135.
Klingenberg, R. et al.: 1996, (NA52 coll.), Nucl. Phys. A610, 306c.
Landau, L.: 1932, Physik. Zeitschrift Sowjetunion 1, 285.
Lattimer J.M. and Prakash, M.: 2001, ‘Neutron Star Structure and the Equation of State’ Astrophys. J. 550, 426.
Madsen, J.: 1998, ‘Physics and Astrophysics of Strange Quark Matter’ in Hadrons in dense matter and hadrosynthesis, Lecture Notes in Physics, Springer-Verlag (ed. J. Cleymans), p. 162, Cape Town, astro-ph/9809032.
Madsen, J.: 2000, ‘Probing Strange Stars and Color Superconductivity by R Mode Instabilities in Millisecond Pulsars’ Phys. Rev. Lett. 85, 10.
Minkowski, P.: 1990, Czech J. Phys. B40, 1003.
Oppenheimer, J.R. and Volkoff, G.M.: 1939, Phys. Rev. 55, 374.
Pons, J.A., Steiner, A.W., Prakash, M. and Lattimer, J.M.: 2001, ‘Evolution of Proto-Neutron Stars with Quarks’ Phys. Rev. Lett. 86, 5223.
Pons, J.A., Walter, F.M., Lattimer, J.M., Prakash, M., Neuhaeuser, R. and An, P.: 2001, ‘Towards a Mass and Radius Determination of the Nearby Isolated Neutron Star RX J185635-3754’ astro-ph/0107404.
Prakash, M., Lattimer, J.M., Pons, J.A., Steiner, A.W. and Reddy, S.: 2000, in Proceedings of ECT * International Workshop on Physics of Neutron Star Interiors (NSI00), Trento, Italy, 19 June–7 July 2000.
Straumann, N.: 1988, Allgemeine Relativitätstheorie und relativistische Astrophysik, Lecture Notes in Physics, 150, Springer Verlag, page 334, equation (14).
Tolman, R.C.: 1939, Phys. Rev. 55, 364.
Weber, F.: 2001, ‘Strangeness in Neutron Stars’ J. Phys. G27, 465.
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Kabana, S., Minkowski, P. Dark quark `stars': do they matter for Ωmatter?. Space Science Reviews 100, 175–192 (2002). https://doi.org/10.1023/A:1015826413450
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DOI: https://doi.org/10.1023/A:1015826413450