Abstract
Recently there have been important developments in the determination of neutron star masses which put severe constraints on the composition and equation of state (EOS) of the neutron star matter. Here we study the effect of quark and nuclear matter mixed phase on mass radius relationship of neutron stars employing recent models from two classes of EOS’s and discuss their implications.
Similar content being viewed by others
References
N K Glendenning,Phys. Rev. D46, 1274 (1992)
A Akaml, V J Pandharipande and D G Ravenhal,Phys. Rev. 58, 1804 (1998)
V K Gupta, Vinita Tuli and Ashok Goyal,Astrophys. J. 579, 374 (2002)
S E Thorsett and D Chakraborty,Astrophys. J.,512, 288 (1999)
J A Orsoz and E Kuulkers,Mon. Not. R. Astron. Soc. 305, 132 (1999)
M H Van Kerkwijk, J Van Paradijs and E J Zuiderwijk,Astron. Astrophys. 303, 497 (1995)
M C Miller and F K Lamb,Astrophys. J. 499, L37 (1998)
M C Miller, F K Lamb and D Psattis,Nucl. Phys. B69, 123 (1998);Astrophys. J. 508, 791 (1998)
M C Miller, F K Lamb and G B Cook,Astrophys. J. 509, 793 (1998)
Author information
Authors and Affiliations
Rights and permissions
About this article
Cite this article
Goyal, A. Hybrid stars. Pramana - J Phys 62, 753–756 (2004). https://doi.org/10.1007/BF02705363
Issue Date:
DOI: https://doi.org/10.1007/BF02705363