The equation of state and composition of hot strange quark matter that is opaque to neutrinos are determined. This study is based on the MIT quark bag model. Three different variants of the lepton population in hot quark matter are considered. In the first, only e–, e+, νe, and \( {\overline{\upnu}}_e \) leptons are present in the material. In the second, μ–, μ+, νμ, and \( {\overline{\upnu}}_{\upmu} \) are added to these leptons. And in the third, τ– neutrinos and τ+ antineutrinos are also present and the phenomenon of neutrino oscillations is taken into account. Numerical calculations are done for different temperatures and lepton charge densities. It is shown that when neutrinos exist in hot quark matter (T~1012 K) the number of u quarks is 24-33% and 37-42% greater than the number of d and s quarks, respectively, depending on the baryon charge concentration. When neutrino oscillations are included, these parameters go to 19-27% and 30-37%. When there are no neutrinos, on the other hand, the number of d quarks is less than the number of u quarks by 2-8%. It is shown that for a fixed baryon charge concentration, the pressure of the quark matter depends strongly on temperature. This dependence is especially strong at comparatively low densities. As opposed to this, the pressure has a weak temperature dependence for a fixed energy density.
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References
E. Witten, Phys. Rev. D, 30, 272 (1984).
Ya. B. Zeldovich and O. Kh. Guseinov, DAN SSSR 162, 791 (1965).
Ya. B. Zeldovich and O. Kh. Guseinov, Pis’ma ZhETF 1(4), 11 (1965).
L. N. Ivanova, V. S. Imshennik, and D. K. Nadezhin, Nauch. Inf. Astron. Soveta AN SSSR 13, 3 (1965).
V. S. Imshennik and D. K. Nadezhin, UFN 156, 561 (1988).
G. H. Bordbar, A. Doostforush, and A. Zamani, Astrophysics 54, 277 (2011) (arxiv, 1103, 2436v1).
A. G. Alaverdyan and G. S. Hajyan, Journal of Physics: Conference Series 496, 012005 (2014).
G. S. Hajyan, A. G. Alaverdyan, Astrophysics 57, 559 (2014).
A. G. Alaverdyan, Proceedings of the Yerevan State University 3, 6 (2016).
A. Chodos, et al., Phys. Rev. D 9, 3471 (1974).
N. K. Glendenning, Nuclear Physics, Particle Physics and General Relativity, Springer, Berkeley, California (1996).
G. H. Bordbar and A. R. Peivand, Research in Astron. Astrophys.11, 851 (2011).
B. Kuchowicz, Bull. Acad. Pol, Sci., Ser. Sci Mat., Astr. et Phys. 11, 317 (1963).
B. Pontecorvo, ZhETF33, 549 (1957); ZhETF 34, 247 (1957).
S. P. Mikheev and A. Yu. Smirnov, Yadernaya Fizika42 (b), 1441 (1985).
G. S. Bisnovatyi-Kogan, Physical Problems of The Theory of Stellar Evolution [in Russian], Nauka, Moscow (1989).
Yu. L. Vartanyan, Sh. R. Melikyan, and A. A. Shaginyan, Astrophysics 55, 429 (2012).
M. Buballa, Phys. Rep. 407, 205 (2005).
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Translated from Astrofizika, Vol. 61, No. 4, pp. 585-598 (November 2018).
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Hajyan, G.S. Equation of State for Hot Quark Matter with Neutrino Confinement. Astrophysics 61, 511–524 (2018). https://doi.org/10.1007/s10511-018-9553-6
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DOI: https://doi.org/10.1007/s10511-018-9553-6