The properties of hadron-quark hybrid stars are studied when the quark phase is described in terms of a local SU(3) Nambu-Jona-Lasinio (NJL) model taking into account the contribution of the vector and axial-vector interaction between the quarks, and the hadronic phase, in the relativistic mean field (RMF) model. For different values of the vector coupling constant GV, the equations of state of the quark matter are calculated and the parameters of the hadron-quark phase transition are determined under the assumption that the phase transition takes place in accordance with Maxwell’s construction. It is shown that for a larger vector coupling constant, the equation of state of the quark matter will be “stiffer” and the coexistence pressure P0 of the phases will be greater. Using the resulting hybrid equations of state, the TOV equations are integrated numerically and the mass and radius of the compact star are determined for different values of the central pressure Pc. It is shown that when GV is larger, the maximum mass of the compact star will be larger and thereby, the radius of the configuration with maximum mass will be smaller. Questions of the stability of hybrid stars are also discussed. It is shown that in terms of the model examined here, for all values of the vector coupling constant, a hybrid star with an infinitely small quark core is stable. These results are compared with recent measurements of the mass and radius of the pulsars PSR J0030+0451 and PSR J0740+6620, carried out at the International Space Station with the NICER X-ray telescope. A comparison of the theoretical results with observational data does not exclude the possibility of quark deconfinement in the interiors of compact stars.
Similar content being viewed by others
References
P. Demorest, T. Pennucci, S. M. Ransom, et al., Nature 467, 1081 (2010).
J. Antoniadis, P. C. C. Freire, N. Wex, et al., Science 340, 6131 (2013).
M. Miller, F. K. Lamb, A. Dittmann, et al., Astrophys. J. Lett. 887, L24 (2019).
E. Fonseca, H. T. Cromartie, T. T. Pennucci, et al., Astrophys. J. Lett. 915, L12 (2021).
M. C. Miller, F. K. Lamb, A. J. Dittmann, et al., Astrophys. J. Lett. 918, L28 (2021).
K. Schertler, C. Greiner, J. Schaffner-Bielich, et al., Nucl. Phys. A 677, 463 (2000).
G. F. Burgio, M. Baldo, P. K. Sahu, et al., Phys. Rev. C 66, 025802 (2002).
G. V. Alaverdyan, A. R. Arutyunyan, and Yu. L. Vartanyan, Astrophysics 46, 361 (2003).
G. V. Alaverdyan, A. R. Arutyunyan, and Yu. L. Vartanyan, Astrophysics 47, 52 (2004).
B. K. Sharma, P. K. Panda, S. K. Patra, Phys. Rev. C 75, 035808 (2007).
G. V. Alaverdyan, Astrophysics 52, 132 (2009.
G. B. Alaverdyan, Gravit. Cosmol. 15, 5 (2009).
A. G. Alaverdyan, G. B. Alaverdyan, and A. O. Chiladze, Int. J. Mod. Phys. D 19, 1557 (2010).
G. B. Alaverdyan, Res. Astron. Astrophys. 10, 1255 (2010).
R. Negreiros, V. A. Dexheimer, and S. Schramm, Phys. Rev. C 85, 035805 (2012).
G. V. Alaverdyan and Yu. L. Vartanyan, Astrophysics 60, 563 (2017).
S. Khanmohamadi, H. R. Moshfegh, and S. A. Tehrani, Phys. Rev. D 101, 023004 (2020).
A. Chodos, R. L. Jaffe, K. Johnson, et al., Phys. Rev. D 9, 3471 (1974).
Y. Nambu and G. Jona-Lasinio, Phys. Rev. 122, 345 (1961).
Y. Nambu and G. Jona-Lasinio, Phys. Rev. 124, 246 (1961).
U. Vogl and W. Weise, Prog. Part. Nucl. Phys. 27, 195 (1991).
T. Hatsuda and T. Kunihiro, Phys. Rep. 247, 221 (1994).
P. Rehberg, S. P. Klevansky, and J. Hüfner, Phys. Rev. C 53, 410 (1996).
M. Buballa, Phys. Rep. 407, 205 (2005).
M. K. Volkov and A. E. Radzhabov, UFN 176, 569 (2006).
P. Wang, A. W. Thomas, and A. G. Williams, Phys. Rev. C 75, 045202 (2007).
M. Alford and A. Sedrakian, Phys. Rev. Lett. 119, 161104 (2017).
I. F. Ranea-Sandoval, M. G. Orsaria, G. Malfatti, et al., Symmetry 11, 425 (2019).
J. J. Li, A. Sedrakian, and M. Alford, Phys. Rev. D 101, 063022 (2020).
H. Pais, D. P. Menezes, and C. Providência, Phys. Rev. C 93, 065805 (2016).
G. V. Alaverdyan and Yu. L. Vartanyan, Astrophysics 61, 483 (2018).
J. D. Walecka, Ann. Phys. 83, 491 (1974).
B. D. Serot and J. D. Walecka, Int. J. Mod. Phys. E 6, 515 (1997).
G. B. Alaverdyan, Symmetry 13, 124 (2021).
G. Lugones and A. G. Grunfeld, Universe 7, 493 (2021).
J. Boguta, and A. R. Bodmer, Nuclear Physics A 292, 413 (1977).
G. ‘t Hooft, Phys. Rev. Lett. 37, 8 (1976).
N. K. Glendenning, Phys. Rev. D 46, 1274 (1992).
M. Ju, J. Hu, and H. Shen, Astrophys. J. 923, 250 (2021).
Z. F. Seidov, Astron. zh. 15, 347 (1971).
R. C. Tolman, Phys. Rev. 55, 364 (1939).
J. R. Oppenheimer and G. M. Volkoff, Phys. Rev. 55, 374 (1939).
G. Baym, H. Bethe, and Ch. Pethick, Nucl. Phys. A, 175, 255 (1971).
E. Fonseca, T. T. Pennucci, J. A. Ellis, et al., Astrophys. J. 832, 167 (2016).
Z. Arzoumanian, A. Brazier, S. Burke-Spolaor, et al., Astrophys. J. Suppl. Ser. 235, 37 (2018).
S. Chandrasekhar, Astrophys. J. 140, 417 (1964); Erratum in Astrophys. J. 140, 1342 (1964).
J. P. Pereira, C. V. Flores, and G. Lugones, Astrophys. J. 860, 12 (2018).
L. Tonetto, and G. Lugones, Phys. Rev. D, 101, 123029 (2020).
J. P. Pereira, M. Bejger, L. Tonetto, et al., Astrophys. J. 910, 145 (2021).
Author information
Authors and Affiliations
Corresponding author
Additional information
Translated from Astrofizika, Vol. 65, No. 2, pp. 301-319, May 2022.
Rights and permissions
About this article
Cite this article
Alaverdyan, G.B. Quark Matter in the NJL Model with a Vector Interaction and the Structure of Hybrid Stars. Astrophysics 65, 278–295 (2022). https://doi.org/10.1007/s10511-022-09737-z
Received:
Accepted:
Published:
Issue Date:
DOI: https://doi.org/10.1007/s10511-022-09737-z