\begin{document}$1.95M_\odot$\end{document}, the appearance of the quark matter (from nuclear to 2f or 3f quark matter) causes a radius difference of 0.5km~2km and provides the possibility of detection by NICER in the future. However, the sequential transition from 2f to 3f quark matter is difficult to detect because the transition does not lead to too high of a change in radius (far smaller than \begin{document}$0.5\; {\rm{km}}$\end{document}). The dependence solely on the measurements of the stellar radii to probe the equation of state of dense matter in neutron stars causes difficulties. Multi-messenger observations can help us to infer the interior of a neutron star in the future."> Multiple configurations of neutron stars containing quark matter -
  • [1]

    D. Blaschke and N. Chamel, Springer Nature Switzerland AG,457: 337 (2018)

  • [2]

    T. Endo, J. Phys. Conf. Ser.,509: 012075 (2014)

  • [3]

    M. Buballa, AIP Conf. Proc.,892: 476 (2007)

  • [4]

    B. Abbottet al., Phys. Rev. Lett.,119: 161101 (2017)

  • [5]

    D. Radice, A. Perego, F. Zappaet al., Astrophys. J,852: L29 (2018)

  • [6]

    K. Chatziioannou, C. -J. Haster, and A. Zimmerman, Phys. Rev. D,97: 104036 (2019)

  • [7]

    T. Malik, N. Alam, M. Fortinet al., Phys. Rev. C,98: 035804 (2018)

  • [8]

    I. Tews, J. Margueron, and S. Reddy, Phys. Rev. C,98: 045804 (2018)

  • [9]

    Z. -Y. Zhu, E. -P. Zhou, and A. Li, Astrophys. J,862: 98 (2018)

  • [10]

    V. Paschalidis, K. Yagi, D. Alvarez-Castilloet al., Phys. Rev. D,97: 084038 (2018)

  • [11]

    R. Nandi, and P. Char, Astrophys. J.,857: 12 (2018)

  • [12]

    J. -E. Christian, A. Zacchi, and J. Schaffner-Bielich, Phys. Rev. D,99: 023009 (2018)

  • [13]

    M. G. Alford, K. Rajagopal, S. Reddyet al., Phys. Rev. D,64: 074017 (2001)

  • [14]

    B. W. Mintz, E. S. Fraga, G. Pagliaraet al., Phys. Rev. D,81: 123012 (2010)

  • [15]

    G. Lugones, A. G. Grunfeld, and M. A. Ajmi, Phys. Rev. C,88: 045803 (2013)

  • [16]

    G. Baymet al., Rept. Prog. Phys.,81: 056902 (2018)

  • [17]

    V. Dexheimer, R. Negreiros, and S. Schramm, Phys. Rev. C,91: 055808 (2015)

  • [18]

    L. McLerran and S. Reddy, Phys. Rev. Lett.,122: 122701 (2019)

  • [19]

    M. Alford, M. Braby, M. W. Pariset al., Astrophys. J.,629: 969 (2005)

  • [20]

    W. Wei, B. Irving, M. Salinaset al., Astrophys. J.,887: 151 (2019)

  • [21]

    B. Kämpfer, J. Phys. A,14: L471 (1981)

  • [22]

    N. K. Glendenning and C. Kettner, Astron. Astrophys.,353: L9 (2000)

  • [23]

    K., C. Greiner, J. Schaffner-Bielich, and M. H. Thoma, Nucl. Phys. A,677: 463 (2000)

  • [24]

    F. Weber, Prog. Part. Nucl. Phys.,54: 193 (2005)

  • [25]

    K. Gendreau and Z. Arzoumanian (NICER Team), AAS Meeting No. 229, id. 309.03

  • [26]

    A. L. Wattset al., Rev. Mod. Phys.,88(2): 021001 (2016)

  • [27]

    P. B. Demorest, T. Pennucci, S. M. Ransomet al., Nature (London),467: 1081 (2010)

  • [28]

    E. Fonsecaet al., Astrophys. J,832: 167 (2016)

  • [29]

    J. Antoniadiset al., Science,340: 1233232 (2013)

  • [30]

    N. Brambillaet al., Eur. Phys. J. C,74: 2981 (2014)

  • [31]

    M. Buballa, V. Dexheimer, A. Dragoet al., J. Phys. G,41: 123001 (2014)

  • [32]

    M. G. Alford, A. Schmitt, K. Rajagopalet al., Rev. Mod. Phys.,80: 1455 (2008)

  • [33]

    D. Alvarez-Castillo, S. Benić, D. Blaschkeet al., Eur. Phys. J. A,52: 232 (2016)

  • [34]

    D. E. Alvarez-Castillo and D. Blaschke, Phys. Part. Nucl.,46: 846 (2015)

  • [35]

    D. Alvarez-Castillo, A. Ayriyan, S. Benićet al., Eur. Phys. J. A,52: 69 (2016)

  • [36]

    A. Zacchi, L. Tolos, and J. Schaffner-Bielich, Phys. Rev. D,95: 103008 (2017)

  • [37]

    B. K. Agrawal and S. K. Dhiman, Phys. Rev. D,79: 103006 (2009)

  • [38]

    L. Bonanno and A. Sedrakian, Astron. Astrophys.,539: A16 (2012)

  • [39]

    M. Buballa, F. Neumann, M. Oertelet al., Phys. Lett. B,595: 36 (2004)

  • [40]

    T. Klähn, D. Blaschke, F. Sandinet al., Phys. Lett. B,654: 170 (2007)

  • [41]

    T. Klähn, R. Lastowiecki, and D. Blaschke, Phys. Rev. D,88: 085001 (2013)

  • [42]

    M. Alford and A. Sedrakian, Phys. Rev. L,119: 161104 (2017)

  • [43]

    T. Klähn andT. Fischer, Astrophys. J,810: 134 (2015)

  • [44]

    C. Fuchs, Lect. Notes Phys.,641: 119 (2004)

  • [45]

    T. Klähnet al., Phys. Rev., C,74: 035802 (2006)

  • [46]

    M. Alford and S. Han, Eur. Phys. J. A,52: 62 (2016)

  • [47]

    S. Han, M. A. A. Mamun, S. Lalitet al., Phys. Rev. D,100: 103022 (2019)

  • [48]

    M. G. Alford, S. Han, and K. Schwenzer, Journal of Physics G Nuclear and Particle Physics,46: 11 (2019)

  • [49]

    B. P. Abbott, R. Abbott, T. D. Abbottet al., Phys. Rev. X,9: 011001 (2019)

  • [50]

    A. Brillante and I. N. Mishustin, Eur. Phys. L,105(3): 39001 (2014)

  • [51]

    C. V. Flores and G. Lugones, Class. Quant. Grav.,31: 155002 (2014)

  • [52]

    H. Sotani, T. Maruyama, and T. Tatsumi, Nucl. Phys. A,906: 37 (2013)

  • [53]

    D. Lai, Mon. Not. Roy. Astron. Soc.,270: 611 (1994)

  • [54]

    H. Yu and N. N. Weinberg, Mon. Not. Roy. Astron. Soc.,470(1): 350 (2017)

  • [55]

    N. Andersson and W. C. G. Ho, Phys. Rev. D,97: 023016 (2018)

  • [56]

    M. C. Miller, F. K. Lamb, A. J. Dittmannet al., ApJL,887: L24 (2019)

  • [57]

    T. E. Riley, A. L. Watts, S. Bogdanovet al., ApJL,887: L21 (2019)

  • [58]

    H. T. Cromartie, E. Fonseca, S. M. Ransom,et al., Nat. Astro, (2019)

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