\begin{document}$ 9.1223\times10^{24} $\end{document} when \begin{document}$ m=10^{17} $\end{document} GeV, \begin{document}$n_{\rm B}=5.99\times10^{31}~\rm{cm^{-3}}$\end{document}, \begin{document}$\phi=7.59\times 10^{-26} \rm{cm^{-2}s^{-1}sr^{-1}}$\end{document}. The good agreement of our calculated luminosities for WDs with observation provides support for our model based on the RC effect by MMs. We obtain a new limit of the MM flux of \begin{document}$\xi=\phi\langle\sigma_m v_{\rm{T}}\rangle_{-28}\leq $\end{document}\begin{document}$ 9.0935\times10^{-13}\rm{cm^{-2}s^{-1}sr^{-1}}$\end{document}, and \begin{document}$ \xi\leq 4.9950\times10^{-13}\rm{cm^{-2}s^{-1}sr^{-1}} $\end{document} at \begin{document}$n_{\rm B}=5.99\times10^{31}\rm{cm^{-3}}$\end{document} when \begin{document}$m=10^{15}\rm{GeV}$\end{document}, \begin{document}$ \beta=9.4868\times10^{-3} $\end{document}, and \begin{document}$ m=10^{17}\rm{GeV}, $\end{document}\begin{document}$ ~\beta=10^{-3} $\end{document}, respectively. Our results show that the RC effect could cause heating that prevents white dwarfs from cooling down into a stellar graveyard. Our results will also provide a new idea for further research on the upper limit of MM flow (note: \begin{document}$n_{\rm B}, \sigma_m, m, \phi, \xi$\end{document} are the baryon number density, reaction cross section, mass, MM flux, and the new limit of the MM flux, respectively, and \begin{document}$ \beta=v_T/c $\end{document} is the ratio of the speed of MMs to that of light)."> New insights into the limit of the magnetic monopole flux and the heating source in white dwarfs -
  • [1]

    L. Mestel, MNRAS.112, 583 (1952)

  • [2]

    R. M. Avakian, CoMBAO.44, 115 (1972)

  • [3]

    L. Bildsten and D. M. Hall, Astrophys. J.549, 219 (2001)

  • [4]

    C. J. Deloye and L. Bildsten, Astrophys. J.580, 1077 (2002)

  • [5]

    E. García-Berro, L. G. Althaus, A. H. Córsicoet al., Asstrophys. J.677, 473 (2008)

  • [6]

    R. V. Lobato, M. Malheiro, and J. G. Coelho, Mgm. Conf.4313, 4318 (2018)

  • [7]

    S. H. Cheng, J. D. Cummings, and B. Ménard, Asstrophys. J.886, 100 (2019)

  • [8]

    M. E. Caplan, C. J. Horowitz, and A. Cumming, Astrophys. J.902(2), 44C (2020)

  • [9]

    C. Callanet al., Nucl. Phys.212, 391 (1983)

  • [10]

    V. A. Rubakov, JETP Lett.33, 644 (1981)

  • [11]

    M. Detrixhe, D. Besson, P. W. Gorhamet al., Phys. Lett. D83, 023513 (2011)

  • [12]

    M. Frank, A. Antoshkin, C. Dukeset al., ICRC36, 888 (2019)

  • [13]

    T. Fujii and A. C. Pierre, ICRC34, 319 (2015)

  • [14]

    B. Kain, Phys. Rev. D100, 063003 (2019)

  • [15]

    A. Rajantie, Phil. Trans. R. Soc. A.370, 5705 (2012)

  • [16]

    N. E. Mavromatos and V. A. Mitsou, IJMPA35, 2030012 (2020)

  • [17]

    J. J. Liu, MNRAS.433, 1108 (2013)

  • [18]

    J. J. Liu, MNRAS.438, 930 (2014)

  • [19]

    J. J. Liu and W. M. Gu, Astrophys. J. Suppl.224, 29 (2016)

  • [20]

    J. J. Liu, D. M. Liuet al., Chin. Phys. C41(12), 125102 (2017)

  • [21]

    J. J. Liu and D. M. Liu, EPJC.78, 84 (2018a)

  • [22]

    J. J. Liu and D. M. Liu, RAA.18(1), 8 (2018)

  • [23]

    J. J. Liu and D. M. Liu, Astrophys. Space Sci.363(5), 115 (2018)

  • [24]

    J. J. Liu and D. M. Liu, New Astron.69, 69 (2019a)

  • [25]

    J. J. Liu, D. M. Liu, and L. H. Hao, ChPhC43, 064107 (2019b)

  • [26]

    J. J. Liu and D. M. Liu, Astron. Nachr.341, 291 (2020)

  • [27]

    Q. H., Peng, J. J. Liu, and C. K. Chou, MPLA35, 2050030 (2020)

  • [28]

    Q. H. Peng, J. J. Liu, and Z. Q. Ma, New Astron.57, 59 (2017)

  • [29]

    W. Bernreuther and N. S. Craigie, Phys. Rev. Lett.55, 2555 (1985)

  • [30]

    Q. H. Peng, Z. Y. Lie, and D. Y. Wang, Sci. Sin. Phys. Mech. As.28, 970 (1985)

  • [31]

    E. Kolb and M. S. Turner., Astrophys. J.286, 702 (1984)

  • [32]

    K. Freese, Asstrophys. J.286, 216 (1984)

  • [33]

    Z. Q. Ma and J. F. Tang, Phys. Lett. B153, 59 (1983)

  • [34]

    T. Kallinger, W. W. Weiss, C. Barbanet al., A&A509, A77 (2010)

  • [35]

    D. Stello, and H. Bruntt, H. Prestonet al., Astrophys. J.674, L53 (2008)

  • [36]

    D. Huber, T. R. Bedding, D. Stelloet al., Astrophys. J.743, 143 (2011)

  • [37]

    S. Sharma, D. Stello, and J. Bland-Hawthornet al., Astrophys. J.822, 15 (2016)

  • [38]

    T. M. Brown, D. W. Latham, M. E. Everettet al., Astron. J.142, 112 (2011)

  • [39]

    E. Parker, Asstrophys. J.160, 383 (1970)

  • [40]

    K. Freese and E. Krasteva, Phys. Rev. D59, 063007 (1999)

  • [41]

    S. K. Grunblatt, J. C. Zinn, A. M. Price-Whelanet al., Astrophys. J.916, 88 (2021)

  • [42]

    V. Silva Aguirre, G. R. Davies, and S. Basu, MNRAS452, 2127 (2015)

  • [43]

    T. D. Morton, Isochrones: Stellar Model Grid Package, v2.0, (Astrophysics Source Code Library, ascl: 1503.010, 2015)

  • [44]

    D. Huber, J. Zinn, M. Bojsen-Hansenet al., Astrophys. J.844, 102 (2017)

  • [45]

    L. da Silva, L. Girardi, L. Pasquiniet al., A&A458, 609 (2006)

  • [46]

    T. S. Rodrigues, D. Bossini, and A. Miglio, Mon. Not. R. Astron. Soc.467, 1433 (2017)

  • [47]

    E. P. Bellinger, Mon. Not. R. Astron. Soc.492, L50 (2020)

  • [48]

    K. Belkacem, M. J. Goupil, M. A. Dupretet al., A&A530, A142 (2011)

  • [49]

    H. Kjeldsen and T. R. Bedding, A&A293, 87 (1995)

  • [50]

    D. Huber, D. Stello, T. R. Beddinget al., Comm. Asteroseismology160, 74 (2009)

  • [51]

    K. Freese, M. S.Turner, and D. N. Schramm, Phys. Rev. Lett.51, 1625 (1983)

  • [52]

    M. Schwarzschild, Structure and Evolution of the Star., (Princeton: Princeton university Press, 1958)

  • [53]

    R. Bjork, Stephan, and B. Chaboyer, Astrophys. J.641, 1102 (2006)

  • [54]

    D. A. Dicus, D. N. Page, and V. L. Teplitz, Phys. Rev. D26, 1306 (1982)

  • [55]

    L. G. Althaus, A. H. Córsico, J. Isernet al., Astron. Astrophys. Rev.18, 471 (2010)

  • [56]

    N. Itoh, H. Hayashi, A. Nishikawaet al., Astrophys. J. Suppl.102, 411 (1996)

  • [57]

    M. Izawa, Prog. Theor.75, 556 (1986)

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