Russian Physics Journal

, Volume 61, Issue 3, pp 548–555 | Cite as

Characteristics of a Degenerate Neutron Gas in a Magnetic Field with Allowance for the Anomalous Magnetic Moment of the Neutron

  • V. V. SkobelevEmail author
  • V. P. Krasin

General expressions for the dependence of the Fermi energy, pressure, and total energy of a degenerate neutron gas in a magnetic field on the magnitude of the field and the neutron concentration with allowance for the anomalous magnetic moment of the neutron have been obtained in implicit form, and the dependence of these quantities on the field is presented in graphical form for the neutron concentration C = 1038 cm–3, which is typical for neutron stars. Analytical estimates of the pressure have been made for the magnitude of the fields possible in neutron stars ~1017–1019 G and this neutron concentration ~1038 cm–3, including when the neutron gas is close to its saturated state with preferred orientation of the anomalous magnetic moment of all the neutrons in alignment with the field. It is found that even such fields ~1017 G have practically no effect on the pressure in comparison with the case when the field is absent, an effect being possible only for В ~ 1018–1019 G. The analytical dependence on the neutron concentration of the corresponding field BS at which the neutron gas transitions to the saturated state has been found in explicit form. It is established that for B > BS the indicated characteristics of the neutron gas, and likewise its state, no longer change.


neutron magnetic field anomalous magnetic moment Fermi energy pressure 


Unable to display preview. Download preview PDF.

Unable to display preview. Download preview PDF.


  1. 1.
    L. Dall’Osso, S. N. Shore, and L. Stella, Mon. Not. R. Astron. Soc., 328, 1869 (2009).ADSCrossRefGoogle Scholar
  2. 2.
    V. V. Skobelev, Russ. Phys. J., 55, No. 1, 122 (2012).CrossRefGoogle Scholar
  3. 3.
    S. S. Avancini, D. P. Menezes, M. B. Pinto, and C. Providencia, Phys. Rev. D, 85, 091901 (2012).ADSCrossRefGoogle Scholar
  4. 4.
    S. Lander and D. Jones, Mon. Not. R. Astron. Soc., 424, 482 (2012).ADSCrossRefGoogle Scholar
  5. 5.
    H.-Y. Chiu, V. Canuto, and L. Fassio-Canuto, Phys. Rev., 176, 1438 (1968).ADSCrossRefGoogle Scholar
  6. 6.
    M. Strickland, V. Dexheimer, and D. P. Menezes, Phys. Rev. D, 86, 125032-1 (2012).ADSCrossRefGoogle Scholar
  7. 7.
    L. D. Landau and E. M. Lifshitz, Statistical Physics, Butterworth-Heinemann, London (1980).zbMATHGoogle Scholar
  8. 8.
    S. Weinberg, Gravitation and Cosmology, John Wiley & Sons, Inc., New York (1972).Google Scholar
  9. 9.
    V. V. Skobelev, Russ. Phys. J., 60, No. 12, 2073–2076 (2018).CrossRefGoogle Scholar

Copyright information

© Springer Science+Business Media, LLC, part of Springer Nature 2018

Authors and Affiliations

  1. 1.Moscow Polytechnic UniversityMoscowRussia

Personalised recommendations