Hostname: page-component-848d4c4894-sjtt6 Total loading time: 0 Render date: 2024-07-05T04:59:14.981Z Has data issue: false hasContentIssue false
  • English
  • Français

Magnetic field dissipation in nucleonic neutron star cores

Published online by Cambridge University Press:  27 February 2023

Dmitry D. Ofengeim Open the ORCID record for Dmitry D. Ofengeim [Opens in a new window] ,
Mikhail E. Gusakov  and
Alexander Y. Potekhin
Dmitry D. Ofengeim*
Affiliation:
Ioffe Institute, 26 Polytekhnicheskaya, St Petersburg 194021, Russia
Mikhail E. Gusakov
Affiliation:
Ioffe Institute, 26 Polytekhnicheskaya, St Petersburg 194021, Russia
Alexander Y. Potekhin
Affiliation:
Ioffe Institute, 26 Polytekhnicheskaya, St Petersburg 194021, Russia
*
*email: ddofengeim@gmail.com
Get access Rights & Permissions [Opens in a new window]

Abstract

We study the long-term heating due to magnetic field decay in the core of neutron star. Two cases for the nucleonic core are considered: normal and strongly superconducting. We give simple scaling relations (depending on the internal stellar temperature and the averaged magnetic field in the core) to estimate the magnetic field decay rate for the most important dissipation processes. Comparison to properties of observed neutron stars suggests that heating due to the magnetic field decay is (at least partially) responsible for the thermal states of middle-aged magnetars and highly-magnetized isolated neutron stars with ages of 1 — 10 Myr.

Keywords

magnetohydrodynamicsstars: neutronstars: magnetic fields
Type
Poster Paper
Information
Proceedings of the International Astronomical Union , Volume 16 , Symposium S363: Neutron Star Astrophysics at the Crossroads: Magnetars and the Multimessenger Revolution , June 2020 , pp. 347 - 349
Copyright
© The Author(s), 2023. Published by Cambridge University Press on behalf of International Astronomical Union

Access options

Get access to the full version of this content by using one of the access options below. (Log in options will check for institutional or personal access. Content may require purchase if you do not have access.)

References

Beznogov, M. V., Potekhin, A. Y., & Yakovlev, D. G., 2021, Phys. Rep., 919, 1.CrossRefGoogle Scholar
Goldreich, P. & Reisenegger, A., 1992, ApJ, 395, 250.CrossRefGoogle Scholar
Gusakov, M. E., Kantor, E. M., & Ofengeim, D. D., 2017, Phys. Rev. D, 96, 103012.CrossRefGoogle Scholar
Gusakov, M. E., Kantor, E. M., & Ofengeim, D. D., 2020, MNRAS, 499, 4561.CrossRefGoogle Scholar
Pearson, J. M., Chamel, N., Potekhin, A. Y. ,, 2018, MNRAS, 481, 2994.Google Scholar
Potekhin, A. Y., Pons, J. A., & Page, D., 2015, Space Sci. Revs, 191, 239.Google Scholar
Potekhin, A. Y., Zyuzin, D. A., Yakovlev, D. G., Beznogov, M. V., Shibanov, Y. A., 2020, MNRAS, 496, 5052.CrossRefGoogle Scholar
Viganò, D., Rea, N., Pons, J. A., Perna, R., Aguilera, D. N., Miralles, J. A., 2013, MNRAS, 434, 123.Google Scholar
Yakovlev, D. G., Kaminker, A. D., Gnedin, O. Y., Haensel, P., 2001, Phys. Rep., 354, 1.CrossRefGoogle Scholar