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Peer-reviewedCC BYLiving Reviews in Computational Astrophysics

Magnetic, thermal and rotational evolution of isolated neutron stars

  • JOSE A. PONS1,2
  • Clara Dehman1,3
  • Daniele Viganò4,5
5 affiliations
  1. 1Departament de Física Aplicada, Universitat d'Alacant, Alicante, Spain
  2. 2Departament de Física Aplicada, Universitat d'Alacant, 03690, Alicante, Spain
  3. 3Departament de Física, Institut d'Estudis Espacials de Catalunya and Institut d'Aplicacions Computacionals de Codi Comunitari (IAC3), Universitat de les Illes Balears, 07122, Palma de Mallorca, Baleares, Spain
  4. 4Institut d'Estudis Espacials de Catalunya (IEEC), 08860 Castelldefels, Catalonia Spain
  5. 5Institut de Ciències de I'Espai (ICE-CSIC), Campus UAB, Carrer de Can Magrans s/n, 08193 Cerdanyola del Vallès, Catalonia Spain
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Abstract

The strong magnetic fields of neutron stars are closely linked to their observed thermal, spectral, and timing properties, such as the distribution of spin periods and their derivatives. To understand the evolution of astrophysical observables over time, it is essential to develop robust theoretical frameworks and numerical models that solve the coupled thermal and magnetic field evolution equations, incorporating detailed microphysics such as thermal and electrical conductivities and neutrino emission rates. These efforts are key to uncovering how the strength and geometry of magnetic fields change with age, ultimately shedding light on the diverse phenomenology of neutron stars. In this review, we outline the fundamental theory underlying magneto-thermal evolution models, with an emphasis on numerical methods and a comprehensive set of benchmark tests intended to guide current and future code development. We revisit established results from axisymmetric simulations, highlight recent progress in fully three-dimensional models, and offer a perspective on the anticipated developments in this rapidly evolving field. Supplementary Information: The online version contains supplementary material available at 10.1007/s41115-026-00028-4.

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Cite

BibTeXRIS
BibTeX
@article{pons2026magnetic,
  title = {{Magnetic, thermal and rotational evolution of isolated neutron stars}},
  author = {JOSE A. PONS and Clara Dehman and Daniele Viganò},
  journal = {Living Reviews in Computational Astrophysics},
  year = {2026},
  month = jun,
  doi = {10.1007/s41115-026-00028-4},
  url = {https://doi.org/10.1007/s41115-026-00028-4},
  note = {CC BY},
}
RIS
TY  - JOUR
TI  - Magnetic, thermal and rotational evolution of isolated neutron stars
AU  - JOSE A. PONS
AU  - Clara Dehman
AU  - Daniele Viganò
PY  - 2026
DA  - 2026/06/09
JO  - Living Reviews in Computational Astrophysics
DO  - 10.1007/s41115-026-00028-4
UR  - https://doi.org/10.1007/s41115-026-00028-4
AB  - The strong magnetic fields of neutron stars are closely linked to their observed thermal, spectral, and timing properties, such as the distribution of spin periods and their derivatives. To understand the evolution of astrophysical observables over time, it is essential to develop robust theoretical frameworks and numerical models that solve the coupled thermal and magnetic field evolution equations, incorporating detailed microphysics such as thermal and electrical conductivities and neutrino emission rates. These efforts are key to uncovering how the strength and geometry of magnetic fields change with age, ultimately shedding light on the diverse phenomenology of neutron stars. In this review, we outline the fundamental theory underlying magneto-thermal evolution models, with an emphasis on numerical methods and a comprehensive set of benchmark tests intended to guide current and future code development. We revisit established results from axisymmetric simulations, highlight recent progress in fully three-dimensional models, and offer a perspective on the anticipated developments in this rapidly evolving field. Supplementary Information: The online version contains supplementary material available at 10.1007/s41115-026-00028-4.
SN  - 2365-0524
SN  - 2367-3621
ER  -