Magnetized neutron stars: perturbative versus fully-numerical approaches
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arXiv
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| Format: | Preprint |
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2026
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| author | Chatterjee, Debarati Guttmann, Daw Novak, Jérôme Oertel, Micaela Steil, Martin Jakob |
| author_facet | Chatterjee, Debarati Guttmann, Daw Novak, Jérôme Oertel, Micaela Steil, Martin Jakob |
| contents | (1) Background: for the study of highly magnetized neutron
stars observed as magnetars, and to quantify the effect of this
intense magnetic field onto the star's structure and shape which
can be particularly relevant for the study of emission of continuous
gravitational waves, both numerical and perturbative approaches have been developed. (2) Methods: we compare these two approaches in General
Relativity with the limitation to the case where the magnetic field has a
purely poloidal structure. The perturbative one (Konno-99)
assumes that the deformation induced by the magnetic field is small
and that this field arises only from dipole currents. The full
numerical one is based on the library LORENE. (3) Results: we have used both
approaches to compute the magnetic field distribution and the
deformation of the star, varying the value of the magnetic field at
the pole, the compactness of the star and its equation of state. (4)
Conclusions: whereas the perturbative approach breaks down for very
high polar magnetic field values (typically above a few times
$10^{16}$ G), it gives very good results for observed values, even
in magnetars. On the contrary, the numerical code exhibits
resolution problems for relatively low magnetic field values
(typically $10^{10}$ G), which translates into imprecise computation of the star's
deformation and mass quadrupole moment. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2605_19761 |
| institution | arXiv |
| publishDate | 2026 |
| record_format | arxiv |
| spellingShingle | Magnetized neutron stars: perturbative versus fully-numerical approaches Chatterjee, Debarati Guttmann, Daw Novak, Jérôme Oertel, Micaela Steil, Martin Jakob High Energy Astrophysical Phenomena General Relativity and Quantum Cosmology Nuclear Theory (1) Background: for the study of highly magnetized neutron stars observed as magnetars, and to quantify the effect of this intense magnetic field onto the star's structure and shape which can be particularly relevant for the study of emission of continuous gravitational waves, both numerical and perturbative approaches have been developed. (2) Methods: we compare these two approaches in General Relativity with the limitation to the case where the magnetic field has a purely poloidal structure. The perturbative one (Konno-99) assumes that the deformation induced by the magnetic field is small and that this field arises only from dipole currents. The full numerical one is based on the library LORENE. (3) Results: we have used both approaches to compute the magnetic field distribution and the deformation of the star, varying the value of the magnetic field at the pole, the compactness of the star and its equation of state. (4) Conclusions: whereas the perturbative approach breaks down for very high polar magnetic field values (typically above a few times $10^{16}$ G), it gives very good results for observed values, even in magnetars. On the contrary, the numerical code exhibits resolution problems for relatively low magnetic field values (typically $10^{10}$ G), which translates into imprecise computation of the star's deformation and mass quadrupole moment. |
| title | Magnetized neutron stars: perturbative versus fully-numerical approaches |
| topic | High Energy Astrophysical Phenomena General Relativity and Quantum Cosmology Nuclear Theory |
| url | https://arxiv.org/abs/2605.19761 |