Deformation of relativistic magnetized stars

K. Konno; T. Obata; Y. Kojima

RECORD

Deformation of relativistic magnetized stars

K. Konno, T. Obata, Y. Kojima

General Relativity and Quantum Cosmology · Submitted 12 Oct 1999

abstract compiled · 2026-09-23 · no language-model review

The authors' main claim We have found that the ellipticity becomes large with increase of a relativistic factor for the models with the same energy ratio of the magnetic energy to the gravitational energy.

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What the abstract itself states, as probabilities: claims first 0.03 · states limitation 0.24 · human participants 0.01 · controlled comparison 0.09 · randomized assignment 0.01 · states quantitative result 0.10 · compares with prior results 0.07 · mentions code or data availability 0.02.

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arXiv listing abstract v1. Results and the main claim are underlined; show every role.

We formulate deformation of relativistic stars due to the magnetic stress, considering the magnetic fields to be perturbations from spherical stars. The ellipticity for the dipole magnetic field is calculated for some stellar models. We have found that the ellipticity becomes large with increase of a relativistic factor for the models with the same energy ratio of the magnetic energy to the gravitational energy.

background contribution method result interpretation main claim

What the classifier reports for each sentence. The number is the probability it gave the label.
#	sentence	role	the authors' own work	states the main conclusion	strength
s0	We formulate deformation of relativistic stars due to the magnetic stress, considering the magnetic fields to be perturbations from spherical stars.	contribution 0.65	0.91	0.05	asserted 0.95
s1	The ellipticity for the dipole magnetic field is calculated for some stellar models.	method 0.52	0.92	0.06	asserted 0.98
s2	We have found that the ellipticity becomes large with increase of a relativistic factor for the models with the same energy ratio of the magnetic energy to the gravitational energy.	result 1.00	0.95	0.83	asserted 1.00

What kind of paper the classifier reports this is: theoretical result 0.99 · evidence from simulation or computation 0.56.

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arXiv listing abstract v1

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full text
figures and tables
references and citing sentences
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P abstract

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S sections
T body sentences
C citations
R cross-paper relations

Every quoted sentence on this record is the authors'. Every label is from Pith's closed vocabulary, with the probability shown beside it. Every number in the measurements table is the authors', checked by code. Record as JSON

The paper

Original abstract

We formulate deformation of relativistic stars due to the magnetic stress, considering the magnetic fields to be perturbations from spherical stars. The ellipticity for the dipole magnetic field is calculated for some stellar models. We have found that the ellipticity becomes large with increase of a relativistic factor for the models with the same energy ratio of the magnetic energy to the gravitational energy.

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References

Forward citations

Cited by 6 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

Magnetoelastic avalanches in magnetar crusts with plastic islands
astro-ph.HE 2026-10 accept novelty 7.0 of 10

Magnetar crust failures can trigger avalanche-like cascades and produce transient oscillation frequencies that resemble observed quasi-periodic oscillations.
Universal Relations for Neutron Stars from Asymptotic Analysis
gr-qc 2026-08 conditional novelty 7.0 of 10

Asymptotic analysis of the relativistic stellar structure equations shows that the I-Love-Q and Love-C universal relations are controlled by two integration constants and one polytrope index, with percent-level deviat...
New Universal Relations for Magnetized Neutron Stars
gr-qc 2026-08 conditional novelty 7.0 of 10

Magnetized neutron stars with dipole fields obey a new exact relation between dipole moment and compactness, and approximate EoS-insensitive relations among dipole moment, quadrupole moment, and ellipticity.
Shirokov and Shapiro Effects in the Hartle-Thorne Spacetime
gr-qc 2026-05 unverdicted novelty 5.0 of 10

In the Hartle-Thorne metric, angular momentum J and quadrupole moment Q couple radial and azimuthal oscillations in the Shirokov effect and alter Shapiro time delay, with oblate shapes increasing delay and frame-dragg...
Magnetized neutron stars: perturbative versus fully-numerical approaches
astro-ph.HE 2026-05 conditional novelty 4.0 of 10

Direct comparison of Konno-99 perturbative and LORENE numerical methods for poloidal magnetized neutron stars shows perturbative validity for observed fields up to ~10^16 G and numerical resolution limits below ~10^10 G.

Show 1 more citing papers

Approximate Universal Relations for Neutron Stars and Quark Stars
gr-qc 2016-08 accept novelty 2.0 of 10

Neutron stars and quark stars obey approximate universal relations among their moment of inertia, tidal Love number, quadrupole moment, and higher multipoles, with residuals of about 1% to 10% across a broad set of eq...

How the literature uses it

10 arXiv papers cite this in 27 sentences

Each citing sentence is taken from the citing paper's LaTeX source and typed by Pith's classifier. A label appears at probability 0.8 or more (0.95 for support), a contest at 0.7 or more; the quoted words are the citing authors'. How each label was checked · JSON

Papers citing it · 18 sentences without a confident label

Uses its method or tool 3 papers

Following Ref. [ref] , we expand $A_i$ and $J_i$ onto vector spherical harmonics and consider only a dipole magnetic field, $ℓ=1$.

Magnetized neutron stars: perturbative versus fully-numerical approaches · Magnetic field · 0.99
The relation between the vector potential and the radial component of the magnetic field at $θ=0$ is [Note that, as in [ref] , we use here the tetrad components of the magnetic field.] [ref] :

The gravitational Higgs mechanism and resulting smoking gun effects · Approach · 0.95
The resulting system of perturbation equation are then given by [ref]

Tidal deformability and gravitational-wave phase evolution of magnetised compact-star binaries · First-order magnetic-field perturbations · 0.88

Cites it as background 2 papers

Various approaches are possible here, with different assumptions and ansatz, going from semi-analytic models based on the perturbation of a spherically symmetric background star [ref] , to full numerical ones following first studies by e.g. [ref] .

Magnetized neutron stars: perturbative versus fully-numerical approaches · Introduction · 0.86
Unlike black holes, neutron stars possess a finite surface and their shape can deviate from spherical symmetry as a result of rotation, tidal deformation, and extreme magnetic fields [ref] .

Shirokov and Shapiro Effects in the Hartle-Thorne Spacetime · Introduction · 0.86

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