pith. sign in

arxiv: 2605.22921 · v1 · pith:DHK4AOOQnew · submitted 2026-05-21 · 🌌 astro-ph.HE · gr-qc

Magnetic field dynamics in isolated neutron stars with an external dipole field

Aurora Capobianco , William Cook , Sebastiano Bernuzzi , Brynmor Haskell , Jacob Fields This is my paper

Pith reviewed 2026-05-25 05:28 UTC · model grok-4.3

classification 🌌 astro-ph.HE gr-qc
keywords neutron starsmagnetic fieldsnumerical relativityTayler instabilitypoloidal-toroidal configurationgravitational wavespulsarsmagnetars
0
0 comments X

The pith

Neutron star magnetic fields relax to a stable mixed poloidal-toroidal geometry with the toroidal component holding at most 10 percent of the total magnetic energy.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The paper runs long-term numerical-relativity simulations of isolated neutron stars that begin with an external dipole field and varying amounts of internal toroidal magnetic energy. It finds that the internal field always settles into a mixed poloidal-toroidal state where the toroidal share drops to 10 percent or less of the total magnetic energy, both inside and outside the star. This stable arrangement appears within roughly one Alfvén crossing time once Tayler instabilities have saturated, with gravitational-wave emission helping the process. A reader would care because the result limits which field shapes can persist in real neutron stars and therefore shapes models of pulsar signals, magnetar flares, and gravitational waves from magnetized merger remnants.

Core claim

The simulations reveal that the internal magnetic field relaxes toward a dynamically stable mixed poloidal-toroidal geometry, in which the toroidal component contributes to ≲10% of the total magnetic energy both in the exterior and in the interior. This configuration emerges within one Alfvén time following the saturation of the Tayler instabilities and is also aided by gravitational-wave emission.

What carries the argument

Long-term numerical-relativity simulations that evolve an initial external dipole field together with mixed poloidal-toroidal internal fields whose toroidal energy fraction ranges up to 80 percent.

If this is right

  • Long-lived neutron star magnetic fields are strongly constrained toward these stable mixed configurations.
  • Pulsar emission models must accommodate predominantly poloidal external fields with only a small toroidal contribution.
  • Magnetar evolution is limited by the low toroidal energy available for outbursts.
  • Gravitational-wave signals from magnetized neutron star remnants carry signatures of this rapid relaxation process.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • The same relaxation mechanism could operate in other compact objects where Alfvén times are short compared with evolutionary timescales.
  • Future gravitational-wave detections from neutron star mergers might show reduced magnetic energy in the toroidal component as a testable signature.
  • The 10 percent toroidal limit may explain why some observed pulsar fields appear stable over millions of years without requiring ongoing dynamo action.

Load-bearing premise

The numerical-relativity simulations accurately capture the long-term dynamical evolution, including the saturation of Tayler instabilities and the contribution of gravitational-wave emission, without being dominated by numerical artifacts or missing physics over the relevant timescales.

What would settle it

A simulation or observation in which a neutron star magnetic field maintains a toroidal energy fraction above 10 percent of the total after one Alfvén time without decaying would falsify the claimed relaxation.

Figures

Figures reproduced from arXiv: 2605.22921 by Aurora Capobianco, Brynmor Haskell, Jacob Fields, Sebastiano Bernuzzi, William Cook.

Figure 1
Figure 1. Figure 1: FIG. 1. Snapshots from the model Bt50 of the star from meridional view (top) and equatorial view (bottom) showing the [PITH_FULL_IMAGE:figures/full_fig_p004_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: FIG. 2. Alfvén time [PITH_FULL_IMAGE:figures/full_fig_p004_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: FIG. 3. 2D projections of the radial component [PITH_FULL_IMAGE:figures/full_fig_p005_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: FIG. 4. Evolution of the energies for all configurations. (Upper) The evolution of the toroidal component of the magnetic field [PITH_FULL_IMAGE:figures/full_fig_p006_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: FIG. 5. Time evolution of the electromagnetic luminosity [PITH_FULL_IMAGE:figures/full_fig_p006_5.png] view at source ↗
Figure 7
Figure 7. Figure 7: FIG. 7. Evolution of the spherical harmonic mode contribu [PITH_FULL_IMAGE:figures/full_fig_p007_7.png] view at source ↗
Figure 6
Figure 6. Figure 6: FIG. 6. Evolution of the spherical harmonic mode contribu [PITH_FULL_IMAGE:figures/full_fig_p007_6.png] view at source ↗
Figure 8
Figure 8. Figure 8: FIG. 8. Evolution of the spherical harmonic mode contribu [PITH_FULL_IMAGE:figures/full_fig_p008_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: FIG. 9. GW signal of Bt50 extracted at [PITH_FULL_IMAGE:figures/full_fig_p008_9.png] view at source ↗
Figure 11
Figure 11. Figure 11: FIG. 11. (Upper) Relative variation in each energy compo [PITH_FULL_IMAGE:figures/full_fig_p010_11.png] view at source ↗
read the original abstract

Neutron stars can harbor extremely strong magnetic fields, yet the structure and stability of their magnetic field configuration remain poorly understood. Observations of pulsars indicate that the large-scale external field is predominantly dipolar far from the star, while the internal magnetic configurations are largely unconstrained. We investigate the dynamical stability of magnetized neutron stars through long-term numerical-relativity simulations. We explore a range of models with an initial external dipole field and mixed poloidal-toroidal internal field where the energy of the toroidal component varies up to $80\%$ of the magnetic energy. We find that the internal magnetic field relaxes toward a dynamically stable mixed poloidal-toroidal geometry, in which the toroidal component contributes to $\lesssim10\%$ of the total magnetic energy both in the exterior and in the interior. This configuration emerges within one Alfv\'en time following the saturation of the Tayler instabilities and also aided by gravitational-wave emission. These results suggest that long-lived neutron star magnetic fields are strongly constrained toward stable mixed configurations, with important implications for pulsar emission models, magnetar evolution, and the interpretation of gravitational-wave signals from magnetized remnants.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 0 minor

Summary. The paper reports results from long-term numerical-relativity simulations of isolated neutron stars initialized with an external dipole field and internal mixed poloidal-toroidal magnetic fields (toroidal energy fraction up to 80%). The central claim is that the internal field relaxes to a dynamically stable mixed poloidal-toroidal geometry in which the toroidal component contributes ≲10% of the total magnetic energy both inside and outside the star; this configuration is reached within one Alfvén time after saturation of the Tayler instability and is aided by gravitational-wave emission.

Significance. If the numerical results hold, the finding would constrain the long-term stable magnetic configurations of neutron stars to mixed geometries with limited toroidal content, carrying implications for pulsar emission models, magnetar spin-down and outburst evolution, and the interpretation of gravitational-wave signals from magnetized merger remnants. The use of full numerical relativity to capture the coupled MHD, spacetime, and GW dynamics is a methodological strength.

major comments (2)
  1. [Abstract] Abstract and results presentation: the headline claim that the toroidal energy fraction relaxes to ≲10% within one Alfvén time after Tayler saturation rests on the assumption that the simulations accurately capture instability growth, nonlinear saturation, and energy redistribution. No information is supplied on grid resolution, AMR hierarchy, artificial dissipation coefficients, or convergence tests for the late-time toroidal fraction, making it impossible to assess whether the reported 10% limit is physical or set by numerical resistivity.
  2. [Results (implied)] The weakest assumption identified in the stress-test note is load-bearing: without demonstrated convergence of the toroidal energy fraction under increased resolution or varied dissipation parameters, the reported attractor configuration cannot be distinguished from an artifact of under-resolved dissipation on Alfvén timescales.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their thoughtful review and for highlighting the methodological strengths of our numerical-relativity approach. We address the concerns about numerical details and convergence below. We will revise the manuscript to supply the requested information and tests.

read point-by-point responses

  1. Referee: [Abstract] Abstract and results presentation: the headline claim that the toroidal energy fraction relaxes to ≲10% within one Alfvén time after Tayler saturation rests on the assumption that the simulations accurately capture instability growth, nonlinear saturation, and energy redistribution. No information is supplied on grid resolution, AMR hierarchy, artificial dissipation coefficients, or convergence tests for the late-time toroidal fraction, making it impossible to assess whether the reported 10% limit is physical or set by numerical resistivity.

    Authors: We agree that these numerical parameters are necessary to evaluate the robustness of the reported attractor. In the revised manuscript we will add a dedicated methods subsection (and, if appropriate, an appendix) that specifies the grid resolution, AMR hierarchy, artificial dissipation coefficients, and any convergence tests performed on the late-time toroidal energy fraction. This addition will allow readers to assess whether the ≲10% limit is physical. revision: yes

  2. Referee: [Results (implied)] The weakest assumption identified in the stress-test note is load-bearing: without demonstrated convergence of the toroidal energy fraction under increased resolution or varied dissipation parameters, the reported attractor configuration cannot be distinguished from an artifact of under-resolved dissipation on Alfvén timescales.

    Authors: We acknowledge that explicit convergence demonstrations are required to rule out numerical artifacts. While the models presented already exhibit consistent relaxation behavior, we will carry out and report additional higher-resolution runs and variations in dissipation parameters in the revised manuscript to confirm that the toroidal fraction limit is insensitive to these choices. revision: yes

Circularity Check

0 steps flagged

No significant circularity; results are direct simulation outputs

full rationale

The paper reports outcomes from numerical-relativity simulations of magnetic field evolution in neutron stars. The central claim—that the internal field relaxes to a mixed poloidal-toroidal state with toroidal energy fraction ≲10% within one Alfvén time after Tayler saturation—is presented as an emergent result of the simulations, not as a quantity defined by construction from fitted parameters, self-citations, or ansatzes. No self-definitional steps, fitted inputs renamed as predictions, or load-bearing self-citation chains appear in the abstract or described derivation. The work is self-contained against external benchmarks of simulation outputs.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

Based on abstract only; no free parameters, invented entities, or ad-hoc axioms are introduced in the provided text. The work relies on standard frameworks for numerical relativity.

axioms (1)
  • standard math The evolution of magnetized neutron stars is governed by the coupled equations of general relativity and ideal magnetohydrodynamics.
    This is the standard modeling framework invoked for numerical-relativity simulations of compact objects with magnetic fields.

pith-pipeline@v0.9.0 · 5738 in / 1448 out tokens · 33530 ms · 2026-05-25T05:28:59.567015+00:00 · methodology

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

77 extracted references · 47 canonical work pages · 27 internal anchors

  1. [1]

    varicose

    with a Courant-Friedrichs-Lewy factor of0.5. Af- ter each timestep, primitive variables are recovered from the conserved variables via a nonlinear inversion proce- dure [69]. Details of the primitive solver are provided in Appendix A of Cooket al.[61]. III. RESULTS A. Magnetic field evolution We begin by discussing the qualitative evolution of the magneti...

  2. [2]

    D. R. Lorimer and M. Kramer,Handbook of Pulsar As- tronomy, Vol. 4 (2004)

    2004

  3. [3]

    C. T. Y. Chung and A. Melatos, mnras411, 2471 (2011), arXiv:1010.2816 [astro-ph.SR]

    work page internal anchor Pith review Pith/arXiv arXiv 2011

  4. [4]

    C. T. Y. Chung and A. Melatos, mnras415, 1703 (2011), arXiv:1104.1016 [astro-ph.SR]

    work page internal anchor Pith review Pith/arXiv arXiv 2011

  5. [5]

    C. H. de Lima, B. Keeshan, H. E. Logan, and Y. Zhang, Phys. Rev. D103, 115034 (2021), arXiv:2010.06441 [hep- ph]

    work page arXiv 2021

  6. [6]

    K. C. Gendreau, Z. Arzoumanian, and T. Okajima, in Space Telescopes and Instrumentation 2012, Society of Photo-Optical Instrumentation Engineers (SPIE) Con- ference Series, Vol. 8443, edited by T. Takahashi, S. S. Murray, and J.-W. A. den Herder (2012) p. 844313

    2012

  7. [7]

    A. V. Bilous, A. L. Watts, A. K. Harding, T. E. Riley, Z. Arzoumanian, S. Bogdanov, K. C. Gendreau, P. S. Ray, S. Guillot, W. C. G. Ho, and D. Chakrabarty, The Astrophysical Journal Letters887, L23 (2019)

    2019

  8. [8]

    T. E. Rileyet al., Astrophys. J.887, L21 (2019), arXiv:1912.05702 [astro-ph.HE]

    work page arXiv 2019

  9. [9]

    T. E. Rileyet al., Astrophys. J. Lett.918, L27 (2021), arXiv:2105.06980 [astro-ph.HE]

    work page arXiv 2021

  10. [10]

    Choudhury, T

    D. Choudhury, T. Salmi, S. Vinciguerra, T. E. Riley, Y. Kini, A. L. Watts, B. Dorsman, S. Bogdanov, S. Guil- lot, P. S. Ray, D. J. Reardon, R. A. Remillard, A. V. Bilous, D. Huppenkothen, J. M. Lattimer, N. Ruther- ford, Z. Arzoumanian, K. C. Gendreau, S. M. Morsink, and W. C. G. Ho, Astrophys. J. Lett.971, L20 (2024), arXiv:2407.06789 [astro-ph.HE]

    work page arXiv 2024

  11. [11]

    Salmi, J

    T. Salmi, J. S. Deneva, P. S. Ray, A. L. Watts, D. Choud- hury, Y. Kini, S. Vinciguerra, H. T. Cromartie, M. T. Wolff, Z. Arzoumanian, S. Bogdanov, K. Gendreau, S. Guillot, W. C. G. Ho, S. M. Morsink, I. Cognard, L. Guillemot, G. Theureau, and M. Kerr, Astrophys. J. 976, 58 (2024), arXiv:2409.14923 [astro-ph.HE]

    work page arXiv 2024

  12. [12]

    Goldreich and W

    P. Goldreich and W. H. Julian, Astrophys. J.157, 869 (1969)

    1969

  13. [13]

    Thompson and R

    C. Thompson and R. C. Duncan, Mon. Not. Roy. Astron. Soc.275, 255 (1995)

    1995

  14. [14]

    Gravitational waves from pulsars: emission by the magnetic field induced distortion

    S. Bonazzola and E. Gourgoulhon, Astron. Astrophys. 312, 675 (1996), arXiv:astro-ph/9602107

    work page internal anchor Pith review Pith/arXiv arXiv 1996

  15. [15]

    R. J. Tayler, Proceedings of the Physical Society B70, 31 (1957)

    1957

  16. [16]

    R. J. Tayler, Mon. Not. R. Astron. Soc.161, 365 (1973)

    1973

  17. [17]

    G. A. E. Wright, Mon. Not. R. Astron. Soc.162, 339 (1973)

    1973

  18. [18]

    Markey and R

    P. Markey and R. J. Tayler, Mon. Not. R. Astron. Soc. 163, 77 (1973)

    1973

  19. [19]

    Markey and R

    P. Markey and R. J. Tayler, Mon. Not. R. Astron. Soc. 168, 505 (1974)

    1974

  20. [20]

    Flowers and M

    E. Flowers and M. A. Ruderman, Astrophys. J.215, 302 (1977)

    1977

  21. [21]

    Ciolfi, V

    R. Ciolfi, V. Ferrari, and L. Gualtieri, Monthly Notices of the Royal Astronomical Society406, 2540–2548 (2010)

    2010

  22. [22]

    Mastrano, A

    A. Mastrano, A. Melatos, A. Reisenegger, and T. Akgün, Monthly Notices of the Royal Astronomical Society417, 2288 (2011)

    2011

  23. [23]

    Twisted-torus configurations with large toroidal magnetic fields in relativistic stars

    R. Ciolfi and L. Rezzolla, Mon. Not. Roy. Astron. Soc. 435, L43 (2013), arXiv:1306.2803 [astro-ph.SR]

    work page internal anchor Pith review Pith/arXiv arXiv 2013

  24. [24]

    P. D. Lasky and A. Melatos, Phys. Rev. D88, 103005 (2013)

    2013

  25. [25]

    Mastrano, A

    A. Mastrano, A. G. Suvorov, and A. Melatos, Monthly Notices of the Royal Astronomical Society447, 3475–3485 (2015)

    2015

  26. [26]

    Castillo, A

    F. Castillo, A. Reisenegger, and J. A. Valdivia, Monthly Notices of the Royal Astronomical Society471, 507–522 (2017)

    2017

  27. [27]

    Stable magnetic fields in stellar interiors

    J. Braithwaite and A. Nordlund, Astron. Astrophys.450, 1077 (2006), arXiv:astro-ph/0510316

    work page internal anchor Pith review Pith/arXiv arXiv 2006

  28. [28]

    Axisymmetric magnetic fields in stars: relative strengths of poloidal and toroidal components

    J. Braithwaite, Mon. Not. R. Astron. Soc.397, 763 (2009), arXiv:0810.1049 [astro-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2009

  29. [29]

    Evolution of the magnetic field in magnetars

    J. Braithwaite and H. C. Spruit, Astron. Astrophys.450, 1097 (2006), arXiv:astro-ph/0510287

    work page internal anchor Pith review Pith/arXiv arXiv 2006

  30. [30]

    The stability of poloidal magnetic fields in rotating stars

    J. Braithwaite, Astron. Astrophys.469, 275 (2007), arXiv:0705.0185 [astro-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2007

  31. [31]

    Armaza, A

    C. Armaza, A. Reisenegger, and J. A. Valdivia, The As- trophysical Journal802, 121 (2015)

    2015

  32. [32]

    On non-axisymmetric magnetic equilibria in stars

    J. Braithwaite, Monthly Notices of the Royal Astronom- ical Society386, 1947 (2008), arXiv:0803.1661

    work page internal anchor Pith review Pith/arXiv arXiv 1947

  33. [33]

    Chandrasekhar and E

    S. Chandrasekhar and E. Fermi, Astrophys. J.118, 116 (1953)

    1953

  34. [34]

    Modelling magnetically deformed neutron stars

    B. Haskell, L. Samuelsson, K. Glampedakis, and N. An- dersson, Mon. Not. Roy. Astron. Soc.385, 531 (2008), arXiv:0705.1780 [astro-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2008

  35. [35]

    M. E. Gusakov, E. M. Kantor, and D. D. Ofengeim, Phys. Rev. D96, 103012 (2017), arXiv:1705.00508 [astro- ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  36. [36]

    D. D. Ofengeim and M. E. Gusakov, Phys. Rev. D98, 043007 (2018), arXiv:1805.03956 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  37. [37]

    Ciolfi, V

    R. Ciolfi, V. Ferrari, L. Gualtieri, and J. A. Pons, Monthly Notices of the Royal Astronomical Society397, 913 (2009), https://academic.oup.com/mnras/article- 12 pdf/397/2/913/2939394/mnras0397-0913.pdf

    2009

  38. [38]

    Instability-driven evolution of poloidal magnetic fields in relativistic stars

    R. Ciolfi, S. K. Lander, G. M. Manca, and L. Rezzolla, Astrophys.J.736, L6 (2011), arXiv:1105.3971 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2011

  39. [39]

    S. K. Lander and D. I. Jones, Mon. Not. Roy. Astron. Soc.395, 2162 (2009), arXiv:0903.0827 [astro-ph.SR]

    work page internal anchor Pith review Pith/arXiv arXiv 2009

  40. [40]

    S. K. Lander and D. I. Jones, Mon. Not. R. Astron. Soc. 412, 1730 (2011), arXiv:1010.0614 [astro-ph.SR]

    work page internal anchor Pith review Pith/arXiv arXiv 2011

  41. [41]

    A. Sur, B. Haskell, and E. Kuhn, Mon. Not. Roy. Astron. Soc.495, 1360 (2020), arXiv:2002.10357 [astro-ph.HE]

    work page arXiv 2020

  42. [42]

    Herbrik and K

    M. Herbrik and K. D. Kokkotas, Monthly Notices of the Royal Astronomical Society466, 1330–1347 (2016)

    2016

  43. [43]

    S. G. Frederick, K. L. Thompson, and M. P. Kuchera, Monthly Notices of the Royal Astronomical Society503, 2764 (2021)

    2021

  44. [44]

    Kiuchi, M

    K. Kiuchi, M. Shibata, and S. Yoshida, Phys. Rev. D78, 024029 (2008)

    2008

  45. [45]

    P. D. Lasky, B. Zink, K. D. Kokkotas, and K. Glampedakis, Astrophys. J. Lett.735, L20 (2011), arXiv:1105.1895 [astro-ph.SR]

    work page internal anchor Pith review Pith/arXiv arXiv 2011

  46. [46]

    P. D. Lasky, B. Zink, and K. D. Kokkotas, (2012), arXiv:1203.3590 [astro-ph.SR]

    work page internal anchor Pith review Pith/arXiv arXiv 2012

  47. [47]

    Poloidal-Field Instability in Magnetized Relativistic Stars

    R. Ciolfi and L. Rezzolla, Astrophys. J.760, 1 (2012), arXiv:1206.6604 [astro-ph.SR]

    work page internal anchor Pith review Pith/arXiv arXiv 2012

  48. [48]

    A. G. Pili, N. Bucciantini, and L. Del Zanna, Mon. Not.Roy.Astron.Soc.439,3541(2014),arXiv:1401.4308 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2014

  49. [49]

    A. G. Pili, N. Bucciantini, and L. Del Zanna, Mon. Not. Roy. Astron. Soc.470, 2469 (2017), arXiv:1705.03795 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  50. [50]

    Tsokaros, M

    A. Tsokaros, M. Ruiz, S. L. Shapiro, and K. Ury¯ u, Phys. Rev. Lett.128, 061101 (2022), arXiv:2111.00013 [gr-qc]

    work page arXiv 2022

  51. [51]

    A. Sur, W. Cook, D. Radice, B. Haskell, and S. Bernuzzi, Mon. Not. Roy. Astron. Soc.511, 3983 (2022), arXiv:2108.11858 [astro-ph.HE]

    work page arXiv 2022

  52. [52]

    P. C.-K. Cheong, A. Tsokaros, M. Ruiz, F. Venturi, J. C. L. Chan, A. K. L. Yip, and K. Uryu, (2024), arXiv:2409.10508 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2024

  53. [53]

    W. Cook, R. K. Joshi, S. Bernuzzi, B. Haskell, and J. Fields, (2025), arXiv:2506.08037 [astro-ph.HE]

    work page arXiv 2025

  54. [54]

    J. M. Stone, K. Tomida, C. J. White, and K. G. Felker, Astrophys. J. Suppl.249, 4 (2020), arXiv:2005.06651 [astro-ph.IM]

    work page arXiv 2020

  55. [55]

    A five-wave HLL Riemann solver for relativistic MHD

    A. Mignone, M. Ugliano, and G. Bodo, Mon. Not. Roy. Astron. Soc.393, 1141 (2009), arXiv:0811.1483 [astro- ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2009

  56. [56]

    J. M. Stone, P. D. Mullen, D. Fielding, P. Grete, M. Guo, P. Kempski, E. R. Most, C. J. White, and G. N. Wong, arXiv e-prints , arXiv:2409.16053 (2024), arXiv:2409.16053 [astro-ph.IM]

    work page arXiv 2024

  57. [57]

    H. Zhu, J. Fields, F. Zappa, D. Radice, J. M. Stone, A. Rashti, W. Cook, S. Bernuzzi, and B. Daszuta, Astro- phys. J. Suppl.278, 50 (2025), arXiv:2409.10383 [gr-qc]

    work page arXiv 2025

  58. [58]

    Fields, H

    J. Fields, H. Zhu, D. Radice, J. M. Stone, W. Cook, S. Bernuzzi, and B. Daszuta, Astrophys. J. Suppl.276, 35 (2025), arXiv:2409.10384 [astro-ph.HE]

    work page arXiv 2025

  59. [59]

    Constraint violation in free evolution schemes: comparing BSSNOK with a conformal decomposition of Z4

    S. Bernuzzi and D. Hilditch, Phys. Rev.D81, 084003 (2010), arXiv:0912.2920 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2010

  60. [60]

    Compact binary evolutions with the Z4c formulation

    D. Hilditch, S. Bernuzzi, M. Thierfelder, Z. Cao, W. Tichy, and B. Bruegmann, Phys. Rev.D88, 084057 (2013), arXiv:1212.2901 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2013

  61. [61]

    Dimmelmeier, N

    H. Dimmelmeier, N. Stergioulas, and J. A. Font, Mon. Not. Roy. Astron. Soc.368, 1609 (2006), arXiv:astro- ph/0511394

    work page arXiv 2006

  62. [62]

    W. Cook, B. Daszuta, J. Fields, P. Hammond, S. Al- banesi, F. Zappa, S. Bernuzzi, and D. Radice, Astrophys. J. Suppl.277, 3 (2025), arXiv:2311.04989 [gr-qc]

    work page arXiv 2025

  63. [63]

    Colella and M

    P. Colella and M. D. Sekora, Journal of Computational Physics227, 7069 (2008)

    2008

  64. [64]

    Harten, J

    A. Harten, J. Comput. Phys.135, 260 (1983)

    1983

  65. [65]

    Einfeldt, SIAM J

    B. Einfeldt, SIAM J. Numer. Anal.25, 294 (1988)

    1988

  66. [66]

    M.N.LemasterandJ.M.Stone,TheAstrophysicalJour- nal691, 1092–1108 (2009)

    2009

  67. [67]

    C. R. Evans and J. F. Hawley, Astrophys. J.332, 659 (1988)

    1988

  68. [68]

    T. A. Gardiner and J. M. Stone, J. Comput. Phys.227, 4123 (2008), arXiv:0712.2634 [astro-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2008

  69. [69]

    Gottlieb and C.-W

    S. Gottlieb and C.-W. Ketcheson, David I.and Shu, Jour- nal of Scientific Computing38, 251 (2009)

    2009

  70. [70]

    Kastaun, J

    W. Kastaun, J. V. Kalinani, and R. Ciolfi, Phys. Rev. D 103, 023018 (2021), arXiv:2005.01821 [gr-qc]

    work page arXiv 2021

  71. [71]

    Piñas, A

    F. Piñas, A. Yip, P. C.-K. Cheong, and M. Ruiz, The Astrophysical Journal1001, 49 (2026)

    2026

  72. [72]

    Fontbuté, S

    J. Fontbuté, S. Bernuzzi, S. Albanesi, D. Radice, A. Rashti, W. Cook, B. Daszuta, and A. Nagar, Phys. Rev. D113, 064036 (2026), arXiv:2508.03799 [gr-qc]

    work page arXiv 2026

  73. [73]

    Gravitational-Wave Extraction from Neutron Star Oscillations: comparing linear and nonlinear techniques

    L. Baiotti, S. Bernuzzi, G. Corvino, R. De Pietri, and A. Nagar, Phys. Rev.D79, 024002 (2009), arXiv:0808.4002 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2009

  74. [74]

    C. D. Ott, Class.Quant.Grav.26, 063001 (2009), arXiv:0809.0695 [astro-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2009

  75. [75]

    C. Afle, S. K. Kundu, J. Cammerino, E. R. Coughlin, D. A. Brown, D. Vartanyan, and A. Burrows, Physical Review D107, 10.1103/physrevd.107.123005 (2023)

    work page doi:10.1103/physrevd.107.123005 2023

  76. [76]

    P. D. Lasky, Publications of the Astronomical Society of Australia32, 10.1017/pasa.2015.35 (2015)

    work page doi:10.1017/pasa.2015.35 2015

  77. [77]

    Jülich Supercomputing Centre, Journal of large-scale re- search facilities7, 10.17815/jlsrf-7-183 (2021)

    work page doi:10.17815/jlsrf-7-183 2021