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Impact of magnetic field-driven anisotropies on the equation of state probed in neutron star mergers

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Pith's one-line read Magnetar-strength magnetic fields in neutron star mergers can make the local pressure of dense matter anisotropic, with >10 percent corrections concentrated in the outer layers of the remnant.

desk verdict Useful first upper-bound estimate of field-driven anisotropies in merger remnants, undercut by a sign error in the backreacted energy density that needs fixing before the feedback comparisons are trusted. read the letter →

arxiv 2506.21696 v1 pith:BGQ477C6 submitted 2025-06-26 astro-ph.HE gr-qcnucl-th

Elias R. Most , Jeffrey Peterson , Luigi Scurto , Helena Pais , Veronica Dexheimer This is my paper
classification astro-ph.HEgr-qcnucl-th
keywords neutronstarmergersmagneticfieldanisotropyequationofstateLandauquantizationanomalousmomentmagnetarremnantsgeneral-relativisticmagnetohydrodynamicsmean-fielddynamo
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

This paper asks whether the extreme magnetic fields produced in a binary neutron star merger are strong enough to change the equation of state of the matter itself, not just the dynamics of the magnetic field. By building two magnetized equations of state that include Landau-level quantization and the anomalous magnetic moment, and by adding a magnetic polarization tensor to a full general-relativistic merger simulation, the authors find that fields above about $10^{17}\,\mathrm{G}$ make the local pressure anisotropic: the pressure parallel to the field differs from the pressure perpendicular to it. In the most favorable case considered, the anisotropy exceeds $10\%$, and it is largest in the outer, crustal layers of the hypermassive remnant rather than in the dense core. The core anisotropies stay at the $10^{-3}$ to $10^{-4}$ level, so the effect does not change the bulk dynamics but could matter wherever magnetic breakout, winds, or jets are launched. The paper presents this as a first assessment and explicitly notes that finite-temperature corrections, which are neglected, would lower the effect.

What carries the argument

The load-bearing object is the magnetic polarization tensor $T^{\mu\nu}_{\mathrm{mag}} = \tfrac12 (m^\mu b^\nu + m^\nu b^\mu) - (u^\mu u^\nu + g^{\mu\nu}) b^\alpha m_\alpha$, with polarization aligned with the comoving field, $m^\mu = \mu b^\mu$, where the magnetic susceptibility $\mu = (P_\perp - P_\parallel)/b^2$ is supplied by the equation of state. When substituted into the ideal MHD equations, this produces an effective pressure $\tilde P = \tfrac32 P_\parallel - \tfrac12 P_\perp$ and a rescaled field $\tilde b^\mu = \sqrt{1-\mu}\, b^\mu$, which lets the scheme keep the structure of ideal GRMHD while absorbing the anisotropy as a bulk-pressure-like correction. The second piece is a mean-field dynamo term with a chosen saturation magnetization $\sigma_B = b^2/\rho$, whose value controls how much of the remnant reaches magnetar-level fields. Landau-level quantization and the anomalous magnetic moment, evaluated in two distinct relativistic mean-field equations of state, are what turn those strong fields into a genuine $P_\parallel \neq P_\perp$.

What would settle it

Run a general-relativistic MHD merger simulation that resolves the Kelvin-Helmholtz and magnetorotational dynamo without any prescribed saturation, and measure the crustal magnetization $b^2/\rho$ (equivalently the local field strength around densities $n_B \lesssim 0.1\,\mathrm{fm}^{-3}$). If it stays below about $3\times 10^{-3}$ (fields below roughly $10^{17}\,\mathrm{G}$), the paper's most optimistic 10-percent anisotropy cannot occur.

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Extended reading notes

Core claim

The central claim is that magnetar-strength magnetic fields in the aftermath of a neutron star merger can alter the local equation of state enough to make the pressure tensor non-negligibly anisotropic, with the effect concentrated in the low-density outer layers of the remnant. The paper reports the first numerical-relativity simulation that includes a magnetic polarization tensor and a magnetic-field-dependent equation of state, using two nuclear models (a Walecka-type NL3ωρ model with a compressible liquid-drop crust and a chiral mean-field model with hyperons) that both treat Landau quantization and the anomalous magnetic moment. In the most optimistic dynamo scenario, where the outer layers are driven to a magnetization $b^2/\rho = 0.02$, local anisotropies $(P_\parallel - P_\perp)/P_\parallel$ reach order unity near the surface and average corrections in excess of $10\%$, while the dense core shows only $10^{-3}$ to $10^{-4}$ corrections. The paper argues that this makes the correction dynamically irrelevant for the core but potentially relevant for the crustal regions where magnetic breakout and wind and jet launching occur.

Load-bearing premise

The 10-percent result rests on the assumption that the outer layers of the remnant really reach the highest dynamo-saturation level the simulations impose ($b^2/\rho = 0.02$); if real turbulence stops at weaker fields, the large anisotropy does not occur.

Editorial extensions

If this is right

  • If the most optimistic saturation $\sigma_B = 0.02$ is realized, local pressure anisotropies in the outer layers of the remnant exceed 10 percent and can approach order unity, making the equation of state itself anisotropic where the field is near equipartition.
  • Core anisotropies remain at the $10^{-3}$ to $10^{-4}$ level, so the merger dynamics and gravitational-wave signal are essentially unaffected by the magnetic-field-driven equation-of-state corrections.
  • Because the anisotropy is sourced by shear-driven dynamo amplification and is non-dissipative, it persists after the dynamo saturates rather than decaying like bulk viscosity.
  • The magnitude is equation-of-state dependent: the CMF model with hyperons shows stronger effects than NL3ωρ, so nuclear-model uncertainties feed directly into whether the crustal correction is dynamically important.
  • Finite-temperature effects are not included, so the published values should be read as an upper bound on the anisotropy.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • A natural testable extension is to replace the hand-set dynamo saturation with a resolved magnetorotational-instability dynamo: the central 10-percent result would only survive if the computed crustal magnetization actually reaches $b^2/\rho \simeq 0.02$.
  • The same polarization-tensor formulation could be applied to isolated magnetar models, where the field is quasi-steady rather than transient, to ask whether crustal anisotropy changes crustal oscillation frequencies or magnetic breakout timescales.
  • If the anisotropy does reach 10 percent in the outer layers, the effective sound speed there changes by a comparable amount, which could leave a small imprint on the post-merger gravitational-wave spectrum even though the core average is tiny.
  • A self-consistent finite-temperature magnetized equation of state would likely shift the anisotropy pattern; because the paper neglects this, the actual merger signal may be closer to the $\sigma_B = 0.003$ case than to the headline 10-percent case.
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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

2 major / 5 minor

Summary. This manuscript studies whether magnetic fields amplified in binary neutron star mergers can make the equation of state anisotropic. The authors construct two zero-temperature, magnetic-field-dependent nuclear equations of state (CMF and NL3ωρ) including Landau quantization and the anomalous magnetic moment, and run general-relativistic magnetohydrodynamic merger simulations with a mean-field dynamo. They post-process the pressure anisotropy (P∥−P⊥)/P∥ and also perform "backreacted" runs using an effective polarizable-MHD system. For the largest imposed dynamo saturation (σB=0.02) they find anisotropies exceeding 10% in the outer crustal layers, while core anisotropies remain at the 10^-3–10^-4 level. The paper argues that this is a first step toward including magnetic-field feedback on the EoS in merger simulations.

Significance. The physical question is novel and timely: merger remnants can reach magnetar-level fields, and magnetic-field effects on the EoS have so far been neglected in this context. The post-processed anisotropy maps are a direct, transparent evaluation of the tabulated EoSs at simulated field strengths, and the two EoS models provide some microphysical diversity. The authors are honest about the upper-bound nature of the estimate and about neglected finite-temperature corrections. However, the methodological centerpiece—the first simulation with a magnetic polarization tensor—is currently undermined by an algebraic sign error in the effective energy density, which affects the backreacted runs and the feedback comparison. If the sign is corrected, this would be a valuable first assessment and a useful reference for future work.

major comments (2)
  1. [Sec. 3, Eq. (14)] The expression for the effective energy density is algebraically inconsistent with the stated polarization model. Combining Eq. (9) with m^μ = μ b^μ gives T_mag^{μν} = μ b^μ b^ν − μ b^2 (u^μ u^ν + g^{μν}). Adding this to Eq. (7) and matching to the effective ideal form Eq. (12) with \tilde b^μ = sqrt(1−μ) b^μ yields \tilde e = e + μ b^2/2 = e + (P⊥ − P∥)/2, whereas Eq. (14) states \tilde e = e − (P⊥ − P∥)/2. Equations (13) and (15) are consistent with the plus sign, so this is a genuine sign error, not a convention choice. Because \tilde e enters the conservative energy and the primitive inversion in Appendix B, the "(B)" runs may solve a different system, and the feedback comparison in Fig. 5 is not currently supported. The post-processed maps in Fig. 4 are unaffected; please correct the implementation or the equation and rerun, and state whether the conclusions of Fig. 5 change.
  2. [Sec. 4 and Fig. 2] The quantitative claim of "corrections in excess of 10%" is realized only for the imposed dynamo saturation σB = b^2/ρ = 0.02, which is an input parameter of the mean-field dynamo model rather than a result of the simulated turbulence. The authors honestly label this the most optimistic case, but the abstract and conclusions should more explicitly state that this is a scenario based on an assumed magnetization, and should give the corresponding anisotropy at the lower saturation σB = 0.003 (visible in Fig. 5) so that the sensitivity of the headline number to the dynamo assumption is clear. Without this, the reader may misread the 10% as a robust prediction rather than an upper bound under a hypothetical saturation.
minor comments (5)
  1. [Appendix B, step 4] The polarization used to rescale the magnetic field is denoted ¯κ, but the susceptibility defined in Sec. 3 is μ; the same symbol κ is also used for the dynamo coefficient (Eq. 4) and the AMM couplings (Table 1). Please use a distinct symbol for the susceptibility.
  2. [Fig. 4 and Sec. 2] The text defines the magnetic susceptibility as μ=(P⊥−P∥)/b^2, while the bottom panels of Fig. 4 plot |P∥−P⊥|/b^2; the sign convention should be stated explicitly in the caption.
  3. [Abstract] The phrase "corrections to the anisotropy" is ambiguous; it should read "pressure anisotropies" or "corrections to the equation of state".
  4. [Sec. 5.1] The order-of-magnitude ranges Π≃10^{-3}–10^{-4}P∥ and Π≃10^{-2}–10^{-1}P∥ would be clearer if tied to the corresponding density ranges (core vs crust) in the same sentence.
  5. [Sec. 3, Eq. (20)] The evolution equation for Π appears to be derived from thermodynamic derivatives, but it is not stated whether this is an exact consequence of the EoS or an additional approximation; please clarify.

Circularity Check

0 steps flagged · score 2.0 of 10

No circular derivation: the anisotropy is evaluated from tabulated microphysical EoS tables at locally evolved field strengths, with the dynamo saturation imposed as an explicit input, not fitted to the reported >10% result.

full rationale

The paper's central quantity, (P∥−P⊥)/P∥, is not an output of a fit or of a self-citation chain. It is tabulated from the NL3ωρ and CMF microphysical models (Appendix A) and evaluated either in post-processing or in the backreacted runs at the local comoving field strength from the GRMHD evolution. The dynamo saturation levels σB = b²/ρ = {0.003, 0.02} are imposed inputs chosen to vary the amplification (Sec. 4), and the paper explicitly labels the larger value as the 'most optimistic case' and calls its results an upper bound, so the >10% statement is a conditional parameter-study result rather than a quantity equal to its input by construction. The effective transformation in Eqs. (12)–(15) recasts the polarizable-fluid stress tensor into ideal-MHD form; even if Eq. (14)'s sign were wrong (a correctness issue raised by the skeptic), the post-processed anisotropy maps would not be circular because they do not use the effective energy density. Self-citations to E. R. Most 2023 and Most & Quataert 2023 supply the mean-field dynamo ansatz and saturation conventions, but those are modeling inputs with stated parameters, not a uniqueness theorem or an unverified premise that itself contains the 10% claim. The only reason not to set 0 is the presence of minor self-citations for the dynamo model; these are not load-bearing and would not change the anisotropy result if replaced by another field-strength prescription. No circular steps are therefore exhibited.

Assumptions & free parameters 2 free parameters · 5 assumptions · 0 invented entities

The central estimate rests on (i) the magnetized EoS models, which are prior work fitted to nuclear data, (ii) the assumed dynamo saturation magnetization, which is imposed by hand, (iii) the zero-temperature treatment, which the authors flag as an upper bound, and (iv) the alignment assumption m^μ = μ b^μ. The only new free parameter introduced to set the result is the dynamo saturation σB; the thermal index Γth=1.8 is a secondary choice. No invented entities are introduced.

free parameters (2)
  • Dynamo saturation magnetization σB = b^2/ρ = 0.003 and 0.02 (dimensionless)
    The mean-field dynamo is run until the magnetization reaches this target; the >10% anisotropy result is obtained for σB=0.02 (Sec. 4, Fig. 2).
  • Thermal index Γth = 1.8
    Used to add a non-magnetized thermal pressure to the cold EoS (Eq. B55); this choice is not derived and affects the dynamics.
assumptions (5)
  • domain assumption The local magnetic field in the EoS can be treated as pointing along a local z-axis for the Landau quantization and AMM computations.
    Appendix A uses B along z locally; this is standard for magnetized EoS but neglects field geometry effects within a fluid element.
  • ad hoc to paper The mean-field dynamo term e^μ = κ b^μ faithfully mimics the turbulent dynamo amplification in the remnant.
    Section 3 Eq. (4); the dynamo coefficient and saturation are imposed, not derived from the MHD equations.
  • ad hoc to paper The polarization vector aligns instantaneously with the comoving magnetic field, m^μ = μ b^μ.
    Section 3 Eq. (10); assumes no relaxation dynamics.
  • domain assumption Zero-temperature EoS with a Gamma-law thermal cap is sufficient for a first assessment; temperature reduces anisotropy.
    Section 5.1 and Section 6 state finite-T corrections are neglected and results are upper bounds.
  • domain assumption The EoS models NL3ωρ and CMF, with their fitted couplings, are valid representations of neutron star matter up to merger densities.
    Section 2 and Appendix A; these are prior models fitted to nuclear data, not derived in this paper.

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Pith. "Pith review of Impact of magnetic field-driven anisotropies on the equation of state probed in neutron star mergers." pith.science (2026). https://pith.science/paper/BGQ477C6

@misc{pith2026250621696,
  author       = {Pith},
  title        = {Pith review of: Impact of magnetic field-driven anisotropies on the equation of state probed in neutron star mergers},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/BGQ477C6}},
  note         = {Machine review of arXiv:2506.21696}
}
abstract

Binary neutron star mergers can produce extreme magnetic fields, some of which can lead to strong magnetar-like remnants. While strong magnetic fields have been shown to affect the dynamics of outflows and angular momentum transport in the remnant, they can also crucially alter the properties of nuclear matter probed in the merger. In this work, we provide a first assessment of the latter, determining the strength of the pressure anisotropy caused by Landau level quantization and the anomalous magnetic moment. To this end, we perform the first numerical relativity simulation with a magnetic polarization tensor and a magnetic-field-dependent equation of state using a new algorithm we present here, which also incorporates a mean-field dynamo model to control the magnetic field strength present in the merger remnant. Our results show that -- in the most optimistic case -- corrections to the anisotropy can be in excess of $10\%$, and are potentially largest in the outer layers of the remnant. This work paves the way for a systematic investigation of these effects.

Figures

Figures reproduced from arXiv: 2506.21696 by the authors.

Figure 1
Figure 1. Normalized pressure anisotropy, (P∥ − P⊥)/P∥, due to the magnetic field as a function of magnetic-field strength, B, and baryon number density, nB, for the CMF model (top panel) and the NL3ωρ model (bottom panel). The parallel pressure component, P∥, is the thermodynamic pressure, P⊥ is the perpendicular pressure. importantly, we also provide a simple way for includ￾ing magnetic polarization into the equations we so… view at source ↗
Figure 2
Figure 2. Evolution of the magnetic field strength, B, during and after merger. Shown are mass-weighted averages (solid lines) and maximum values (dashed lines) for both equations of state, CMF and NL3ωρ, where ‘B’ indicates feedback of the magnetic field onto the equation of state. σB indicates the magnetization for saturation of the mean-field dynamo. Times, t, are stated relative to the time of merger, tmer. where ρ = mBnB… view at source ↗
Figure 3
Figure 3. Hypermassive neutron star using the CMF and NL3ωρ equations of state about 12 ms after merger. Shown is the absolute magnetic field strength, B, (top panels) and the ratio of poloidal, Bpoloidal, and toroidal, Btoroidal, magnetic field (bottom panels). Green contour lines indicate level surfaces of the baryon rest-mass density ρB in g/cm3 . described in Sec. 2. In order to compare the effect of magnetic field depend… view at source ↗
Figures from the paper (2 more)
Figure 4
Figure 4. Figure 4: Normalized pressure anisotropy, (P∥ − P⊥)/P∥, (top panels) and magnetic susceptibility, µ = (P∥ − P⊥)/b2 , (bottom panels) shown at 8 ms after merger for the CMF and NL3ωρ equation of state. b 2 denotes the local magnetic field energy in the comoving frame. We show res…
Figure 5
Figure 5. Figure 5: Magnetic pressure anisotropy inside the magnetar remnant. Shown are mass-weighted averages (solid lines) and maximum values (dashed lines) for both equations of state, CMF and NL3ωρ. The maximum values are always located inside the crust region, whereas the mass-weight…

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Forward citations

Cited by 2 Pith papers

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

  1. Magnetic Field Configurations in Binary Neutron Star Mergers II: Inspiral, Merger and Ejecta

    astro-ph.HE 2025-08 conditional novelty 6.0 of 10

    Initial magnetic field topology, especially anti-aligned poloidal fields, strongly controls post-merger field amplification and ejecta magnetisation in neutron star merger simulations.

  2. The equation of state for neutron stars

    nucl-th 2026-07 unverdicted

    A textbook-style review of the neutron-star equation of state covering the models, experimental and observational constraints, and open questions, with no new result claimed or derived.

Reference graph

Works this paper leans on

180 extracted references · 60 canonical work pages · cited by 2 Pith papers

  1. [1]

    , " * write output.state after.block = add.period write newline

    ENTRY address archivePrefix author booktitle chapter doi edition editor eprint howpublished institution journal key month number organization pages publisher school series title misctitle type volume year version url label extra.label sort.label short.list INTEGERS output.state before.all mid.sentence after.sentence after.block FUNCTION init.state.consts ...

  2. [2]

    write newline

    " write newline "" before.all 'output.state := FUNCTION format.url url empty "" new.block "" url * "" * if FUNCTION format.eprint eprint empty "" archivePrefix empty "" archivePrefix "arXiv" = new.block " " eprint * " " * new.block " " eprint * " " * if if if FUNCTION format.doi doi empty "" " " doi * " " * if FUNCTION format.pid doi empty eprint empty ur...

  3. [3]

    5j- VHi QᇕK ok, 1oʯA #XJ oM \ͳ z+ K 9zgF 5Qv]a =ԃΕAnVFGQ 4 = Mc 6XPg\8hE&Ke *> eת l <-q BWM! N >ˤ

    thebibliography [1] 20pt to REFERENCES 6pt =0pt \@twocolumntrue 12pt -12pt 10pt plus 3pt =0pt =0pt =1pt plus 1pt =0pt =0pt -12pt =13pt plus 1pt =20pt =13pt plus 1pt \@M =10000 =-1.0em =0pt =0pt 0pt =0pt =1.0em @enumiv\@empty 10000 10000 `\.\@m \@noitemerr \@latex@warning Empty `thebibliography' environment \@ifnextchar \@reference \@latexerr Missing key o...

    2017

  4. [4]

    P., et al

    Abbott, B. P., et al. 2017, title GW170817: Observation of Gravitational Waves from a Binary Neutron Star Inspiral , Phys. Rev. Lett., 119, 161101, 10.1103/PhysRevLett.119.161101

    doi:10.1103/physrevlett.119.161101 2017

  5. [5]

    P., et al

    Abbott, B. P., et al. 2018, title GW170817: Measurements of neutron star radii and equation of state , Phys. Rev. Lett., 121, 161101, 10.1103/PhysRevLett.121.161101

    doi:10.1103/physrevlett.121.161101 2018

  6. [6]

    P., et al

    Abbott, B. P., et al. 2020, title GW190425: Observation of a Compact Binary Coalescence with Total Mass 3.4 M_ , Astrophys. J. Lett., 892, L3, 10.3847/2041-8213/ab75f5

    doi:10.3847/2041-8213/ab75f5 2020

  7. [7]

    2023, title Role of turbulence and winding in the development of large-scale, strong magnetic fields in long-lived remnants of binary neutron star mergers , Phys

    Aguilera-Miret, R., Palenzuela, C., Carrasco, F., & Vigan\`o, D. 2023, title Role of turbulence and winding in the development of large-scale, strong magnetic fields in long-lived remnants of binary neutron star mergers , Phys. Rev. D, 108, 103001, 10.1103/PhysRevD.108.103001

    doi:10.1103/physrevd.108.103001 2023

  8. [8]

    2022, title Universality of the Turbulent Magnetic Field in Hypermassive Neutron Stars Produced by Binary Mergers , Astrophys

    Aguilera-Miret, R., Vigan\`o, D., & Palenzuela, C. 2022, title Universality of the Turbulent Magnetic Field in Hypermassive Neutron Stars Produced by Binary Mergers , Astrophys. J. Lett., 926, L31, 10.3847/2041-8213/ac50a7

    doi:10.3847/2041-8213/ac50a7 2022

Show all 180 references
  1. [9]

    2015, title Coexistence of phases in asymmetric nuclear matter under strong magnetic fields , J

    Aguirre, R., & Bauer, E. 2015, title Coexistence of phases in asymmetric nuclear matter under strong magnetic fields , J. Phys. G, 42, 105101, 10.1088/0954-3899/42/10/105101

    2015 doi

  2. [10]

    2014, title Neutron matter under strong magnetic fields: a comparison of models , Phys

    Aguirre, R., Bauer, E., & Vida\ na, I. 2014, title Neutron matter under strong magnetic fields: a comparison of models , Phys. Rev. C, 89, 035809, 10.1103/PhysRevC.89.035809

    2014 doi

  3. [11]

    2003, title Gauge conditions for long term numerical black hole evolutions without excision , Phys

    Alcubierre, M., Bruegmann, B., Diener, P., et al. 2003, title Gauge conditions for long term numerical black hole evolutions without excision , Phys. Rev. D, 67, 084023, 10.1103/PhysRevD.67.084023

    2003 doi

  4. [12]

    G., Bovard, L., Hanauske, M., Rezzolla, L., & Schwenzer, K

    Alford, M. G., Bovard, L., Hanauske, M., Rezzolla, L., & Schwenzer, K. 2018, title Viscous Dissipation and Heat Conduction in Binary Neutron-Star Mergers , Phys. Rev. Lett., 120, 041101, 10.1103/PhysRevLett.120.041101

    2018 doi

  5. [13]

    C., et al

    Andersen, B. C., et al. 2020, title A bright millisecond-duration radio burst from a Galactic magnetar , Nature, 587, 54, 10.1038/s41586-020-2863-y

    2020 doi

  6. [14]

    W., Lehner, L., et al

    Anderson, M., Hirschmann, E. W., Lehner, L., et al. 2008, title Magnetized Neutron Star Mergers and Gravitational Wave Signals , Phys. Rev. Lett., 100, 191101, 10.1103/PhysRevLett.100.191101

    2008 doi

  7. [15]

    2018, title Gravitational-wave constraints on the neutron-star-matter Equation of State , Phys

    Annala, E., Gorda, T., Kurkela, A., & Vuorinen, A. 2018, title Gravitational-wave constraints on the neutron-star-matter Equation of State , Phys. Rev. Lett., 120, 172703, 10.1103/PhysRevLett.120.172703

    2018 doi

  8. [16]

    P., Rabhi, A., et al

    Avancini, S., Bertolino, B. P., Rabhi, A., et al. 2018, title Stability of the neutron-proton-electron matter under strong magnetic fields: The covariant Vlasov approach , Phys. Rev. C, 98, 025805, 10.1103/PhysRevC.98.025805

    2018 doi

  9. [17]

    S., Barros, C

    Avancini, S. S., Barros, C. C., Brito, L., et al. 2012, title Light clusters in nuclear matter and the ``pasta'' phase, Phys. Rev. C, 85, 035806, 10.1103/PhysRevC.85.035806

    2012 doi

  10. [18]

    Backes, B. C. T., Marquezb, K. D., & Menezes, D. P. 2021, title Effects of strong magnetic fields on the hadron-quark deconfinement transition , Eur. Phys. J. A, 57, 229, 10.1140/epja/s10050-021-00544-2

    2021 doi

  11. [19]

    2008, title Accurate evolutions of inspiralling neutron-star binaries: prompt and delayed collapse to black hole , Phys

    Baiotti, L., Giacomazzo, B., & Rezzolla, L. 2008, title Accurate evolutions of inspiralling neutron-star binaries: prompt and delayed collapse to black hole , Phys. Rev. D, 78, 084033, 10.1103/PhysRevD.78.084033

    2008 doi

  12. [20]

    Bamber, J., Tsokaros, A., Ruiz, M., & Shapiro, S. L. 2024, title Jetlike structures in low-mass binary neutron star merger remnants , Phys. Rev. D, 110, 024046, 10.1103/PhysRevD.110.024046

    2024 doi

  13. [21]

    Bamber, J., Tsokaros, A., Ruiz, M., & Shapiro, S. L. 2025, title Postmerger multimessenger analysis of binary neutron stars: Effect of the magnetic field strength and topology , Phys. Rev. D, 111, 044038, 10.1103/PhysRevD.111.044038

    2025 doi

  14. [22]

    S., Hu, J

    Bao, S. S., Hu, J. N., Zhang, Z. W., & Shen, H. 2014, title Effects of the symmetry energy on properties of neutron star crusts near the neutron drip density , Phys. Rev. C, 90, 045802, 10.1103/PhysRevC.90.045802

    2014 doi

  15. [23]

    Barr\`ere, P., Guilet, J., Reboul-Salze, A., Raynaud, R., & Janka, H. T. 2022, title A new scenario for magnetar formation: Tayler-Spruit dynamo in a proto-neutron star spun up by fallback , Astron. Astrophys., 668, A79, 10.1051/0004-6361/202244172

    2022 doi

  16. [24]

    W., & Shapiro, S

    Baumgarte, T. W., & Shapiro, S. L. 2003, title General - relativistic MHD for the numerical construction of dynamical space - times , Astrophys. J., 585, 921, 10.1086/346103

    2003 doi

  17. [25]

    T., & Oechslin, R

    Bauswein, A., Janka, H. T., & Oechslin, R. 2010, title Testing Approximations of Thermal Effects in Neutron Star Merger Simulations , Phys. Rev. D, 82, 084043, 10.1103/PhysRevD.82.084043

    2010 doi

  18. [26]

    2017, title Neutron-star radius constraints from GW170817 and future detections , Astrophys

    Bauswein, A., Just, O., Janka, H.-T., & Stergioulas, N. 2017, title Neutron-star radius constraints from GW170817 and future detections , Astrophys. J. Lett., 850, L34, 10.3847/2041-8213/aa9994

    2017 doi

  19. [27]

    A., & Pethick, C

    Baym, G., Bethe, H. A., & Pethick, C. 1971, title Neutron star matter , Nucl. Phys. A, 175, 225, 10.1016/0375-9474(71)90281-8

    1971 doi

  20. [28]

    L., & Fortin, M

    Bejger, M., Blaschke, D., Haensel, P., Zdunik, J. L., & Fortin, M. 2017, title Consequences of a strong phase transition in the dense matter equation of state for the rotational evolution of neutron stars , Astron. Astrophys., 600, A39, 10.1051/0004-6361/201629580

    2017 doi

  21. [29]

    G., Bauer, E., & Vida\ na, I

    Benvenuto, O. G., Bauer, E., & Vida\ na, I. 2023, title Hot and highly magnetized neutron star matter properties with Skyrme interactions , Eur. Phys. J. A, 59, 159, 10.1140/epja/s10050-023-01070-z

    2023 doi

  22. [30]

    2010, title Constraint violation in free evolution schemes: Comparing BSSNOK with a conformal decomposition of Z4 , Phys

    Bernuzzi, S., & Hilditch, D. 2010, title Constraint violation in free evolution schemes: Comparing BSSNOK with a conformal decomposition of Z4 , Phys. Rev. D, 81, 084003, 10.1103/PhysRevD.81.084003

    2010 doi

  23. [31]

    D., Ravi, V., Belov, K

    Bochenek, C. D., Ravi, V., Belov, K. V., et al. 2020, title A fast radio burst associated with a Galactic magnetar , Nature, 587, 59, 10.1038/s41586-020-2872-x

    2020 doi

  24. [32]

    P., & Keiser , S

    Boss , A. P., & Keiser , S. A. 2013, title Collapse and Fragmentation of Magnetic Molecular Cloud Cores with the Enzo AMR MHD Code. I. Uniform Density Spheres , , 764, 136, 10.1088/0004-637X/764/2/136

    2013 doi

  25. [33]

    2021, title kuibit: Analyzing Einstein Toolkit simulations with Python , The Journal of Open Source Software, 6, 3099, 10.21105/joss.03099

    Bozzola , G. 2021, title kuibit: Analyzing Einstein Toolkit simulations with Python , The Journal of Open Source Software, 6, 3099, 10.21105/joss.03099

    2021 doi

  26. [34]

    M., & Levin, Y

    Bransgrove, A., Beloborodov, A. M., & Levin, Y. 2020, title A Quake Quenching the Vela Pulsar , 10.3847/1538-4357/ab93b7

    2020 doi

  27. [35]

    2018, title Magnetic field evolution of neutron stars I

    Bransgrove, A., Levin, Y., & Beloborodov, A. 2018, title Magnetic field evolution of neutron stars I. Basic formalism, numerical techniques and first results , Mon. Not. Roy. Astron. Soc., 473, 2771, 10.1093/mnras/stx2508

    2018 doi

  28. [36]

    2013, title A fully covariant mean-field dynamo closure for numerical 3+1 resistive GRMHD , Mon

    Bucciantini, N., & Del Zanna, L. 2013, title A fully covariant mean-field dynamo closure for numerical 3+1 resistive GRMHD , Mon. Not. Roy. Astron. Soc., 428, 71, 10.1093/mnras/sts005

    2013 doi

  29. [37]

    D., Most, E

    Chabanov, M., Tootle, S. D., Most, E. R., & Rezzolla, L. 2023, title Crustal Magnetic Fields Do Not Lead to Large Magnetic-field Amplifications in Binary Neutron Star Mergers , Astrophys. J. Lett., 945, L14, 10.3847/2041-8213/acbbc5

    2023 doi

  30. [38]

    K., Mihailov, L

    Chamel, N., Stoyanov, Z. K., Mihailov, L. M., et al. 2015, title Role of Landau quantization on the neutron-drip transition in magnetar crusts , Phys. Rev. C, 91, 065801, 10.1103/PhysRevC.91.065801

    2015 doi

  31. [39]

    F., Foucart, F., & Quataert, E

    Chandra, M., Gammie, C. F., Foucart, F., & Quataert, E. 2015, title An Extended Magnetohydrodynamics Model for Relativistic Weakly Collisional Plasmas , Astrophys. J., 810, 162, 10.1088/0004-637X/810/2/162

    2015 doi

  32. [40]

    2015, title Consistent neutron star models with magnetic field dependent equations of state , Mon

    Chatterjee, D., Elghozi, T., Novak, J., & Oertel, M. 2015, title Consistent neutron star models with magnetic field dependent equations of state , Mon. Not. Roy. Astron. Soc., 447, 3785, 10.1093/mnras/stu2706

    2015 doi

  33. [41]

    Chatterjee, D., Gulminelli, F., & Menezes, D. P. 2019, title Estimating magnetar radii with an empirical meta-model , JCAP, 03, 035, 10.1088/1475-7516/2019/03/035

    2019 doi

  34. [42]

    2018, title Measuring the neutron star tidal deformability with equation-of-state-independent relations and gravitational waves , Phys

    Chatziioannou, K., Haster, C.-J., & Zimmerman, A. 2018, title Measuring the neutron star tidal deformability with equation-of-state-independent relations and gravitational waves , Phys. Rev. D, 97, 104036, 10.1103/PhysRevD.97.104036

    2018 doi

  35. [43]

    2015, title Quark magnetar in the three-flavor Nambu Jona-Lasinio model with vector interactions and a magnetized gluon potential , Phys

    Chu, P.-C., Wang, X., Chen, L.-W., & Huang, M. 2015, title Quark magnetar in the three-flavor Nambu Jona-Lasinio model with vector interactions and a magnetized gluon potential , Phys. Rev. D, 91, 023003, 10.1103/PhysRevD.91.023003

    2015 doi

  36. [44]

    2017, title General relativistic magnetohydrodynamic simulations of binary neutron star mergers forming a long-lived neutron star , Phys

    Ciolfi, R., Kastaun, W., Giacomazzo, B., et al. 2017, title General relativistic magnetohydrodynamic simulations of binary neutron star mergers forming a long-lived neutron star , Phys. Rev. D, 95, 063016, 10.1103/PhysRevD.95.063016

    2017 doi

  37. [45]

    Combi, L., & Siegel, D. M. 2023 a , title GRMHD Simulations of Neutron-star Mergers with Weak Interactions: r-process Nucleosynthesis and Electromagnetic Signatures of Dynamical Ejecta , Astrophys. J., 944, 28, 10.3847/1538-4357/acac29

    2023 doi

  38. [46]

    Combi, L., & Siegel, D. M. 2023 b , title Jets from Neutron-Star Merger Remnants and Massive Blue Kilonovae , Phys. Rev. Lett., 131, 231402, 10.1103/PhysRevLett.131.231402

    2023 doi

  39. [47]

    2024, Phase Stability in the 3-Dimensional Open-source Code for the Chiral mean-field Model , 2409.06837

    Cruz-Camacho, N., Kumar, R., Reinke Pelicer, M., et al. 2024, Phase Stability in the 3-Dimensional Open-source Code for the Chiral mean-field Model , 2409.06837

    2024 arXiv

  40. [48]

    2024, title Magnetized Outflows from Short-lived Neutron Star Merger Remnants Can Produce a Blue Kilonova , Astrophys

    Curtis, S., Bosch, P., M\"osta, P., et al. 2024, title Magnetized Outflows from Short-lived Neutron Star Merger Remnants Can Produce a Blue Kilonova , Astrophys. J. Lett., 961, L26, 10.3847/2041-8213/ad0fe1

    2024 doi

  41. [49]

    J., & Van Alphen, P

    De Haas, W. J., & Van Alphen, P. M. 1930, title The Dependence of the Susceptibility of Diamagnetic Metals upon the Field - Communication No. 212a from the Physical Labroratory, Leiden, Proc. Acad. Sci. Amst., 33, 1106. https://www.dwc.knaw.nl/DL/publications/PU00015989.pdf

    1930

  42. [50]

    2007, title ECHO: an Eulerian Conservative High Order scheme for general relativistic magnetohydrodynamics and magnetodynamics , Astron

    Del Zanna, L., Zanotti, O., Bucciantini, N., & Londrillo, P. 2007, title ECHO: an Eulerian Conservative High Order scheme for general relativistic magnetohydrodynamics and magnetodynamics , Astron. Astrophys., 473, 11, 10.1051/0004-6361:20077093

    2007 doi

  43. [51]

    2019, title What do we learn about vector interactions from GW170817? , J

    Dexheimer, V., de Oliveira Gomes, R., Schramm, S., & Pais, H. 2019, title What do we learn about vector interactions from GW170817? , J. Phys. G, 46, 034002, 10.1088/1361-6471/ab01f0

    2019 doi

  44. [52]

    O., et al

    Dexheimer, V., Franzon, B., Gomes, R. O., et al. 2017, title What is the magnetic field distribution for the equation of state of magnetized neutron stars? , Phys. Lett. B, 773, 487, 10.1016/j.physletb.2017.09.008

    2017 doi

  45. [53]

    2012, title Hybrid Stars in a Strong Magnetic Field , Eur

    Dexheimer, V., Negreiros, R., & Schramm, S. 2012, title Hybrid Stars in a Strong Magnetic Field , Eur. Phys. J. A, 48, 189, 10.1140/epja/i2012-12189-y

    2012 doi

  46. [54]

    2008, title Proto-Neutron and Neutron Stars in a Chiral SU(3) Model , Astrophys

    Dexheimer, V., & Schramm, S. 2008, title Proto-Neutron and Neutron Stars in a Chiral SU(3) Model , Astrophys. J., 683, 943, 10.1086/589735

    2008 doi

  47. [55]

    A., & Schramm, S

    Dexheimer, V. A., & Schramm, S. 2010, title A Novel Approach to Model Hybrid Stars , Phys. Rev. C, 81, 045201, 10.1103/PhysRevC.81.045201

    2010 doi

  48. [56]

    2001, title A unified equation of state of dense matter and neutron star structure , Astron

    Douchin, F., & Haensel, P. 2001, title A unified equation of state of dense matter and neutron star structure , Astron. Astrophys., 380, 151, 10.1051/0004-6361:20011402

    2001 doi

  49. [57]

    D., Liu, Y

    Duez, M. D., Liu, Y. T., Shapiro, S. L., & Stephens, B. C. 2005, title Relativistic magnetohydrodynamics in dynamical spacetimes: Numerical methods and tests , Phys. Rev. D, 72, 024028, 10.1103/PhysRevD.72.024028

    2005 doi

  50. [58]

    2016, title General Relativistic Magnetohydrodynamic Simulations of Binary Neutron Star Mergers with the APR4 Equation of State , Class

    Endrizzi, A., Ciolfi, R., Giacomazzo, B., Kastaun, W., & Kawamura, T. 2016, title General Relativistic Magnetohydrodynamic Simulations of Binary Neutron Star Mergers with the APR4 Equation of State , Class. Quant. Grav., 33, 164001, 10.1088/0264-9381/33/16/164001

    2016 doi

  51. [59]

    L., Hammond, P., Radice, D., et al

    Espino, P. L., Hammond, P., Radice, D., et al. 2024, title Neutrino Trapping and Out-of-Equilibrium Effects in Binary Neutron-Star Merger Remnants , Phys. Rev. Lett., 132, 211001, 10.1103/PhysRevLett.132.211001

    2024 doi

  52. [60]

    B., Paschalidis, V., Haas, R., M\"osta, P., & Shapiro, S

    Etienne, Z. B., Paschalidis, V., Haas, R., M\"osta, P., & Shapiro, S. L. 2015, title IllinoisGRMHD: An Open-Source, User-Friendly GRMHD Code for Dynamical Spacetimes , Class. Quant. Grav., 32, 175009, 10.1088/0264-9381/32/17/175009

    2015 doi

  53. [61]

    2016, title Larger and more heterogeneous neutron star crusts: A result of strong magnetic fields , Phys

    Fang, J., Avancini, S., Pais, H., & Provid\^encia, C. 2016, title Larger and more heterogeneous neutron star crusts: A result of strong magnetic fields , Phys. Rev. C, 94, 062801, 10.1103/PhysRevC.94.062801

    2016 doi

  54. [62]

    2017 a , title Effect of strong magnetic fields on the crust-core transition and inner crust of neutron stars , Phys

    Fang, J., Pais, H., Pratapsi, S., et al. 2017 a , title Effect of strong magnetic fields on the crust-core transition and inner crust of neutron stars , Phys. Rev. C, 95, 045802, 10.1103/PhysRevC.95.045802

    2017 doi

  55. [63]

    2017 b , title Crust-core transition of a neutron star: effects of the symmetry energy and temperature under strong magnetic fields , Phys

    Fang, J., Pais, H., Pratapsi, S., & Provid\^encia, C. 2017 b , title Crust-core transition of a neutron star: effects of the symmetry energy and temperature under strong magnetic fields , Phys. Rev. C, 95, 062801, 10.1103/PhysRevC.95.062801

    2017 doi

  56. [64]

    J., Horowitz, C

    Fattoyev, F. J., Horowitz, C. J., Piekarewicz, J., & Reed, B. 2020, title GW190814: Impact of a 2.6 solar mass neutron star on the nucleonic equations of state , Phys. Rev. C, 102, 065805, 10.1103/PhysRevC.102.065805

    2020 doi

  57. [65]

    J., de la Incera, V., Keith, J

    Ferrer, E. J., de la Incera, V., Keith, J. P., Portillo, I., & Springsteen, P. L. 2010, title Equation of State of a Dense and Magnetized Fermion System , Phys. Rev. C, 82, 065802, 10.1103/PhysRevC.82.065802

    2010 doi

  58. [66]

    J., & Hackebill, A

    Ferrer, E. J., & Hackebill, A. 2022, title Hadron-quark phase transition at finite density in the presence of a magnetic field: Anisotropic approach , Int. J. Mod. Phys. A, 37, 2250048, 10.1142/S0217751X22500488

    2022 doi

  59. [67]

    2023, title Thermal Effects in Binary Neutron Star Mergers , Astrophys

    Fields, J., Prakash, A., Breschi, M., et al. 2023, title Thermal Effects in Binary Neutron Star Mergers , Astrophys. J. Lett., 952, L36, 10.3847/2041-8213/ace5b2

    2023 doi

  60. [68]

    J., Burgio, G

    Figura, A., Lu, J. J., Burgio, G. F., Li, Z. H., & Schulze, H. J. 2020, title Hybrid equation of state approach in binary neutron-star merger simulations , Phys. Rev. D, 102, 043006, 10.1103/PhysRevD.102.043006

    2020 doi

  61. [69]

    A., Sanches, S

    Foga c a, D. A., Sanches, S. M., Motta, T. F., & Navarra, F. S. 2016, title Compact stars with strongly coupled quark matter in a strong magnetic field , Phys. Rev. C, 94, 055805, 10.1103/PhysRevC.94.055805

    2016 doi

  62. [70]

    S., & Mizher, A

    Fraga, E. S., & Mizher, A. J. 2008, title Chiral transition in a strong magnetic background , Phys. Rev. D, 78, 025016, 10.1103/PhysRevD.78.025016

    2008 doi

  63. [71]

    2016, title A self-consistent study of magnetic field effects on hybrid stars , Mon

    Franzon, B., Dexheimer, V., & Schramm, S. 2016, title A self-consistent study of magnetic field effects on hybrid stars , Mon. Not. Roy. Astron. Soc., 456, 2937, 10.1093/mnras/stv2606

    2016 doi

  64. [72]

    2024, title Relativistic bulk rheology: From neutron star mergers to viscous cosmology , Phys

    Gavassino, L., & Noronha, J. 2024, title Relativistic bulk rheology: From neutron star mergers to viscous cosmology , Phys. Rev. D, 109, 096040, 10.1103/PhysRevD.109.096040

    2024 doi

  65. [73]

    2013, title Formation of Stable Magnetars from Binary Neutron Star Mergers , Astrophys

    Giacomazzo, B., & Perna, R. 2013, title Formation of Stable Magnetars from Binary Neutron Star Mergers , Astrophys. J. Lett., 771, L26, 10.1088/2041-8205/771/2/L26

    2013 doi

  66. [74]

    2011, title Accurate evolutions of inspiralling and magnetized neutron-stars: Equal-mass binaries , Phys

    Giacomazzo, B., Rezzolla, L., & Baiotti, L. 2011, title Accurate evolutions of inspiralling and magnetized neutron-stars: Equal-mass binaries , Phys. Rev. D, 83, 044014, 10.1103/PhysRevD.83.044014

    2011 doi

  67. [75]

    I., & Perna, R

    Giacomazzo, B., Zrake, J., Duffell, P., MacFadyen, A. I., & Perna, R. 2015, title Producing Magnetar Magnetic Fields in the Merger of Binary Neutron Stars , Astrophys. J., 809, 39, 10.1088/0004-637X/809/1/39

    2015 doi

  68. [76]

    O., Pais, H., Dexheimer, V., Provid\^encia, C., & Schramm, S

    Gomes, R. O., Pais, H., Dexheimer, V., Provid\^encia, C., & Schramm, S. 2019, title Limiting magnetic field for minimal deformation of a magnetized neutron star , Astron. Astrophys., 627, A61, 10.1051/0004-6361/201935310

    2019 doi

  69. [77]

    V., Miransky, V

    Gorbar, E. V., Miransky, V. A., & Shovkovy, I. A. 2011, title Normal ground state of dense relativistic matter in a magnetic field , Phys. Rev. D, 83, 085003, 10.1103/PhysRevD.83.085003

    2011 doi

  70. [78]

    2007, 3+1 formalism and bases of numerical relativity , gr-qc/0703035

    Gourgoulhon, E. 2007, 3+1 formalism and bases of numerical relativity , gr-qc/0703035

    2007 arXiv

  71. [79]

    2010, title Kadath: A Spectral solver for theoretical physics , J

    Grandclement, P. 2010, title Kadath: A Spectral solver for theoretical physics , J. Comput. Phys., 229, 3334, 10.1016/j.jcp.2010.01.005

    2010 doi

  72. [80]

    M., Cook, W., Radice, D., et al

    Guti \'e rrez, E. M., Cook, W., Radice, D., et al. 2025, title Magnetic Field Configurations in Binary Neutron Star Mergers I: Post-merger Remnant and Disk , 2506.18995

    2025

  73. [81]

    2016, title Baryon onset in a magnetic field , AIP Conf

    Haber, A., Preis, F., & Schmitt, A. 2016, title Baryon onset in a magnetic field , AIP Conf. Proc., 1701, 080010, 10.1063/1.4938699

    2016 doi

  74. [82]

    2017, title Rotational properties of hypermassive neutron stars from binary mergers , Phys

    Hanauske, M., Takami, K., Bovard, L., et al. 2017, title Rotational properties of hypermassive neutron stars from binary mergers , Phys. Rev. D, 96, 043004, 10.1103/PhysRevD.96.043004

    2017 doi

  75. [83]

    R., Millman, K

    Harris, C. R., Millman, K. J., van der Walt, S. J., et al. 2020, title Array programming with NumPy , Nature, 585, 357, 10.1038/s41586-020-2649-2

    2020 doi

  76. [84]

    2018, title Electrical Resistivity and Hall Effect in Binary Neutron-Star Mergers , Eur

    Harutyunyan, A., Nathanail, A., Rezzolla, L., & Sedrakian, A. 2018, title Electrical Resistivity and Hall Effect in Binary Neutron-Star Mergers , Eur. Phys. J. A, 54, 191, 10.1140/epja/i2018-12624-1

    2018 doi

  77. [85]

    2013, title Compact binary evolutions with the Z4c formulation , Phys

    Hilditch, D., Bernuzzi, S., Thierfelder, M., et al. 2013, title Compact binary evolutions with the Z4c formulation , Phys. Rev. D, 88, 084057, 10.1103/PhysRevD.88.084057

    2013 doi

  78. [86]

    J., & Piekarewicz, J

    Horowitz, C. J., & Piekarewicz, J. 2001 a , title Neutron star structure and the neutron radius of Pb-208 , Phys. Rev. Lett., 86, 5647, 10.1103/PhysRevLett.86.5647

    2001 doi

  79. [87]

    J., & Piekarewicz, J

    Horowitz, C. J., & Piekarewicz, J. 2001 b , title The Neutron radii of Pb-208 and neutron stars , Phys. Rev. C, 64, 062802, 10.1103/PhysRevC.64.062802

    2001 doi

  80. [88]

    Hunter, J. D. 2007, title Matplotlib: A 2D graphics environment, Computing in Science & Engineering, 9, 90, 10.1109/MCSE.2007.55

    2007 doi

  81. [89]

    2025, From proto-neutron star dynamo to low-field magnetars , 2501.04768

    Igoshev, A., Barr\`ere, P., Raynaud, R., et al. 2025, From proto-neutron star dynamo to low-field magnetars , 2501.04768

    2025 arXiv

  82. [90]

    Isayev, A. A. 2014, title Absolute stability window and upper bound on the magnetic field strength in a strongly magnetized strange quark star , Int. J. Mod. Phys. A, 29, 1450173, 10.1142/S0217751X14501735

    2014 doi

  83. [91]

    H.-Y., Chabanov, M., & Rezzolla, L

    Jiang, J.-L., Ng, H. H.-Y., Chabanov, M., & Rezzolla, L. 2025, title Long-term impact of the magnetic-field strength on the evolution and electromagnetic emission by neutron-star merger remnants , 2502.14962

    2025 arXiv

  84. [92]

    M., & Beloborodov, A

    Kaspi, V. M., & Beloborodov, A. 2017, title Magnetars , Ann. Rev. Astron. Astrophys., 55, 261, 10.1146/annurev-astro-081915-023329

    2017 doi

  85. [93]

    V., & Ciolfi, R

    Kastaun, W., Kalinani, J. V., & Ciolfi, R. 2021, title Robust Recovery of Primitive Variables in Relativistic Ideal Magnetohydrodynamics , Phys. Rev. D, 103, 023018, 10.1103/PhysRevD.103.023018

    2021 doi

  86. [94]

    2025, title Effect of quark anomalous magnetic moment on neutral dense quark matter under magnetic field , Eur

    Kawaguchi, M., Siddique, I., & Huang, M. 2025, title Effect of quark anomalous magnetic moment on neutral dense quark matter under magnetic field , Eur. Phys. J. C, 85, 246, 10.1140/epjc/s10052-025-13952-1

    2025 doi

  87. [95]

    2016, title Binary Neutron Star Mergers and Short Gamma-Ray Bursts: Effects of Magnetic Field Orientation, Equation of State, and Mass Ratio , Phys

    Kawamura, T., Giacomazzo, B., Kastaun, W., et al. 2016, title Binary Neutron Star Mergers and Short Gamma-Ray Bursts: Effects of Magnetic Field Orientation, Equation of State, and Mass Ratio , Phys. Rev. D, 94, 064012, 10.1103/PhysRevD.94.064012

    2016 doi

  88. [96]

    2025, General Relativistic Magnetohydrodynamics Simulations for Binary Neutron Star Mergers, ed

    Kiuchi, K. 2025, General Relativistic Magnetohydrodynamics Simulations for Binary Neutron Star Mergers, ed. C. Bambi, Y. Mizuno, S. Shashank, & F. Yuan (Singapore: Springer Nature Singapore), 529--572, 10.1007/978-981-97-8522-3_16

    2025 doi

  89. [97]

    2015, title Efficient magnetic-field amplification due to the Kelvin-Helmholtz instability in binary neutron star mergers , Phys

    Kiuchi, K., Cerd\'a-Dur\'an, P., Kyutoku, K., Sekiguchi, Y., & Shibata, M. 2015, title Efficient magnetic-field amplification due to the Kelvin-Helmholtz instability in binary neutron star mergers , Phys. Rev. D, 92, 124034, 10.1103/PhysRevD.92.124034

    2015 doi

  90. [98]

    2018, title Global simulations of strongly magnetized remnant massive neutron stars formed in binary neutron star mergers , Phys

    Kiuchi, K., Kyutoku, K., Sekiguchi, Y., & Shibata, M. 2018, title Global simulations of strongly magnetized remnant massive neutron stars formed in binary neutron star mergers , Phys. Rev. D, 97, 124039, 10.1103/PhysRevD.97.124039

    2018 doi

  91. [99]

    2014, title High resolution numerical-relativity simulations for the merger of binary magnetized neutron stars , Phys

    Kiuchi, K., Kyutoku, K., Sekiguchi, Y., Shibata, M., & Wada, T. 2014, title High resolution numerical-relativity simulations for the merger of binary magnetized neutron stars , Phys. Rev. D, 90, 041502, 10.1103/PhysRevD.90.041502

    2014 doi

  92. [100]

    2024, title A large-scale magnetic field produced by a solar-like dynamo in binary neutron star mergers , Nature Astron., 8, 298, 10.1038/s41550-024-02194-y

    Kiuchi, K., Reboul-Salze, A., Shibata, M., & Sekiguchi, Y. 2024, title A large-scale magnetic field produced by a solar-like dynamo in binary neutron star mergers , Nature Astron., 8, 298, 10.1038/s41550-024-02194-y

    2024 doi

  93. [101]

    A., Konig, J., & Ring, P

    Lalazissis, G. A., Konig, J., & Ring, P. 1997, title A New parametrization for the Lagrangian density of relativistic mean field theory , Phys. Rev. C, 55, 540, 10.1103/PhysRevC.55.540

    1997 doi

  94. [102]

    K., Haensel, P., Haskell, B., Zdunik, J

    Lander, S. K., Haensel, P., Haskell, B., Zdunik, J. L., & Fortin, M. 2021, title Magnetic fields in late-stage proto-neutron stars , Mon. Not. Roy. Astron. Soc., 503, 875, 10.1093/mnras/stab460

    2021 doi

  95. [103]

    M., Pethick, C

    Lattimer, J. M., Pethick, C. J., Ravenhall, D. G., & Lamb, D. Q. 1985, title PHYSICAL PROPERTIES OF HOT, DENSE MATTER: THE GENERAL CASE , Nucl. Phys. A, 432, 646, 10.1016/0375-9474(85)90006-5

    1985 doi

  96. [104]

    M., & Swesty, F

    Lattimer, J. M., & Swesty, F. D. 1991, title A Generalized equation of state for hot, dense matter , Nucl. Phys. A, 535, 331, 10.1016/0375-9474(91)90452-C

    1991 doi

  97. [105]

    M., Szyma\'nski, M., Sasaki, C., & Redlich, K

    Lo, P. M., Szyma\'nski, M., Sasaki, C., & Redlich, K. 2020, title Deconfinement in the presence of a strong magnetic field , Phys. Rev. D, 102, 034024, 10.1103/PhysRevD.102.034024

    2020 doi

  98. [106]

    2012, title The Einstein Toolkit: A Community Computational Infrastructure for Relativistic Astrophysics , Class

    Loffler, F., et al. 2012, title The Einstein Toolkit: A Community Computational Infrastructure for Relativistic Astrophysics , Class. Quant. Grav., 29, 115001, 10.1088/0264-9381/29/11/115001

    2012 doi

  99. [107]

    2022, title Landau quantization and spin polarization of cold magnetized quark matter * , Chin

    Lu, Z.-Y., Xu, J.-F., Wen, X.-J., Peng, G.-X., & Ruggieri, M. 2022, title Landau quantization and spin polarization of cold magnetized quark matter * , Chin. Phys. C, 46, 064104, 10.1088/1674-1137/ac5513

    2022 doi

  100. [108]

    Lugones, G., & Grunfeld, A. G. 2019, title Surface tension of hot and dense quark matter under strong magnetic fields , Phys. Rev. C, 99, 035804, 10.1103/PhysRevC.99.035804

    2019 doi

  101. [109]

    2003, title Stellar evolution with rotation and magnetic fields: 1

    Maeder, A., & Meynet, G. 2003, title Stellar evolution with rotation and magnetic fields: 1. The Relative importance of rotational and magnetic effects , Astron. Astrophys., 411, 543, 10.1051/0004-6361:20031491

    2003 doi

  102. [110]

    S., et al

    Makishima, K., Enoto, T., Hiraga, J. S., et al. 2014, title Possible Evidence for Free Precession of a Strongly Magnetized Neutron Star in the Magnetar 4U 0142+61 , Phys. Rev. Lett., 112, 171102, 10.1103/PhysRevLett.112.171102

    2014 doi

  103. [111]

    2021, title A NuSTAR confirmation of the 36 ks hard X-ray pulse-phase modulation in the magnetar 1E 1547.0 - 5408 , Mon

    Makishima, K., Enoto, T., Yoneda, H., & Odaka, H. 2021, title A NuSTAR confirmation of the 36 ks hard X-ray pulse-phase modulation in the magnetar 1E 1547.0 - 5408 , Mon. Not. Roy. Astron. Soc., 502, 2266, 10.1093/mnras/stab149

    2021 doi

  104. [112]

    2019, title A NuSTAR study of the 55 ks hard X-ray pulse-phase modulation in the magnetar 4U 0142+61 , Publ

    Makishima, K., Murakami, H., Enoto, T., & Nakazawa, K. 2019, title A NuSTAR study of the 55 ks hard X-ray pulse-phase modulation in the magnetar 4U 0142+61 , Publ. Astron. Soc. Jap., 71, Publications of the Astronomical Society of Japan, Volume 71, Issue 1, 1 January 2019, 15,...

    2019 doi

  105. [113]

    2024, Observational Clues to the Magnetic Evolution of Magnetars , 2407.15409

    Makishima, K., Uchida, N., & Enoto, T. 2024, Observational Clues to the Magnetic Evolution of Magnetars , 2407.15409

    2024 arXiv

  106. [114]

    S., Metzger, B

    Margalit, B., Jermyn, A. S., Metzger, B. D., Roberts, L. F., & Quataert, E. 2022, title Angular-momentum Transport in Proto-neutron Stars and the Fate of Neutron Star Merger Remnants , Astrophys. J., 939, 51, 10.3847/1538-4357/ac8b01

    2022 doi

  107. [115]

    Margalit, B., & Metzger, B. D. 2017, title Constraining the Maximum Mass of Neutron Stars From Multi-Messenger Observations of GW170817 , Astrophys. J. Lett., 850, L19, 10.3847/2041-8213/aa991c

    2017 doi

  108. [116]

    D., Thompson, T

    Metzger, B. D., Thompson, T. A., & Quataert, E. 2018, title A magnetar origin for the kilonova ejecta in GW170817 , Astrophys. J., 856, 101, 10.3847/1538-4357/aab095

    2018 doi

  109. [117]

    Miravet-Ten\'es, M., Guerra, D., Ruiz, M., Cerd\'a-Dur\'an, P., & Font, J. A. 2024, Identifying thermal effects in neutron star merger remnants with model-agnostic waveform reconstructions and third-generation detectors , 2401.02493

    2024 arXiv

  110. [118]

    K., Rawat, N

    Mishra, A., Singh, A. K., Rawat, N. S., & Aman, P. 2019, title Kaons and antikaons in strong magnetic fields , Eur. Phys. J. A, 55, 107, 10.1140/epja/i2019-12783-5

    2019 doi

  111. [119]

    2024 a , title Speed of sound in magnetized nuclear matter , Phys

    Mondal, R., Chaudhuri, N., Roy, P., & Sarkar, S. 2024 a , title Speed of sound in magnetized nuclear matter , Phys. Rev. C, 109, 054911, 10.1103/PhysRevC.109.054911

    2024 doi

  112. [120]

    2024 b , title Speed of sound and isothermal compressibility in a magnetized quark matter with anomalous magnetic moment of quarks , Phys

    Mondal, R., Duari, S., Chaudhuri, N., Sarkar, S., & Roy, P. 2024 b , title Speed of sound and isothermal compressibility in a magnetized quark matter with anomalous magnetic moment of quarks , Phys. Rev. D, 110, 054010, 10.1103/PhysRevD.110.054010

    2024 doi

  113. [121]

    Most, E. R. 2023, Impact of a mean field dynamo on neutron star mergers leading to magnetar remnants , 10.1103/PhysRevD.108.123012

    2023 doi

  114. [122]

    R., Haber, A., Harris, S

    Most, E. R., Haber, A., Harris, S. P., et al. 2024, title Emergence of Microphysical Bulk Viscosity in Binary Neutron Star Postmerger Dynamics , Astrophys. J. Lett., 967, L14, 10.3847/2041-8213/ad454f

    2024 doi

  115. [123]

    R., & Noronha, J

    Most, E. R., & Noronha, J. 2021, title Dissipative magnetohydrodynamics for nonresistive relativistic plasmas: An implicit second-order flux-conservative formulation with stiff relaxation , Phys. Rev. D, 104, 103028, 10.1103/PhysRevD.104.103028

    2021 doi

  116. [124]

    R., Papenfort, L

    Most, E. R., Papenfort, L. J., & Rezzolla, L. 2019, title Beyond second-order convergence in simulations of magnetized binary neutron stars with realistic microphysics , Mon. Not. Roy. Astron. Soc., 490, 3588, 10.1093/mnras/stz2809

    2019 doi

  117. [125]

    R., Papenfort, L

    Most, E. R., Papenfort, L. J., Weih, L. R., & Rezzolla, L. 2020, title A lower bound on the maximum mass if the secondary in GW190814 was once a rapidly spinning neutron star , Mon. Not. Roy. Astron. Soc., 499, L82, 10.1093/mnrasl/slaa168

    2020 doi

  118. [126]

    R., & Quataert, E

    Most, E. R., & Quataert, E. 2023, title Flares, Jets, and Quasiperiodic Outbursts from Neutron Star Merger Remnants , Astrophys. J. Lett., 947, L15, 10.3847/2041-8213/acca84

    2023 doi

  119. [127]

    R., & Raithel, C

    Most, E. R., & Raithel, C. A. 2021, title Impact of the nuclear symmetry energy on the post-merger phase of a binary neutron star coalescence , Phys. Rev. D, 104, 124012, 10.1103/PhysRevD.104.124012

    2021 doi

  120. [128]

    R., Weih, L

    Most, E. R., Weih, L. R., Rezzolla, L., & Schaffner-Bielich, J. 2018, title New constraints on radii and tidal deformabilities of neutron stars from GW170817 , Phys. Rev. Lett., 120, 261103, 10.1103/PhysRevLett.120.261103

    2018 doi

  121. [129]

    R., Harris, S

    Most, E. R., Harris, S. P., Plumberg, C., et al. 2021, title Projecting the likely importance of weak-interaction-driven bulk viscosity in neutron star mergers , Mon. Not. Roy. Astron. Soc., 509, 1096, 10.1093/mnras/stab2793

    2021 doi

  122. [130]

    2020, title A magnetar engine for short GRBs and kilonovae , Astrophys

    M\"osta, P., Radice, D., Haas, R., Schnetter, E., & Bernuzzi, S. 2020, title A magnetar engine for short GRBs and kilonovae , Astrophys. J. Lett., 901, L37, 10.3847/2041-8213/abb6ef

    2020 doi

  123. [131]

    Mueller, H., & Serot, B. D. 1996, title Relativistic mean field theory and the high density nuclear equation of state , Nucl. Phys. A, 606, 508, 10.1016/0375-9474(96)00187-X

    1996 doi

  124. [132]

    Musolino, C., Rezzolla, L., & Most, E. R. 2024, title On the impact of neutrinos on the launching of relativistic jets from ''magnetars'' produced in neutron-star mergers , 2410.06253

    2024 arXiv

  125. [133]

    R., & Rezzolla, L

    Nathanail, A., Most, E. R., & Rezzolla, L. 2021, title GW170817 and GW190814: tension on the maximum mass , Astrophys. J. Lett., 908, L28, 10.3847/2041-8213/abdfc6

    2021 doi

  126. [134]

    2021, title Dynamical ejecta synchrotron emission as a possible contributor to the changing behaviour of GRB170817A afterglow , Mon

    Nedora, V., Radice, D., Bernuzzi, S., et al. 2021, title Dynamical ejecta synchrotron emission as a possible contributor to the changing behaviour of GRB170817A afterglow , Mon. Not. Roy. Astron. Soc., 506, 5908, 10.1093/mnras/stab2004

    2021 doi

  127. [135]

    2022, title Transient Relativistic Fluid Dynamics in a General Hydrodynamic Frame , Phys

    Noronha, J., Spali\'nski, M., & Speranza, E. 2022, title Transient Relativistic Fluid Dynamics in a General Hydrodynamic Frame , Phys. Rev. Lett., 128, 252302, 10.1103/PhysRevLett.128.252302

    2022 doi

  128. [136]

    F., & Vucetich, H

    Orsaria, M., Ranea-Sandoval, I. F., & Vucetich, H. 2011, title Magnetars as Highly Magnetized Quark Stars: an analytical treatment , Astrophys. J., 734, 41, 10.1088/0004-637X/734/1/41

    2011 doi

  129. [137]

    2021, title Strong magnetic fields: neutron stars with an extended inner crust , Eur

    Pais, H., Bertolino, B., Fang, J., Wang, X., & Provid\^encia, C. 2021, title Strong magnetic fields: neutron stars with an extended inner crust , Eur. Phys. J. A, 57, 193, 10.1140/epja/s10050-021-00506-8

    2021 doi

  130. [138]

    2015, title Light clusters, pasta phases and phase transitions in core-collapse supernova matter , Phys

    Pais, H., Chiacchiera, S., & Provid\^encia, C. 2015, title Light clusters, pasta phases and phase transitions in core-collapse supernova matter , Phys. Rev. C, 91, 055801, 10.1103/PhysRevC.91.055801

    2015 doi

  131. [139]

    2016, title Vlasov formalism for extended relativistic mean field models: The crust-core transition and the stellar matter equation of state , Phys

    Pais, H., & Provid\^encia, C. 2016, title Vlasov formalism for extended relativistic mean field models: The crust-core transition and the stellar matter equation of state , Phys. Rev. C, 94, 015808, 10.1103/PhysRevC.94.015808

    2016 doi

  132. [140]

    2022, title Large eddy simulations of magnetized mergers of neutron stars with neutrinos , Phys

    Palenzuela, C., Liebling, S., & Mi\ nano, B. 2022, title Large eddy simulations of magnetized mergers of neutron stars with neutrinos , Phys. Rev. D, 105, 103020, 10.1103/PhysRevD.105.103020

    2022 doi

  133. [141]

    L., Neilsen, D., et al

    Palenzuela, C., Liebling, S. L., Neilsen, D., et al. 2015, title Effects of the microphysical Equation of State in the mergers of magnetized Neutron Stars With Neutrino Cooling , Phys. Rev. D, 92, 044045, 10.1103/PhysRevD.92.044045

    2015 doi

  134. [142]

    1998, title Chiral Lagrangian for strange hadronic matter , Phys

    Papazoglou, P., Schramm, S., Schaffner-Bielich, J., Stoecker, H., & Greiner, W. 1998, title Chiral Lagrangian for strange hadronic matter , Phys. Rev. C, 57, 2576, 10.1103/PhysRevC.57.2576

    1998 doi

  135. [143]

    J., Tootle, S

    Papenfort, L. J., Tootle, S. D., Grandcl\'ement, P., Most, E. R., & Rezzolla, L. 2021, title New public code for initial data of unequal-mass, spinning compact-object binaries , Phys. Rev. D, 104, 024057, 10.1103/PhysRevD.104.024057

    2021 doi

  136. [144]

    2019, title Thermodynamics conditions of matter in neutron star mergers , Eur

    Perego, A., Bernuzzi, S., & Radice, D. 2019, title Thermodynamics conditions of matter in neutron star mergers , Eur. Phys. J. A, 55, 124, 10.1140/epja/i2019-12810-7

    2019 doi

  137. [145]

    2023, title Temperature and strong magnetic field effects in dense matter , Phys

    Peterson, J., Costa, P., Kumar, R., et al. 2023, title Temperature and strong magnetic field effects in dense matter , Phys. Rev. D, 108, 063011, 10.1103/PhysRevD.108.063011

    2023 doi

  138. [146]

    M., Lora-Clavijo, F

    Pimentel, O. M., Lora-Clavijo, F. D., & Gonz\'alez, G. A. 2018, title Numerical general relativistic MHD with magnetically polarized matter , Astrophys. J., 861, 115, 10.3847/1538-4357/aac6d0

    2018 doi

  139. [147]

    A., & Vigan \`o , D

    Pons, J. A., & Vigan \`o , D. 2019, title Magnetic, thermal and rotational evolution of isolated neutron stars, Living Reviews in Computational Astrophysics, 5, 1

    2019

  140. [148]

    Y., & Chabrier, G

    Potekhin, A. Y., & Chabrier, G. 2018, title Magnetic neutron star cooling and microphysics , Astron. Astrophys., 609, A74, 10.1051/0004-6361/201731866

    2018 doi

  141. [149]

    2022, title Spin-down induced quark-hadron phase transition in cold isolated neutron stars , Mon

    Prasad, R., & Mallick, R. 2022, title Spin-down induced quark-hadron phase transition in cold isolated neutron stars , Mon. Not. Roy. Astron. Soc., 516, 1127, 10.1093/mnras/stac2324

    2022 doi

  142. [150]

    2006, Producing ultra-strong magnetic fields in neutron star mergers , 10.1126/science.1125201

    Price, D., & Rosswog, S. 2006, Producing ultra-strong magnetic fields in neutron star mergers , 10.1126/science.1125201

    2006 doi

  143. [151]

    2018, title Tidal deformability from GW170817 as a direct probe of the neutron star radius , Astrophys

    Raithel, C., \"Ozel, F., & Psaltis, D. 2018, title Tidal deformability from GW170817 as a direct probe of the neutron star radius , Astrophys. J. Lett., 857, L23, 10.3847/2041-8213/aabcbf

    2018 doi

  144. [152]

    2021, title Realistic finite-temperature effects in neutron star merger simulations , Phys

    Raithel, C., Paschalidis, V., & \"Ozel, F. 2021, title Realistic finite-temperature effects in neutron star merger simulations , Phys. Rev. D, 104, 063016, 10.1103/PhysRevD.104.063016

    2021 doi

  145. [153]

    A., & Most, E

    Raithel, C. A., & Most, E. R. 2022, title Characterizing the Breakdown of Quasi-universality in Postmerger Gravitational Waves from Binary Neutron Star Mergers , Astrophys. J. Lett., 933, L39, 10.3847/2041-8213/ac7c75

    2022 doi

  146. [154]

    A., & Paschalidis, V

    Raithel, C. A., & Paschalidis, V. 2023, title Influence of stellar compactness on finite-temperature effects in neutron star merger simulations , Phys. Rev. D, 108, 083029, 10.1103/PhysRevD.108.083029

    2023 doi

  147. [155]

    A., & Paschalidis, V

    Raithel, C. A., & Paschalidis, V. 2024, title Detectability of finite-temperature effects from neutron star mergers with next-generation gravitational wave detectors , Phys. Rev. D, 110, 043002, 10.1103/PhysRevD.110.043002

    2024 doi

  148. [156]

    2020, title Magnetar formation through a convective dynamo in protoneutron stars , Sci

    Raynaud, R., Guilet, J., Janka, H.-T., & Gastine, T. 2020, title Magnetar formation through a convective dynamo in protoneutron stars , Sci. Adv., 6, eaay2732, 10.1126/sciadv.aay2732

    2020 doi

  149. [157]

    2024, title Tayler-Spruit dynamo in binary neutron star merger remnants , 2411.19328

    Reboul-Salze, A., Barr\`ere, P., Kiuchi, K., et al. 2024, title Tayler-Spruit dynamo in binary neutron star merger remnants , 2411.19328

    2024

  150. [158]

    R., & Weih, L

    Rezzolla, L., Most, E. R., & Weih, L. R. 2018, title Using gravitational-wave observations and quasi-universal relations to constrain the maximum mass of neutron stars , Astrophys. J. Lett., 852, L25, 10.3847/2041-8213/aaa401

    2018 doi

  151. [159]

    S., & Denicol, G

    Rocha, G. S., & Denicol, G. S. 2021, title Transient fluid dynamics with general matching conditions: A first study from the method of moments , Phys. Rev. D, 104, 096016, 10.1103/PhysRevD.104.096016

    2021 doi

  152. [160]

    2010, title New Developments in Relativistic Viscous Hydrodynamics , Int

    Romatschke, P. 2010, title New Developments in Relativistic Viscous Hydrodynamics , Int. J. Mod. Phys. E, 19, 1, 10.1142/S0218301310014613

    2010 doi

  153. [161]

    L., & Tsokaros, A

    Ruiz, M., Shapiro, S. L., & Tsokaros, A. 2018, title GW170817, General Relativistic Magnetohydrodynamic Simulations, and the Neutron Star Maximum Mass , Phys. Rev. D, 97, 021501, 10.1103/PhysRevD.97.021501

    2018 doi

  154. [162]

    2024, title Assessing the joint effect of temperature and magnetic field on the neutron star equation of state , Phys

    Scurto, L., Carvalho, V., Pais, H., & Provid\^encia, C. 2024, title Assessing the joint effect of temperature and magnetic field on the neutron star equation of state , Phys. Rev. C, 110, 045805, 10.1103/PhysRevC.110.045805

    2024 doi

  155. [163]

    2023, title Strong magnetic fields and pasta phases reexamined , Phys

    Scurto, L., Pais, H., & Gulminelli, F. 2023, title Strong magnetic fields and pasta phases reexamined , Phys. Rev. C, 107, 045806, 10.1103/PhysRevC.107.045806

    2023 doi

  156. [164]

    D., & Walecka, J

    Serot, B. D., & Walecka, J. D. 1986, title The Relativistic Nuclear Many Body Problem , Adv. Nucl. Phys., 16, 1

    1986

  157. [165]

    Shapiro, S. L. 2000, title Differential rotation in neutron stars: Magnetic braking and viscous damping , Astrophys. J., 544, 397, 10.1086/317209

    2000 doi

  158. [166]

    2019, title Constraint on the maximum mass of neutron stars using GW170817 event , Phys

    Shibata, M., Zhou, E., Kiuchi, K., & Fujibayashi, S. 2019, title Constraint on the maximum mass of neutron stars using GW170817 event , Phys. Rev. D, 100, 023015, 10.1103/PhysRevD.100.023015

    2019 doi

  159. [167]

    2013, title Strange quark matter in strong magnetic fields within a confining model , Phys

    Sinha, M., Huang, X.-G., & Sedrakian, A. 2013, title Strange quark matter in strong magnetic fields within a confining model , Phys. Rev. D, 88, 025008, 10.1103/PhysRevD.88.025008

    2013 doi

  160. [168]

    Strickland, M., Dexheimer, V., & Menezes, D. P. 2012, title Bulk Properties of a Fermi Gas in a Magnetic Field , Phys. Rev. D, 86, 125032, 10.1103/PhysRevD.86.125032

    2012 doi

  161. [169]

    G., & Pons, J

    Suvorov, A. G., & Pons, J. A. 2025, title Magnetar structure in nonlinear electrodynamics with mixed poloidal-toroidal fields , 2503.01409

    2025 arXiv

  162. [170]

    2020, title Neutron Star Equation of State in light of GW190814 , Phys

    Tan, H., Noronha-Hostler, J., & Yunes, N. 2020, title Neutron Star Equation of State in light of GW190814 , Phys. Rev. Lett., 125, 261104, 10.1103/PhysRevLett.125.261104

    2020 doi

  163. [171]

    2017, title Equation of State for Nucleonic and Hyperonic Neutron Stars with Mass and Radius Constraints , Astrophys

    Tolos, L., Centelles, M., & Ramos, A. 2017, title Equation of State for Nucleonic and Hyperonic Neutron Stars with Mass and Radius Constraints , Astrophys. J., 834, 3, 10.3847/1538-4357/834/1/3

    2017 doi

  164. [172]

    Tsokaros, A., Bamber, J., Ruiz, M., & Shapiro, S. L. 2025, title Masking the Equation-of-State Effects in Binary Neutron Star Mergers , Phys. Rev. Lett., 134, 121401, 10.1103/PhysRevLett.134.121401

    2025 doi

  165. [173]

    2023, Self-consistent treatment of thermal effects in neutron-star post-mergers: observational implications for third-generation gravitational-wave detectors , 2310.20378

    Villa-Ortega, V., Lorenzo-Medina, A., Calder\'on Bustillo, J., et al. 2023, Self-consistent treatment of thermal effects in neutron-star post-mergers: observational implications for third-generation gravitational-wave detectors , 2310.20378

    2023 arXiv

  166. [174]

    E., et al

    Virtanen, P., Gommers, R., Oliphant, T. E., et al. 2020, title SciPy 1.0: Fundamental Algorithms for Scientific Computing in Python , Nature Methods, 17, 261, 10.1038/s41592-019-0686-2

    2020 doi

  167. [175]

    2022, title Pasta phases in neutron stars under strong magnetic fields , Phys

    Wang, X., Li, J., Fang, J., Pais, H., & Provid\^encia, C. 2022, title Pasta phases in neutron stars under strong magnetic fields , Phys. Rev. D, 105, 063004, 10.1103/PhysRevD.105.063004

    2022 doi

  168. [176]

    2024, title Isospin asymmetric matter in uniform and nonuniform strong magnetic fields , Phys

    Wang, Y., & Wen, X.-J. 2024, title Isospin asymmetric matter in uniform and nonuniform strong magnetic fields , Phys. Rev. C, 109, 015201, 10.1103/PhysRevC.109.015201

    2024 doi

  169. [177]

    C., Meier, D

    Wheeler, J. C., Meier, D. L., & Wilson, J. R. 2002, title Asymmetric supernovae from magneto-centrifugal jets , Astrophys. J., 568, 807, 10.1086/338953

    2002 doi

  170. [178]

    2022, Binary neutron star merger simulations with neutrino transport and turbulent viscosity: impact of different schemes and grid resolution , 10.1093/mnras/stad107

    Zappa, F., Bernuzzi, S., Radice, D., & Perego, A. 2022, Binary neutron star merger simulations with neutrino transport and turbulent viscosity: impact of different schemes and grid resolution , 10.1093/mnras/stad107

    2022 doi

  171. [179]

    G., Campanelli, M., & Lousto, C

    Zlochower, Y., Baker, J. G., Campanelli, M., & Lousto, C. O. 2005, title Accurate black hole evolutions by fourth-order numerical relativity , Phys. Rev. D, 72, 024021, 10.1103/PhysRevD.72.024021

    2005 doi

  172. [180]

    A., et al

    Zyla, P. A., et al. 2020, title Review of Particle Physics , PTEP, 2020, 083C01, 10.1093/ptep/ptaa104

    2020 doi

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