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Quantum term reshapes dark star rotation, universal relation holds

2026-07-09 23:20 UTC pith:GOWKSQNO

load-bearing objection Solid computational extension to slow rotation, but the 'clean diagnostic' claim is oversold the 2 major comments →

arxiv 2607.06898 v1 pith:GOWKSQNO submitted 2026-07-08 gr-qc

Slowly rotating condensate dark stars beyond the mean-field approximation

Grigoris Panotopoulos , \'Angel Rinc\'on , Ilidio Lopes This is my paper
classification gr-qc
keywords Bose-Einstein condensate dark starsLee-Huang-Yang correctionslow rotationmoment of inertiatidal deformabilityuniversal relationsI-Love-QHartle formalism
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

The paper asks whether the leading quantum-fluctuation correction to the mean-field description of a Bose-Einstein condensate — the Lee-Huang-Yang (LHY) term, originally derived for dilute hard-sphere Bose gases — leaves a detectable imprint on the rotational and tidal properties of compact stars made entirely of condensed dark matter. The authors integrate the full relativistic structure equations (TOV plus Hartle slow-rotation plus tidal Love-number machinery) for a polytropic n=1 equation of state with and without the LHY correction, using two concrete parameter choices for the boson mass and scattering length. They find that the LHY term produces a measurable reduction of the dimensionless moment of inertia at fixed compactness, while the approximate universal relation between moment of inertia and tidal deformability (the I-Λ relation familiar from neutron-star and quark-star physics) is preserved to within a few percent. The stellar models produced fall in the 1–2 solar mass, 10–20 km radius range currently probed by NICER and gravitational-wave detectors. The authors supply polynomial fits for the I-Λ and I-compactness relations and argue that the LHY footprint is large enough to serve as a diagnostic of beyond-mean-field quantum physics in a putative population of dark stars.

Core claim

The Lee-Huang-Yang beyond-mean-field correction, when self-consistently retained in the equation of state of slowly rotating Bose-Einstein condensate dark stars, shifts the moment of inertia at fixed compactness by an amount large enough to be observationally relevant, while the universal I-Λ relation — which links moment of inertia to tidal deformability independently of the equation of state — remains intact to within a few percent. This means the quantum-fluctuation signature is not washed out by the universality that normally erases EoS-level distinctions, making it a potentially clean diagnostic of beyond-mean-field physics in compact objects.

What carries the argument

The central mechanism is the Lee-Huang-Yang (LHY) correction: a subleading term in the pressure of a dilute Bose gas, proportional to the square root of the number density, that arises from quantum fluctuations beyond the mean-field Gross-Pitaevskii description. When inserted into the relativistic stellar structure equations (TOV for hydrostatic equilibrium, Hartle's dipole equation for frame-dragging under slow rotation, and a Riccati equation for the tidal Love number), this term modifies the pressure-density relation and thereby shifts the mass-radius curves, the moment of inertia, and the tidal deformability — but not the universal relation between the latter two.

Load-bearing premise

The polytropic n=1 equation of state with the LHY correction is derived for dilute gases where the dimensionless parameter n·a_s³ is much smaller than one. The paper applies this description to stellar interiors at supranuclear densities without explicitly verifying that the diluteness condition holds there, and the Thomas-Fermi approximation (neglecting quantum kinetic energy) is assumed throughout the star.

What would settle it

A measurement of both moment of inertia and tidal deformability for a compact object in the 1–2 solar mass range that lies on the I-Λ universal curve but shows no LHY-level deviation from the mean-field prediction would weaken the diagnostic claim — though it would not by itself rule out BEC dark stars, since the LHY correction could simply be too small for the particular (m, a_s) values realized.

Watch this falsifier — get emailed when new claim-graph text bears on it.

If this is right

  • If a population of compact objects is found whose moment-of-inertia and tidal-deformability measurements are consistent with the LHY-shifted I-Λ curve rather than the mean-field baseline, that would be evidence for beyond-mean-field quantum physics in the stellar interior.
  • The preservation of I-Λ universality for BEC dark stars means gravitational-wave measurements of tidal deformability alone could constrain the moment of inertia of a dark star without prior knowledge of whether it is a neutron star or a condensate star.
  • Combined with pulsar mass constraints (the two-solar-mass lower bound) and the equation-of-state interpretation of the light remnant HESS J1731-347, the LHY diagnostic could narrow the allowed (boson mass, scattering length) parameter space for dark matter.
  • The polynomial fits supplied for I-Λ and I-C relations can be used directly by future observational campaigns to test the BEC dark star hypothesis against measured compact-star properties.

Where Pith is reading between the lines

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

  • The fact that the I-Λ universal relation survives the LHY correction suggests that universality is governed by the gross gravitational structure (compactness, mass distribution) rather than by the microscopic physics of the interior — which would predict that other exotic compact objects (dark energy stars, boson stars with different self-interactions) should also lie on or near the same universal
  • The two-model approach (varying boson mass and scattering length) hints that future observations could invert the problem: given measured I, Λ, mass, and radius, one could in principle solve for the underlying particle parameters (m, a_s) of the dark matter boson, turning compact-star astronomy into a dark-matter particle-physics probe.
  • If the diluteness condition na_s³ ≪ 1 fails at the core densities of these stars (which the paper does not verify), the LHY correction itself may be unreliable — but the direction of its effect (stiffening or softening the EoS) would still indicate how higher-order quantum corrections would trend, so the diagnostic logic could survive even if the quantitative shift changes.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

2 major / 7 minor

Summary. This manuscript studies slowly rotating Bose-Einstein condensate (BEC) dark stars in General Relativity, incorporating the leading beyond-mean-field Lee-Huang-Yang (LHY) correction to the polytropic n=1 equation of state. The authors solve the TOV equations, Hartle's slow-rotation formalism for the frame-dragging function and moment of inertia, and the Riccati equation for the gravito-electric tidal Love number. Two representative parameter sets (Models A and B) are considered, each with and without the LHY correction. The main findings are: (1) the LHY term produces a measurable reduction of the dimensionless moment of inertia at fixed compactness, (2) the I-Lambda universal relation is preserved to within a few percent, and (3) polynomial fits for the I-Lambda and I-C relations are provided. The authors claim the LHY footprint is large enough to serve as a clean diagnostic of beyond-mean-field quantum physics.

Significance. The paper applies a well-established theoretical framework (TOV + Hartle + Hinderer/Postnikov tidal formalism) to a specific exotic compact object model. The inclusion of the LHY correction in the rotating case is a natural extension of the authors' prior non-rotating work (Ref. [22]). The provision of polynomial fits for the I-Lambda and I-C relations for BEC dark stars is a useful contribution for the community. The framework is standard and correctly applied, and the parameter choices yield objects in the observationally relevant mass-radius window.

major comments (2)
  1. Abstract and Section 4: The claim that the LHY footprint is 'large enough to serve as a clean diagnostic of beyond-mean-field quantum physics' is not quantitatively supported. The paper itself states that the I-Lambda relation is preserved 'to within a few per cent,' which is well inside the known ~10% intrinsic scatter of the I-Love-Q universal relations across hadronic EoS models (Yagi & Yunes 2017, Ref. [25]). The I-C relation (Fig. 4) does show a larger visible shift, but using it as a diagnostic requires independent measurements of both I and C, and the moment of inertia has never been measured for any compact object. Without a single quantitative comparison between the LHY-induced fractional shift and either (a) realistic observational uncertainties for tidal deformability (currently ~50-100% for individual GW events) or (b) the intrinsic scatter of hadronic I-Love-Q relations, the
  2. Section 3, discussion of Fig. 4: The text states that 'nearly identical trends for all four cases' are observed in the I-C plot, but the figure appears to show a visible separation between the zeta=0 and zeta=1 curves at a level (~10-15% by eye at C~0.15) that is larger than the 'few per cent' cited for the I-Lambda relation. This apparent tension between the I-Lambda universality claim and the I-C shift should be clarified. If the I-C shift is indeed the primary observable signature, the authors should state this explicitly and quantify it, rather than emphasizing the I-Lambda preservation.
minor comments (7)
  1. Throughout: The paper refers to 'I-Love-Q' universal relations, but only the I-Lambda and I-C subsets are computed; the quadrupole moment Q is not calculated. The title 'I-Love-Q programme' is used loosely; consider clarifying that only the I-Love subset is tested.
  2. Section 3, Eq. (50): The parameter zeta is introduced as a 'dimensionless free parameter' but only takes values 0 or 1 in the analysis. Calling it a free parameter when it functions as a binary switch between {0,1} would be clearer.
  3. Section 3, after Eq. (59): The decision not to quote an I-bar(C) fit for Model B at zeta=1, while providing one for Model A, is somewhat asymmetric. A brief justification or at least a note that the Y(z) form suffices would help the reader.
  4. Section 2.2, Eq. (26): The moment of inertia integral involves the ratio omega-tilde/Omega, but the numerical procedure for obtaining this ratio (e.g., the shooting method or boundary condition matching) is not described. A brief mention of the numerical method would improve reproducibility.
  5. No numerical convergence tests or error estimates are shown for the TOV, Hartle, or Riccati integrations. While the framework is standard, a brief statement of the numerical accuracy (e.g., relative tolerance) would strengthen the fits in Table 1 and Eqs. (57)-(59).
  6. Fig. 1: The two panels appear to use different x-axis ranges (0-1.5 vs. 0-2.0 solar masses) without clear justification. Consider using the same range or explaining the choice.
  7. Section 1: The phrase 'the great open question' is somewhat informal; consider rephrasing.

Circularity Check

0 steps flagged

No significant circularity; derivation is self-contained against standard external physics.

full rationale

The paper's derivation chain is straightforward and non-circular. The EoS (Eq. 50) is the standard Lee-Huang-Yang correction from many-body theory (Lee, Huang, Yang 1957, Ref. [20]) — an external, parameter-free result with stated assumptions (dilute gas, na_s³≪1) that do not include the target quantities (I, Λ, C). The TOV equations (Eqs. 5–7), Hartle's slow-rotation formalism (Eqs. 11–26), and the tidal Love number machinery (Eqs. 27–37) are all standard GR results from external sources. The numerical integration of these equations produces the stellar sequences, and the polynomial fits (Eqs. 54–59) are explicitly labeled as least-squares fits to numerical data — not presented as predictions. The central claim (LHY reduces Ī at fixed C) follows from applying a known EoS correction to known structure equations and reading off the output; no step reduces to its own inputs by construction. The self-citation to Ref. [22] (same first author) is for parameter choices (Models A, B) and verification of the non-rotating baseline, which is a consistency check rather than a load-bearing theoretical dependency. The 'clean diagnostic' claim is an interpretive extrapolation (more properly a correctness/overclaiming concern) rather than a circular derivation step. No step in the chain exhibits self-definitional, fitted-input-as-prediction, or self-citation-load-bearing circularity.

Axiom & Free-Parameter Ledger

4 free parameters · 4 axioms · 1 invented entities

The paper introduces no new fundamental entities beyond the BEC dark star concept from prior literature. The free parameters (m, a_s) are chosen by hand to match observational mass ranges. The key domain assumptions (Thomas-Fermi, diluteness) are standard for dilute Bose gases but their validity at compact-star densities is the main unverified premise.

free parameters (4)
  • m (boson mass) = 0.50 GeV (Model A), 0.45 GeV (Model B)
    Chosen by hand to produce stellar masses in the 1-2 solar mass range; not fitted to data but selected to be compatible with observations.
  • a_s (s-wave scattering length) = 0.10 fm (Model A), 0.11 fm (Model B)
    Chosen by hand alongside m; same rationale as above.
  • zeta (LHY switch) = 0 or 1
    Dimensionless parameter introduced in Eq. (50) to toggle the LHY correction on or off; not a physical free parameter but a computational switch.
  • Polynomial fit coefficients {a,b,c,d,e} and {a0,a1,a2} = Tabulated in Table 1 and Eqs. 57-59
    Fitted to numerical sequences via least-squares; these are empirical fits, not fundamental parameters.
axioms (4)
  • domain assumption Thomas-Fermi approximation: the quantum kinetic term is negligible compared to the interaction term in the Gross-Pitaevskii equation.
    Invoked in Section 3 to derive the polytropic EoS p = K*rho^2. Validity at supranuclear densities is not verified.
  • domain assumption Diluteness condition na_s^3 << 1 holds throughout the stellar interior.
    Required for the LHY expansion (Eqs. 47-49) to be valid. Not checked at the densities of a 1-2 solar mass compact star.
  • standard math Hartle slow-rotation formalism is valid, i.e., J/M^2 << 1 (angular velocity small compared to Keplerian).
    Standard approximation in general relativity; invoked in Section 2.2. Valid for millisecond pulsars but not for rapidly rotating objects.
  • domain assumption The I-Love-Q universal relations hold for BEC dark stars as they do for neutron stars and quark stars.
    Assumed based on prior work by Yagi and Yunes [23-25]; verified numerically in this paper to within a few percent.
invented entities (1)
  • BEC dark star (self-gravitating Bose-Einstein condensate of dark matter) no independent evidence
    purpose: Alternative compact object model composed of bosonic dark matter
    No direct observational evidence for BEC dark stars exists. The paper provides falsifiable predictions (I-C relation shifts) but no current observation confirms the entity. The concept originates from prior literature [9-11].

pith-pipeline@v1.1.0-glm · 20113 in / 2784 out tokens · 240296 ms · 2026-07-09T23:20:16.588091+00:00 · methodology

0 comments
read the original abstract

We investigate rotational properties and universal relations of slowly rotating Bose-Einstein condensate dark stars in the context of General Relativity, both at the mean-field level and when the leading beyond-mean-field Lee-Huang-Yang correction is retained self-consistently. Adopting the polytropic $n=1$ equation of state appropriate to a dilute, self-interacting Bose gas, parameterised by the boson mass $m$ and the $s$-wave scattering length $a_s$, we integrate the Tolman-Oppenheimer-Volkoff equations together with Hartle's dipole equation for the frame-dragging angular velocity, and we compute the moment of inertia, the gravito-electric tidal Love number and the dimensionless tidal deformability. The resulting equilibrium sequences yield gravitational masses in the $1$--$2\,M_{\odot}$ range with radii of $10$--$20\,\mathrm{km}$, squarely within the window presently probed by NICER and the LIGO-Virgo-KAGRA network. We observe that the LHY term produces a measurable reduction of the dimensionless moment of inertia at fixed compactness, whilst the I-$\Lambda$ universal relation is preserved to within a few per cent. We supply polynomial fits for the I-$\Lambda$ and I-$C$ relations, and show that the LHY footprint is large enough to serve as a clean diagnostic of beyond-mean-field quantum physics in a putative dark star population, complementing existing dark matter constraints from pulsar masses and from the equation-of-state interpretation of the unusually light compact remnant HESS~J1731-347.

Figures

Figures reproduced from arXiv: 2607.06898 by \'Angel Rinc\'on, Grigoris Panotopoulos, Ilidio Lopes.

Figure 1
Figure 1. Figure 1: Gravitational red-shift versus stellar mass for model A (in blue color) and model B [PITH_FULL_IMAGE:figures/full_fig_p012_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Moment of inertia I/R3 as a function of the stellar mass M (in solar masses) for two different EoS and different values of the parameters {m, as}. The color code is given as follow: i) Dashed blue line corresponds to Model A (ζ = 0), ii) Solid blue line corresponds to Model A (ζ = 1), iii) Dashed red line corresponds to Model B (ζ = 0), and finally iv) Solid red line corresponds to Model B (ζ = 1). 13 [PI… view at source ↗
Figure 3
Figure 3. Figure 3: Universal relations I − Λ for two different EoS and different values of the parameters {m, as}. The color code is given as follow: i) Dashed blue line corresponds to Model A (ζ = 0), ii) Solid blue line corresponds to Model A (ζ = 1), iii) Dashed red line corresponds to Model B (ζ = 0), and finally iv) Solid red line corresponds to Model B (ζ = 1). Bullets correspond to numerical points, whereas the contin… view at source ↗
Figure 4
Figure 4. Figure 4: Universal relations I − C for two different EoS and different values of the parameters {m, as}. The color code is given as follow: i) Dashed blue line corresponds to Model A (ζ = 0), ii) Solid blue line corresponds to Model A (ζ = 1), iii) Dashed red line corresponds to Model B (ζ = 0), and finally iv) Solid red line corresponds to Model B (ζ = 1). Bullets correspond to numerical points, whereas the contin… view at source ↗

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Reference graph

Works this paper leans on

65 extracted references · 65 canonical work pages · 45 internal anchors

  1. [1]

    S. L. Shapiro and S. A. Teukolsky,Black holes, white dwarfs, and neutron stars: The physics of compact objects. Wiley-Interscience, New York, 1983. https://doi.org/10.1002/9783527617661

    work page doi:10.1002/9783527617661 1983

  2. [2]

    N. K. Glendenning,Compact Stars: Nuclear Physics, Particle Physics, and General Relativity. Astronomy and Astrophysics Library. Springer-Verlag, New York, 2nd ed., 2000. https://ui.adsabs.harvard.edu/abs/2000csnp.conf.....G

    work page 2000

  3. [3]

    Haensel, A

    P. Haensel, A. Y. Potekhin, and D. G. Yakovlev,Neutron Stars 1: Equation of State and Structure, vol. 326 ofAstrophysics and Space Science Library. Springer, New York, 2007. https://doi.org/10.1007/978-0-387-47301-7

    work page doi:10.1007/978-0-387-47301-7 2007

  4. [4]

    The Nuclear Equation of State and Neutron Star Masses

    J. M. Lattimer, “The Nuclear Equation of State and Neutron Star Masses,”Annual Review of Nuclear and Particle Science62no. 1, (Nov., 2012) 485–515,arXiv:1305.3510 [nucl-th]

    work page internal anchor Pith review Pith/arXiv arXiv 2012

  5. [5]

    Neutron stars and the dense matter equation of state,

    K. Chatziioannou, H. T. Cromartie, S. Gandolfi, I. Tews, D. Radice, A. W. Steiner, and A. L. Watts, “Neutron stars and the dense matter equation of state,”Reviews of Modern Physics97no. 4, (Oct., 2025) 045007,arXiv:2407.11153 [nucl-th]

    work page arXiv 2025

  6. [6]

    The Physics of Neutron Stars

    J. M. Lattimer and M. Prakash, “The Physics of Neutron Stars,”Science304no. 5670, (Apr., 2004) 536–542,arXiv:astro-ph/0405262 [astro-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2004

  7. [7]

    The Equation of State of Hot, Dense Matter and Neutron Stars

    J. M. Lattimer and M. Prakash, “The equation of state of hot, dense matter and neutron stars,”Phys. Rep.621(Mar., 2016) 127–164,arXiv:1512.07820 [astro-ph.SR]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  8. [8]

    Neutron Stars and the Nuclear Matter Equation of State,

    J. M. Lattimer, “Neutron Stars and the Nuclear Matter Equation of State,”Annual Review of Nuclear and Particle Science71(Sept., 2021) 433–464

    work page 2021

  9. [9]

    Can dark matter be a Bose-Einstein condensate?

    C. G. B¨ ohmer and T. Harko, “Can dark matter be a Bose-Einstein condensate?,”J. Cosmol. Astropart. Phys.2007no. 06, (2007) 025,0705.4158

    work page internal anchor Pith review Pith/arXiv arXiv 2007

  10. [10]

    Bose-Einstein Condensate general relativistic stars

    P.-H. Chavanis and T. Harko, “Bose-Einstein Condensate general relativistic stars,”Phys. Rev. D86no. 6, (2012) 064011,1108.3986. 19

    work page internal anchor Pith review Pith/arXiv arXiv 2012

  11. [12]

    Boson Stars: Gravitational Equilibria of Selfinteracting Scalar Fields,

    M. Colpi, S. L. Shapiro, and I. Wasserman, “Boson Stars: Gravitational Equilibria of Selfinteracting Scalar Fields,”Phys. Rev. Lett.57(1986) 2485–2488

    work page 1986

  12. [13]

    Mass-radius relation of Newtonian self-gravitating Bose-Einstein condensates with short-range interactions: I. Analytical results

    P.-H. Chavanis, “Mass-radius relation of Newtonian self-gravitating Bose-Einstein condensates with short-range interactions. I. Analytical results,”Phys. Rev. D84no. 4, (2011) 043531,1103.2050

    work page internal anchor Pith review Pith/arXiv arXiv 2011

  13. [14]

    Bosonic dark matter dynamics in hybrid neutron stars

    Z. Buras-Stubbs and I. Lopes, “Bosonic dark matter dynamics in hybrid neutron stars,” Phys. Rev. D109no. 4, (Feb., 2024) 043043,arXiv:2402.19238 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2024

  14. [15]

    The Radius of PSR J0740+6620 from NICER and XMM-Newton Data

    M. C. Milleret al., “The Radius of PSR J0740+6620 from NICER and XMM-Newton Data,”Astrophys. J. Lett.918no. 2, (2021) L28,arXiv:2105.06979 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2021

  15. [16]

    A NICER View of the Massive Pulsar PSR J0740+6620 Informed by Radio Timing and XMM-Newton Spectroscopy

    T. E. Rileyet al., “A NICER View of the Massive Pulsar PSR J0740+6620 Informed by Radio Timing and XMM-Newton Spectroscopy,”Astrophys. J. Lett.918no. 2, (2021) L27, arXiv:2105.06980 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2021

  16. [17]

    A NICER View of the Nearest and Brightest Millisecond Pulsar: PSR J0437$\unicode{x2013}$4715

    D. Choudhuryet al., “A NICER View of the Nearest and Brightest Millisecond Pulsar: PSR J0437–4715,”Astrophys. J. Lett.971no. 1, (2024) L20,arXiv:2407.06789 [astro-ph.HE]. [18]LIGO Scientific, VirgoCollaboration, B. P. Abbottet al., “GW170817: Observation of Gravitational Waves from a Binary Neutron Star Inspiral,”Phys. Rev. Lett.119no. 16, (2017) 161101,a...

    work page internal anchor Pith review Pith/arXiv arXiv 2024

  17. [18]

    Eigenvalues and Eigenfunctions of a Bose System of Hard Spheres and Its Low-Temperature Properties,

    T. D. Lee, K. Huang, and C. N. Yang, “Eigenvalues and Eigenfunctions of a Bose System of Hard Spheres and Its Low-Temperature Properties,”Physical Review106no. 6, (1957) 1135–1145

    work page 1957

  18. [19]

    Ferroelectricity driven magnetism at domain walls in LaAlO$_3$/PbTiO$_3$ superlattices

    D. S. Petrov, “Quantum Mechanical Stabilization of a Collapsing Bose-Bose Mixture,” Phys. Rev. Lett.115no. 15, (2015) 155302,1508.02889

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  19. [20]

    Condensate Dark Stars Beyond the Mean-Field Approximation: The Lee-Huang-Yang Correction,

    G. Panotopoulos, “Condensate Dark Stars Beyond the Mean-Field Approximation: The Lee-Huang-Yang Correction,”Physics8no. 1, (2026) 32,2601.05506

    work page arXiv 2026

  20. [24]

    Slowly rotating relativistic stars. 1. Equations of structure,

    J. B. Hartle, “Slowly rotating relativistic stars. 1. Equations of structure,”Astrophys. J. 150(1967) 1005–1029

    work page 1967

  21. [25]

    Rotating Stars in Relativity

    V. Paschalidis and N. Stergioulas, “Rotating Stars in Relativity,”Living Rev. Rel.20no. 1, (2017) 7,arXiv:1612.03050 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  22. [27]

    Tidal Love numbers of neutron stars

    T. Hinderer, “Tidal Love numbers of neutron stars,”Astrophys. J.677(2008) 1216–1220, arXiv:0711.2420 [astro-ph]. [Erratum: Astrophys.J. 697, 964 (2009)]

    work page internal anchor Pith review Pith/arXiv arXiv 2008

  23. [28]

    Constraining neutron star tidal Love numbers with gravitational wave detectors

    ´E. ´E. Flanagan and T. Hinderer, “Constraining neutron-star tidal Love numbers with gravitational-wave detectors,”Phys. Rev. D77no. 2, (2008) 021502,0709.1915

    work page internal anchor Pith review Pith/arXiv arXiv 2008

  24. [30]

    Tidal Love Numbers of Neutron and Self-Bound Quark Stars

    S. Postnikov, M. Prakash, and J. M. Lattimer, “Tidal Love numbers of neutron and self-bound quark stars,”Phys. Rev. D82no. 2, (2010) 024016,1004.5098

    work page internal anchor Pith review Pith/arXiv arXiv 2010

  25. [31]

    Influence of N,N,N-trimethyl-1-adamantyl ammonium (TMAda+) Structure Directing Agent on Al Pair Distributions and Features in Chabazite Zeolite

    G. Panotopoulos, ´A. Rinc´ on, and I. Lopes, “Slowly rotating dark energy stars,”Physics of the Dark Universe34(2021) 100885,2110.12523

    work page internal anchor Pith review Pith/arXiv arXiv 2021

  26. [32]

    Dynamical Mean-Field Theory for Markovian Open Quantum Many-Body Systems

    G. Panotopoulos, ´A. Rinc´ on, and I. Lopes, “Radial oscillations and tidal Love numbers of dark energy stars,”European Physical Journal Plus135no. 10, (2020) 856,2008.02563

    work page internal anchor Pith review Pith/arXiv arXiv 2020

  27. [33]

    Neutron stars: new constraints on asymmetric dark matter

    O. Ivanytskyi, V. Sagun, and I. Lopes, “Neutron stars: New constraints on asymmetric dark matter,”Phys. Rev. D102no. 6, (Sept., 2020) 063028,arXiv:1910.09925 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2020

  28. [34]

    A sharpened Riesz-Sobolev inequality

    I. Lopes and G. Panotopoulos, “Dark matter admixed strange quark stars in the Starobinsky model of gravity,”Phys. Rev. D97no. 2, (2018) 024030,1706.02007

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  29. [35]

    A strangely light neutron star within a supernova remnant,

    V. Doroshenko, V. Suleimanov, G. P¨ uhlhofer, and A. Santangelo, “A strangely light neutron star within a supernova remnant,”Nature Astronomy6(Dec., 2022) 1444–1451

    work page 2022

  30. [36]

    Quark Models and Radial Oscillations: Decoding the HESS J1731-347 Compact Object's Equation of State

    I. A. Rather, G. Panotopoulos, and I. Lopes, “Quark models and radial oscillations: decoding the HESS J1731-347 compact object’s equation of state,”European Physical Journal C83no. 11, (Nov., 2023) 1065,arXiv:2307.03703 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2023

  31. [37]

    Asteroseismology: radial oscillations of neutron stars with realistic equation of state

    V. Sagun, G. Panotopoulos, and I. Lopes, “Asteroseismology: Radial oscillations of neutron stars with realistic equation of state,”Phys. Rev. D101no. 6, (Mar., 2020) 063025, arXiv:2002.12209 [astro-ph.HE]. 21

    work page internal anchor Pith review Pith/arXiv arXiv 2020

  32. [38]

    What is the nature of the HESS J1731-347 compact object?

    V. Sagun, E. Giangrandi, T. Dietrich, O. Ivanytskyi, R. Negreiros, and C. Providˆ encia, “What Is the Nature of the HESS J1731-347 Compact Object?,”Astrophys. J.958no. 1, (Nov., 2023) 49,arXiv:2306.12326 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2023

  33. [39]

    Is the Compact Object Associated with HESS J1731-347 a Strange Quark Star? A Possible Astrophysical Scenario for Its Formation,

    F. Di Clemente, A. Drago, and G. Pagliara, “Is the Compact Object Associated with HESS J1731-347 a Strange Quark Star? A Possible Astrophysical Scenario for Its Formation,” Astrophys. J.967no. 2, (June, 2024) 159,arXiv:2211.07485 [gr-qc]

    work page arXiv 2024

  34. [40]

    Static Solutions of Einstein’s Field Equations for Spheres of Fluid,

    R. C. Tolman, “Static Solutions of Einstein’s Field Equations for Spheres of Fluid,”Phys. Rev. D55no. 4, (1939) 364–373

    work page 1939

  35. [41]

    On Massive Neutron Cores,

    J. R. Oppenheimer and G. M. Volkoff, “On Massive Neutron Cores,”Phys. Rev. D55 no. 4, (1939) 374–381

    work page 1939

  36. [42]

    An introduction to the theory of rotating relativistic stars

    E. Gourgoulhon, “An Introduction to the theory of rotating relativistic stars,” inCompStar 2010: School and Workshop on Computational Tools for Compact Star Astrophysics. 3, 2010.arXiv:1003.5015 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2010

  37. [43]

    Slowly rotating neutron and strange stars in $R^2$ gravity

    K. V. Staykov, D. D. Doneva, S. S. Yazadjiev, and K. D. Kokkotas, “Slowly rotating neutron and strange stars inR 2 gravity,”JCAP10(2014) 006,arXiv:1407.2180 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2014

  38. [44]

    Millisecond pulsars modelled as strange quark stars admixed with condensed dark matter

    G. Panotopoulos and I. Lopes, “Millisecond pulsars modeled as strange quark stars admixed with condensed dark matter,”Int. J. Mod. Phys. D27no. 09, (2018) 1850093, arXiv:1804.05023 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  39. [45]

    Moments of inertia for neutron and strange stars: limits derived for the Crab pulsar

    M. Bejger and P. Haensel, “Moments of inertia for neutron and strange stars: Limits derived for the Crab pulsar,”Astron. Astrophys.396(2002) 917,arXiv:astro-ph/0209151

    work page internal anchor Pith review Pith/arXiv arXiv 2002

  40. [46]

    Relativistic tidal properties of neutron stars

    T. Damour and A. Nagar, “Relativistic tidal properties of neutron stars,”Phys. Rev. D80 (2009) 084035,arXiv:0906.0096 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2009

  41. [47]

    Relativistic theory of tidal Love numbers

    T. Binnington and E. Poisson, “Relativistic theory of tidal Love numbers,”Phys. Rev. D 80(2009) 084018,arXiv:0906.1366 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2009

  42. [48]

    Nuclear physics constraints from binary neutron star mergers in the Einstein Telescope era

    F. Iacovelli, M. Mancarella, C. Mondal, A. Puecher, T. Dietrich, F. Gulminelli, M. Maggiore, and M. Oertel, “Nuclear physics constraints from binary neutron star mergers in the Einstein Telescope era,”Phys. Rev. D108no. 12, (2023) 122006,arXiv:2308.12378 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2023

  43. [49]

    Extreme Love in the SPA: constraining the tidal deformability of supermassive objects with extreme mass ratio inspirals and semi-analytical, frequency-domain waveforms

    G. A. Piovano, A. Maselli, and P. Pani, “Constraining the tidal deformability of supermassive objects with extreme mass ratio inspirals and semianalytical frequency-domain waveforms,”Phys. Rev. D107no. 2, (2023) 024021,arXiv:2207.07452 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2023

  44. [50]

    Neutron Star Observations: Prognosis for Equation of State Constraints

    J. M. Lattimer and M. Prakash, “Neutron Star Observations: Prognosis for Equation of State Constraints,”Phys. Rept.442(2007) 109–165,arXiv:astro-ph/0612440. 22

    work page internal anchor Pith review Pith/arXiv arXiv 2007

  45. [51]

    Equations of state for supernovae and compact stars

    M. Oertel, M. Hempel, T. Kl¨ ahn, and S. Typel, “Equations of state for supernovae and compact stars,”Rev. Mod. Phys.89no. 1, (2017) 015007,arXiv:1610.03361 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  46. [52]

    Gravitational decoupled anisotropies in compact stars

    L. Gabbanelli, ´A. Rinc´ on, and C. Rubio, “Gravitational decoupled anisotropies in compact stars,”Eur. Phys. J. C78no. 5, (2018) 370,arXiv:1802.08000 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  47. [53]

    Relativistic Anisotropic Fluid Spheres Satisfying a Non-Linear Equation of State

    F. Tello-Ortiz, M. Malaver, ´A. Rinc´ on, and Y. Gomez-Leyton, “Relativistic anisotropic fluid spheres satisfying a non-linear equation of state,”Eur. Phys. J. C80no. 5, (2020) 371,arXiv:2005.11038 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2020

  48. [54]

    Anisotropic strange quark stars with a non-linear equation-of-state

    I. Lopes, G. Panotopoulos, and ´A. Rinc´ on, “Anisotropic strange quark stars with a non-linear equation-of-state,”Eur. Phys. J. Plus134no. 9, (2019) 454,arXiv:1907.03549 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  49. [55]

    Durgapal IV model in light of the minimal geometric deformation approach

    F. Tello-Ortiz, ´A. Rinc´ on, P. Bhar, and Y. Gomez-Leyton, “Durgapal IV model in light of the minimal geometric deformation approach,”Chin. Phys. C44(2020) 105102, arXiv:2006.04512 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2020

  50. [56]

    A Generalized Double Chaplygin Model for Anisotropic Matter: The Newtonian Case

    G. Abell´ an, A. Rincon, and E. Sanchez, “A Generalized Double Chaplygin Model for Anisotropic Matter: The Newtonian Case,”Universe9no. 8, (2023) 352, arXiv:2308.12236 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2023

  51. [57]

    Anisotropic interior solution by gravitational decoupling based on a non-standard anisotropy,

    G. Abell´ an,´A. Rinc´ on, E. Fuenmayor, and E. Contreras, “Anisotropic interior solution by gravitational decoupling based on a non-standard anisotropy,”Eur. Phys. J. Plus135 no. 7, (2020) 606

    work page 2020

  52. [58]

    Condensate dark matter stars

    X. Y. Li, T. Harko, and K. S. Cheng, “Condensate dark matter stars,”JCAP06(2012) 001,arXiv:1205.2932 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2012

  53. [59]

    Phase transitions between dilute and dense axion stars

    P.-H. Chavanis, “Phase transitions between dilute and dense axion stars,”Phys. Rev. D98 no. 2, (2018) 023009,arXiv:1710.06268 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  54. [60]

    Abramowitz and I

    M. Abramowitz and I. A. Stegun, eds.,Handbook of Mathematical Functions with Formulas, Graphs, and Mathematical Tables, vol. 55 ofApplied Mathematics Series. Dover Publications, New York, 9th ed., 1972. https://ui.adsabs.harvard.edu/abs/1988AmJPh..56..958A

    work page 1972

  55. [61]

    Chandrasekhar,An Introduction to the Study of Stellar Structure

    S. Chandrasekhar,An Introduction to the Study of Stellar Structure. Astrophysical Monographs. University of Chicago Press, Chicago, 1939. https://archive.org/details/AnIntroductionToTheStudyOfStellarStructure. Reprinted by Dover Publications, New York, 1958

    work page 1939

  56. [62]

    Fetter and J

    A. Fetter and J. D. Valecka,Quantum Theory of Many-Particle Systems. Physics Series. Dover Publications, Inc., 2003

    work page 2003

  57. [63]

    R. K. Pathria and P. D. Beale,Statistical Mechanics. Academic Press, Elsevier, Oxford, 3rd ed., 2011.https://doi.org/10.1016/C2009-0-62310-2. 23

    work page doi:10.1016/c2009-0-62310-2 2011

  58. [64]

    On the theory of superfluidity,

    N. N. Bogolyubov, “On the theory of superfluidity,”J. Phys. (USSR)11(1947) 23–32. https://inspirehep.net/literature/45477. Also published as Izv. Akad. Nauk Ser. Fiz. 11(1947) 77–90

    work page 1947

  59. [65]

    PSR J0030+0451 Mass and Radius from NICER Data and Implications for the Properties of Neutron Star Matter

    M. C. Milleret al., “PSR J0030+0451 Mass and Radius fromN ICERData and Implications for the Properties of Neutron Star Matter,”Astrophys. J. Lett.887no. 1, (2019) L24,arXiv:1912.05705 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  60. [66]

    Photon and neutrino redshift in the field of braneworld compact stars

    J. Hladik and Z. Stuchlik, “Photon and neutrino redshift in the field of braneworld compact stars,”JCAP07(2011) 012,arXiv:1108.5760 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2011

  61. [67]

    I-Love-Q

    K. Yagi and N. Yunes, “I-Love-Q,”Science341(2013) 365–368,arXiv:1302.4499 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2013

  62. [68]

    I-Love-Q Relations in Neutron Stars and their Applications to Astrophysics, Gravitational Waves and Fundamental Physics

    K. Yagi and N. Yunes, “I-Love-Q Relations in Neutron Stars and their Applications to Astrophysics, Gravitational Waves and Fundamental Physics,”Phys. Rev. D88no. 2, (2013) 023009,arXiv:1303.1528 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2013

  63. [69]

    Approximate Universal Relations for Neutron Stars and Quark Stars

    K. Yagi and N. Yunes, “Approximate Universal Relations for Neutron Stars and Quark Stars,”Phys. Rept.681(2017) 1–72,arXiv:1608.02582 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  64. [70]

    Constraining the Equation of State with Moment of Inertia Measurements

    J. M. Lattimer and B. F. Schutz, “Constraining the equation of state with moment of inertia measurements,”Astrophys. J.629(2005) 979–984,arXiv:astro-ph/0411470

    work page internal anchor Pith review Pith/arXiv arXiv 2005

  65. [71]

    Rotational behavior of exotic compact objects,

    Z. Buras-Stubbs and I. Lopes, “Rotational behavior of exotic compact objects,”Phys. Rev. D113no. 4, (2026) 043049,2601.07811. 24

    work page arXiv 2026