REVIEW 3 major objections 3 minor 65 references
Treating disk clumps as spinning test bodies lets a general-relativistic model fit the twin kilohertz QPOs of eight neutron-star X-ray binaries without inventing an effective cosmological constant, and the fits read out the disk's internal
Reviewed by Pith at T0; open to challenge. T0 means a machine referee read the full paper against a public rubric. the ladder, T0–T4 →
T0 review · deepseek-v4-flash
2026-08-01 05:05 UTC pith:XULPTIWB
load-bearing objection Plausible MPM extension of the RPM with MPD spin corrections, but the statistical preference over SdS is not established from the printed evidence table. the 3 major comments →
The macroscopic precession model of quasi-periodic oscillations for rotating compact objects
The pith
A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.
Core claim
The paper's central claim is that the frequency splitting of twin kilohertz QPOs can be reproduced by non-minimal spin-curvature coupling of macroscopic disk inhomogeneities, without any ad hoc modification of the Kerr or Schwarzschild spacetime. By adopting the specific spin tensor S^tr = C_n r^n, the model yields modified azimuthal and radial epicyclic frequencies whose leading corrections depend on the power-law index n. Monte Carlo Markov chain fits to eight neutron-star sources show that the macroscopic precession model in Schwarzschild spacetime outperforms the effective Schwarzschild-de Sitter model in five sources and is statistically equivalent in three, while the Kerr version never
What carries the argument
The central machinery is the Mathisson-Papapetrou-Dixon (MPD) system for a spinning test body, together with the Tulczyjew-Dixon spin condition and the extra symmetry condition that the spin is orthogonal to the orbital plane. The spin tensor ansatz S^tr = C_n r^n, with fixed integer n = 1, 2, 3, encodes the geometry of the accreting flow (filament-like, thin-disk, thick-disk). The first-order-in-spin corrections to the Keplerian frequency and to the squared radial epicyclic frequency, equations (A.1)–(A.4), carry the entire physical effect; they replace the effective cosmological constant of the Schwarzschild-de Sitter model by a genuine spin-curvature interaction term.
Load-bearing premise
The load-bearing premise is that the internal spin structure of disk clumps is exactly a power law, S^tr = C_n r^n, with a fixed integer n and a freely fitted amplitude; if real disk inhomogeneities do not follow this form, the claimed selection of internal structure and the statistical success over the Schwarzschild-de Sitter model would be artifacts of that parametrization.
What would settle it
A clean falsifier is a neutron-star (or black-hole) QPO source whose best-fit requires κ ≳ 1 in the emitting region, since the test-particle approximation would fail exactly where the model claims to work. A second falsifier is a robust statistical preference for the Kerr version of the model with well-constrained physical mass and high spin — such a source would indicate that central rotation, not disk spin, drives the frequency splittings, contradicting the paper's conclusion that the Schwarzschild version is favored.
If this is right
- The plain Schwarzschild relativistic precession model (RPM-S) is statistically always disfavored by the eight sources, so it is effectively ruled out as a description of twin kHz QPOs.
- The phenomenological Schwarzschild-de Sitter model (RPM-SdS), which previously dominated the fits, is overtaken or matched by the spinning-test-body model in all eight sources, suggesting the apparent cosmological constant is a surrogate for neglected spin effects.
- In six of eight sources the fitted disk index is n = 2, i.e., a disk-like internal structure, while two sources prefer n = 3; this is the first QPO-based hint that the data select the internal structure of accreting matter.
- The Kerr-based version of the model (MPM-K) restores physically acceptable neutron-star masses and spins wherever the RPM-Kerr model gave absurd values, even though rotation of the central object does not statistically improve the fits.
- The inferred disk radii satisfy the radial ordering condition and provide an absolute upper bound on the disk radius where the test-particle approximation breaks down, giving a concrete, testable scale for each source.
Where Pith is reading between the lines
- If the power-law ansatz for the spin tensor were replaced by a physically derived model of disk turbulence or clump formation, the fitted index n would acquire a direct microphysical meaning; the current n-clustering is an invitation to construct such a model.
- The analysis suggests a sharp observational test for black-hole binaries: a measured QPO source with independently known spin j that strongly prefers the Kerr version of the model (with n = 1) would indicate that central rotation, not disk structure, is being probed.
- The degeneracy between the amplitude C_n and the mass M in the fits deserves closer scrutiny; a dedicated posterior-correlation analysis would clarify whether the claimed preference for n = 2 reflects genuine disk structure or merely absorbs the freedom in the ansatz.
- If the spin-curvature mechanism is correct, the ratio of the lower to upper QPO frequency should deviate from the geodesic RPM relation in a way that depends on n; a precision measurement of this ratio in a single source could discriminate n without full MCMC.
Editorial analysis
A structured set of objections, weighed in public.
Referee Report
Summary. The paper proposes a 'macroscopic precession model' (MPM) in which the twin kilohertz QPOs of eight neutron-star X-ray binaries are produced not by structureless test particles but by small spinning bodies governed by the Mathisson-Papapetrou-Dixon equations. The authors compute first-order spin-curvature corrections to the Keplerian and radial epicyclic frequencies in Kerr and Schwarzschild backgrounds, parametrize the spin tensor by the power-law ansatz S^{tr}=C_n r^n, and perform MCMC fits for n=1,2,3. They compare MPM with the standard relativistic precession model (RPM) in Schwarzschild, Kerr, and Schwarzschild–de Sitter variants, and claim that MPM-S outperforms RPM-SdS in five sources, clusters toward n=2 ('thin-disk' configurations), and removes the need for an effective cosmological-constant term, while healing the unphysical masses and spins found in RPM-K.
Significance. If the central claim were robust, this would be an interesting contribution: it offers a physically motivated alternative to the phenomenological SdS phase in QPO fitting and suggests that QPO data could constrain the internal structure of accreting matter. The perturbative MPD formalism is standard, and the paper is transparent about the explicit spin corrections in Appendix A. The use of a common MCMC pipeline across models and the articulation of two falsifiability tests in the conclusions are also positive features. However, the significance is presently limited by three load-bearing problems: the statistical evidence is not reported consistently, the quoted mass prior is violated by the displayed RPM-K best fits, and the power-law spin ansatz is introduced by hand. These issues prevent the paper from supporting its headline statistical and physical conclusions as written.
major comments (3)
- [§3 and Table B.1] The statistical criterion is internally inconsistent and does not reproduce the text's headline claim. The text defines Δ = lnB_i − lnB_0 with lnB_0 = min{lnB_i}, then states that 0≤Δ≤1 means 'weakly excluded'; under this definition the best model has Δ=0 and is automatically 'weakly excluded', which is contradictory. More seriously, Table B.1 does not support the claim that MPM-S outperforms RPM-SdS by Δ>6 in five sources. For example, GX 17+2 lists Δ=0 for both models; Cir X1 lists 3 vs 7 (difference 4); 4U1608–52 lists 1 vs 5 (difference 4). Only Sco X1 and 4U0614+091 show differences larger than 6. Since the abstract's conclusion is explicitly a statistical selection, the evidence values need to be recomputed, clearly defined, and reported with a consistent reference model before the central claim can be assessed.
- [§2.1, Eq. (20)] The physical content of the model is fixed by the ad hoc ansatz S^{tr}=C_n r^n, with n restricted to 1,2,3 and C_n a free parameter per source. No derivation from disk turbulence, vorticity, or clump formation is provided; the labels 'filament-like', 'thin-disk', and 'thick-disk' are interpretive. The claimed 'data select the internal structure' therefore only selects among three imposed power laws, not the structure itself. Since the amplitude C_n is also unconstrained independently, it could absorb part of the frequency shift that RPM-SdS attributes to the effective cosmological constant. To support the central claim, the paper should either derive the power-law profile from a microphysical disk model or compare against alternative profiles and show that the n≈2 clustering is not an artifact of the parametrization.
- [§3, Eq. (30a) and Table B.1] The reported RPM-K best-fit masses are inconsistent with the stated prior. Equation (30a) gives M∈[0,5] M⊙ for the MCMC analysis, yet Table B.1 lists RPM-K best fits of M=5.118, 8.602, 6.352, 5.938, 6.566, and 7.708 M⊙ for Cir X1, GX 17+2, Sco X1, 4U1608–52, 4U1728–34, and 4U0614+091, respectively. Either the prior was not enforced for these runs or the table quotes results obtained with a different pipeline/prior. As printed, this contradicts the claim that all models were analyzed with the same pipeline, and it weakens the argument that RPM-K is rejected because it gives unphysical masses.
minor comments (3)
- [Table B.1] There are typos in the model labels: 'PRM–SdS' should be 'RPM–SdS' in the 4U1728–34 block, and 'MPD-S' should be 'MPM-S' in the same block.
- [§2.2] The sentence 'It easy to prove that all the formulas reduce...' is missing 'is'. More substantively, the Schwarzschild limit should be stated more carefully: the limit g_{tφ}→0 is not the same as a→0 off the equatorial plane, although it is valid for equatorial circular motion.
- [§3] The paper refers to 'Bayesian evidence lnB_i' but reports −ln Lbar in Table B.1. The relationship between the quoted log-likelihood maxima and the evidence differences Δ should be stated explicitly; currently the reader cannot reconstruct Δ from the printed LLH values.
Circularity Check
Partial circularity: RPM-SdS is implemented via the same n=3 spin ansatz, so the 'spin replaces SdS' claim is partly a renaming; the n=2 preference is a genuine fit, but the reported evidence table is internally inconsistent.
specific steps
-
renaming known result
[Sec. 3 (model comparison and statistical criteria); Eq. (20); Table B.1]
"For RPM-SdS we consider an effective n=3 to ensure the correct physical dimensions of the cosmological constant R_0 (Boshkayev et al. 2023b), as discussed in Bianchini et al. (2025). ... accounting for spinning test particles has the net effect to reduce the index n=3 of the effective RPM-SdS model to the mostly preferred n=2 of the MPM-S case."
RPM-SdS is fitted with the same power-law index n=3 of the spin ansatz S^{tr}=C_n r^n (Eq. 20), so its frequency corrections are the n=3 member of the MPM family. The paper's claim that spin replaces the de Sitter phase is therefore a renaming of the fitted parameter (C_3 in place of R_0) in the n=3 cases, not a test of the physical origin. Table B.1 confirms the degeneracy: where MPM-S selects n=3 (GX 5-1, GX 17+2), it is statistically equivalent to RPM-SdS (Δ=0 in both rows).
-
fitted input called prediction
[Abstract and Sec. 3; Eq. (20)]
"We now specify the specific spin tensor, by embedding in it the symmetry of the accretion flow through the ansatz S^{tr}=C_n r^n. ... Regarding the power-law index n, we fix it to the values n={1,2,3} and assess, case by case, the best choice. ... Our statistical analyzes show that the data select the internal structure of the accreting matter."
The 'internal structure' said to be selected by the data is the exponent n of a hand-inserted ansatz, with C_n freely fitted per source. The clustering around n=2 is thus a comparison among three pre-chosen power-law curves, i.e. a fit output, not a derivation of disk structure from the MPD equations. Presenting this as 'the data select the internal structure' elevates the fitted index to a model discovery, though the paper is transparent that n is fixed beforehand.
full rationale
The MPD frequency calculation (Eqs. 1-19 and Appendix A) is self-contained and not circular: the spin corrections are derived from the MPD equations and the stated metric, and the test-particle limit is recovered. The ansatz Eq. (20) is an input, not an output, and fitting C_n is standard. The main partial circularity is the SdS comparison: RPM-SdS is implemented with 'an effective n=3' of the same spin-ansatz family, so the n=3 MPM-S and RPM-SdS are the same functional family; the claim that spin explains SdS is then a reparametrization (C_3 ↔ R_0). This is not a full circularity because six of eight sources prefer n=2, a distinct functional form that outperforms SdS, giving the central claim independent content. I did not count the self-citation to Bianchini et al. (2025) as load-bearing: the MPM-S fits are reproduced in Table B.1 and Fig. B.1 of this paper. Separately, the statistical section contains an internal inconsistency: it defines Δ = lnB_i − lnB_0 with lnB_0 = min{lnB_i}, which would make the best model 'decisively excluded'; Table B.1 uses the opposite convention (best model Δ=0). This undermines the reproducibility of the evidence but is a reporting error, not a circular reduction.
Axiom & Free-Parameter Ledger
free parameters (4)
- C_n (spin amplitude) =
values of order 10^-4 to 10^-3 in km^(1-n), source-dependent (Table B.1)
- n (power-law index) =
discrete: fitted among {1,2,3} (Table B.1)
- M (compact object mass) =
values in [1.1, 2.4] M_⊙ for MPM-S/K, source-dependent (Table B.1)
- j (Kerr spin parameter) =
MPM-K values in [-0.39, 0.44]; RPM-K values sometimes >0.9 (Table B.1)
axioms (4)
- domain assumption Test-body spin is small: κ=|S^0|/(m r) ≪ 1 and the TPA holds (Eq. 2).
- domain assumption The disk clumps move on equatorial circular orbits with spin orthogonal to the orbital plane (ESC, Eq. 7b).
- ad hoc to paper The spin tensor is parametrized as S^{tr}=C_n r^n (Eq. 20).
- domain assumption The lowest-order frequencies are given by the standard RPM identifications: f_L=(Ω_ϕ−Ω_r)/(2π), f_U=Ω_ϕ/(2π) (Eqs. 19, 28).
invented entities (1)
-
Macroscopic disk spin distribution S^{tr}=C_n r^n
no independent evidence
read the original abstract
The relativistic precession model (RPM) interprets the twin kilohertz quasi-periodic oscillations (QPOs) as geodesic frequencies of test particles orbiting in the spacetime of X-ray binaries hosting either a neutron star (NS) or a black hole. In several NS X-ray binaries, QPOs are well reproduced by effective geometries nearly degenerate with a Schwarzschild-de Sitter (SdS) spacetime, hindering independent determinations of the mass, the angular momentum and other observables. We propose how to solve this physical limitation by incorporating the effects of orbiting matter spin, culminating in introducing the macroscopic precession model (MPM). We treat the disk inhomogeneities as spinning test bodies governed by the Mathisson-Papapetrou-Dixon (MPD) equations and obtain non-minimal spin curvature corrections to the azimuthal and the radial epicyclic frequencies. We perform Monte Carlo Markov chain (MCMC) fits, based on the Metropolis algorithm, and model eight NS X-ray binary sources. Our statistical analyzes show that the data select the internal structure of the accreting matter, without requiring corrections to Kerr and Schwarzschild spacetimes through the introduction of any correcting de Sitter phase. Physically, the MPM paradigm explains why an effective SdS-like structure could be statistically favored if spin is not employed, through non-minimal spin-curvature coupling, leaving unaltered the test particle hypothesis.
Reference graph
Works this paper leans on
-
[1]
Ingram, A. R. and Motta, S. E. , title =. New Astronomy Reviews , volume =. 2019 , doi =
2019
-
[2]
McHardy, I. M. and Kording, E. and Knigge, C. and Uttley, P. and Fender, R. P. , title =. Nature , volume =. 2006 , doi =
2006
-
[3]
Motta, S. E. and Mu\ noz-Darias, T. and Sanna, A. and Fender, R. and Belloni, T. and Stella, L. , title =. Mon. Not. R. Astron. Soc. Lett. , volume =. 2014 , doi =
2014
-
[4]
Quasiperiodic oscillations for spherically symmetric regular black holes
Boshkayev, Kuantay and Idrissov, Anuar and Luongo, Orlando and Muccino, Marco. Quasiperiodic oscillations for spherically symmetric regular black holes. Phys. Rev. D. 2023. doi:10.1103/PhysRevD.108.044063. arXiv:2303.03248
Pith/arXiv arXiv 2023
-
[5]
Motta, S. E. and Belloni, T. M. and Stella, L. and Mu\ noz-Darias, T. and Fender, R. , title =. Mon. Not. R. Astron. Soc. , volume =. 2013 , month = nov, doi =
2013
-
[6]
and Idrissov, A
Boshkayev, K. and Idrissov, A. and Luongo, O. and Muccino, M. , title =. Phys. Rev. D , volume =. 2023 , doi =
2023
-
[7]
and Luongo, O
Boshkayev, K. and Luongo, O. and Muccino, M. , title =. Phys. Rev. D , volume =. 2023 , doi =
2023
-
[8]
and Török, G
Bakala, P. and Török, G. and Karas, V. and Dovčiak, M. and Wildner, M. and Wzientek, D. and Šrámková, E. and Abramowicz, M. and Goluchová, K. and Mazur, G. P. and Vincent, F. H. , title =. Mon. Not. R. Astron. Soc. , volume =. 2014 , doi =
2014
-
[9]
and Rahimov, O
Turimov, B. and Rahimov, O. , title =. Universe , volume =. 2022 , doi =
2022
-
[10]
and Nampalliwar, S
Bambi, C. and Nampalliwar, S. , title =. EPL (Europhysics Letters) , volume =. 2016 , doi =
2016
-
[11]
Loomis, S. P. and Brown, J. D. , title =. Phys. Rev. D , volume =. 2017 , doi =
2017
-
[12]
Plyatsko, R. M. and Stefanyshyn, O. B. and Fenyk, M. T. , title =. Classical and Quantum Gravity , volume =. 2011 , month = sep, doi =
2011
-
[13]
and Fenyk, M
Plyatsko, R. and Fenyk, M. , title =. Phys. Rev. D , volume =. 2012 , month = may, doi =
2012
-
[14]
, title =
Lukes-Gerakopoulos, G. , title =. Phys. Rev. D , volume =. 2017 , month = nov, doi =
2017
-
[15]
and Geralico, A
Bini, D. and Geralico, A. and Vines, J. , title =. Phys. Rev. D , volume =. 2017 , month = oct, doi =
2017
-
[16]
Santos, E. B. and Batista, C. , title =. Phys. Rev. D , volume =. 2020 , month = may, doi =
2020
-
[17]
Giamb \`o , Roberto and Luongo, Orlando and Muccino, Marco and Rossi, Alessandro. Generalizing the relativistic precession model of quasi-periodic oscillations through anharmonic corrections. JCAP. 2026. doi:10.1088/1475-7516/2026/05/026. arXiv:2504.18403
Pith/arXiv arXiv 2026
-
[18]
and Abramowicz, M
Török, G. and Abramowicz, M. A. and Kluźniak, W. and Stuchlík, Z. , title =. Astron. Astrophys. , volume =. 2005 , doi =
2005
-
[19]
Information criteria for astrophysical model selection. MNRAS , keywords =. doi:10.1111/j.1745-3933.2007.00306.x , archivePrefix =. astro-ph/0701113 , primaryClass =
arXiv 2007
-
[20]
Measuring the effective complexity of cosmological models
Kunz, Martin and Trotta, Roberto and Parkinson, David. Measuring the effective complexity of cosmological models. Phys. Rev. D. 2006. doi:10.1103/PhysRevD.74.023503. arXiv:astro-ph/0602378
Pith/arXiv arXiv 2006
-
[21]
Bulletin of the Astronomical Society of India , year = 2002, month = sep, volume =
The maximum mass of neutron stars. Bulletin of the Astronomical Society of India , year = 2002, month = sep, volume =
2002
-
[22]
Extended Bodies in General Relativity: Their Description and Motion
Dixon, W. Extended Bodies in General Relativity: Their Description and Motion. Isolated Gravitating Systems in General Relativity. 1979
1979
-
[23]
Velandia-Heredia, Nelson and Tejeiro-Sarmiento, Juan Manuel. Numerical solution of Mathisson-Papapetrou-Dixon equations for spinning test particles in a Kerr metric. 2017. doi:10.15446/mo.n57.73391. arXiv:1712.01404
Pith/arXiv arXiv 2017
-
[24]
Black hole spin measurements through the relativistic precession model: XTE J1550-564. , keywords =. doi:10.1093/mnrasl/slt181 , archivePrefix =. 1312.3114 , primaryClass =
-
[25]
Precise mass and spin measurements for a stellar-mass black hole through X-ray timing: the case of GRO J1655-40. , keywords =. doi:10.1093/mnras/stt2068 , archivePrefix =. 1309.3652 , primaryClass =
-
[26]
, title =
van der Klis, M. , title =. Adv. Space Res. , volume =. 2006 , month = dec, doi =
2006
-
[27]
and van der Klis, M
Hasinger, G. and van der Klis, M. , title =. Astron. Astrophys. , volume =
-
[28]
Shirey, R. E. and Bradt, H. V. and Levine, A. M. and Morgan, E. H. , title =. Astrophys. J. , volume =. 1998 , month = oct, doi =
1998
-
[29]
and Ford, E
van Straaten, S. and Ford, E. C. and van der Klis, M. and Méndez, M. and Kaaret, P. , title =. Astrophys. J. , volume =. 2000 , month = sep, doi =
2000
-
[31]
Twin Peaks kHz QPOs: Mathematics of the 3:2 Orbital Resonance. , keywords =. doi:10.1093/pasj/56.3.553 , archivePrefix =. astro-ph/0403341 , primaryClass =
-
[32]
The Importance of Discovering a 3:2 Twin-Peak Quasi-periodic Oscillation in an Ultraluminous X-Ray Source, or How to Solve the Puzzle of Intermediate-Mass Black Holes. , keywords =. doi:10.1086/422810 , archivePrefix =. astro-ph/0402012 , primaryClass =
-
[33]
Mass-Angular-momentum Relations Implied by Models of Twin Peak Quasi-periodic Oscillations. , keywords =. doi:10.1088/0004-637X/760/2/138 , archivePrefix =. 1408.4220 , primaryClass =
-
[34]
Lamb, Frederick K. and Boutloukos, Stratos. Accreting Neutron Stars in Low-Mass X-Ray Binary Systems. Short-Period Binary Stars: Observations, Analyses, and Results. 2008. doi:10.1007/978-1-4020-6544-6_5
-
[35]
kHz Quasiperiodic Oscillations in Low-Mass X-Ray Binaries as Probes of General Relativity in the Strong-Field Regime. , keywords =. doi:10.1103/PhysRevLett.82.17 , archivePrefix =. astro-ph/9812124 , primaryClass =
-
[36]
Living Reviews in Relativity , volume=
The motion of point particles in curved spacetime , author=. Living Reviews in Relativity , volume=. 2011 , eprint=
2011
-
[37]
An axiomatic approach to electromagnetic and gravitational radiation reaction of particles in curved spacetime , author=. Phys. Rev. D , volume=. 1997 , eprint=
1997
-
[38]
Self-force via a Green's function decomposition , author=. Phys. Rev. D , volume=. 2003 , eprint=
2003
-
[39]
Gravitational radiation reaction to a particle motion
Mino, Yasushi and Sasaki, Misao and Tanaka, Takahiro. Gravitational radiation reaction to a particle motion. Phys. Rev. D. 1997. doi:10.1103/PhysRevD.55.3457. arXiv:gr-qc/9606018
Pith/arXiv arXiv 1997
-
[40]
Axiomatic approach to radiation reaction of scalar point particles in curved space-time
Quinn, Theodore C. Axiomatic approach to radiation reaction of scalar point particles in curved space-time. Phys. Rev. D. 2000. doi:10.1103/PhysRevD.62.064029. arXiv:gr-qc/0005030
Pith/arXiv arXiv 2000
-
[41]
Mazur, Pawel O. and Mottola, Emil. Gravitational vacuum condensate stars. Proc. Nat. Acad. Sci. 2004. doi:10.1073/pnas.0402717101. arXiv:gr-qc/0407075
Pith/arXiv arXiv 2004
-
[42]
Black hole mimickers: from theory to observation
Bambi, Cosimo and others. Black hole mimickers: from theory to observation. 2025. arXiv:2505.09014
Pith/arXiv arXiv 2025
-
[43]
Semi-classical dust collapse and regular black holes
Malafarina, Daniele. Semi-classical dust collapse and regular black holes. 2022. arXiv:2209.11406
Pith/arXiv arXiv 2022
-
[44]
Negative refraction from optical properties of spacetime media
Luongo, Orlando. Negative refraction from optical properties of spacetime media. Class. Quant. Grav. 2025. doi:10.1088/1361-6382/ae187f. arXiv:2504.09987
arXiv 2025
-
[45]
Belloni, T. M. and Stella, L. , title =. Space Sci. Rev. , volume =. 2014 , month = aug, doi =. 1407.7373 , archivePrefix =
Pith/arXiv arXiv 2014
-
[46]
, title =
Wang, J. , title =. Int. J. Astron. Astrophys. , volume =. 2016 , month = jan, doi =
2016
-
[47]
Swank, J. , title =. AIP Conf. Proc. , volume =. 2004 , doi =. astro-ph/0402511 , archivePrefix =
Pith/arXiv arXiv 2004
-
[48]
Lewin, W. H. G. and van Paradijs, J. and van der Klis, M. , title =. Space Sci. Rev. , volume =. 1988 , month = sep, doi =
1988
-
[49]
van der Klis, M. , title =. Astronomical Time Series , publisher=. 1997 , doi =. astro-ph/9710016 , archivePrefix =
Pith/arXiv arXiv 1997
-
[50]
Smith, K. L. and Tandon, C. R. and Wagoner, R. V. , title =. Astrophys. J. , volume =. 2021 , month = jan, doi =. 2011.05346 , archivePrefix =
Pith/arXiv arXiv 2021
-
[51]
Belloni, T. M. , title =. The Jet Paradigm , pages =. 2009 , month = oct, publisher =. doi:10.1007/978-3-540-76937-8_3 , url =. 0909.2474 , archivePrefix =
Pith/arXiv arXiv 2009
-
[52]
Done, C. and Gierliński, M. and Kubota, A. , title =. Astron. Astrophys. Rev. , volume =. 2007 , month = aug, publisher =. doi:10.1007/s00159-007-0006-1 , url =. 0708.0148 , archivePrefix =
Pith/arXiv arXiv 2007
-
[53]
, title =
van der Klis, M. , title =. Annu. Rev. Astron. Astrophys. , volume =. 1989 , month = nov, doi =
1989
-
[54]
, title =
Tagger, M. , title =. Revista Mexicana de Astronomia y Astrofisica, Volume 27 , series =. 2007 , month = mar, adsurl =
2007
-
[55]
The Motion of point particles in curved spacetime
Poisson, Eric and Pound, Adam and Vega, Ian. The Motion of point particles in curved spacetime. Living Rev. Rel. 2011. doi:10.12942/lrr-2011-7. arXiv:1102.0529
Pith/arXiv arXiv 2011
-
[56]
Costa, L. Filipe O. and Lukes-Gerakopoulos, Georgios and Semer \'a k, Old r ich. Spinning particles in general relativity: Momentum-velocity relation for the Mathisson-Pirani spin condition. Phys. Rev. D. 2018. doi:10.1103/PhysRevD.97.084023. arXiv:1712.07281
Pith/arXiv arXiv 2018
-
[57]
Boutloukos, Stratos and van der Klis, M. and Altamirano, D. and Klein-Wolt, M. and Wijnands, R. and Jonker, P. G. and Fender, R. P. Discovery of twin kHz QPOs in the peculiar X-ray binary Circinus X-1. Astrophys. J. 2006. doi:10.1086/518858. arXiv:astro-ph/0608089
Pith/arXiv arXiv 2006
-
[58]
Cherepashchuk, A. M. and Khruzina, T. S. and Bogomazov, A. I. Parameters of the X-ray binary system Scorpius X-1. Mon. Not. Roy. Astron. Soc. 2021. doi:10.1093/mnras/stab2515. arXiv:2109.00967
Pith/arXiv arXiv 2021
-
[59]
The Distance, Mass, and Radius of the Neutron Star in 4U 1608-52
Guver, Tolga and Ozel, Feryal and Cabrera-Lavers, Antonio and Wroblewski, Patricia. The Distance, Mass, and Radius of the Neutron Star in 4U 1608-52. Astrophys. J. 2010. doi:10.1088/0004-637X/712/2/964. arXiv:0811.3979
Pith/arXiv arXiv 2010
-
[60]
The bursting behavior of 4u 1728-34: parameters of a neutron star and geometry of a ns-disk system
Shaposhnikov, Nickolai and Titarchuk, Lev and Haberl, Frank. The bursting behavior of 4u 1728-34: parameters of a neutron star and geometry of a ns-disk system. Astrophys. J. Lett. 2003. doi:10.1086/378255. arXiv:astro-ph/0307215
Pith/arXiv arXiv 2003
-
[61]
The highest-frequency kHz QPOs in neutron star low mass X-ray binaries
van Doesburgh, Marieke and van der Klis, Michiel and Morsink, Sharon. The highest-frequency kHz QPOs in neutron star low mass X-ray binaries. Mon. Not. Roy. Astron. Soc. 2018. doi:10.1093/mnras/sty1404. arXiv:1805.11361
Pith/arXiv arXiv 2018
-
[62]
Bianchini, Gabriele and Luongo, Orlando and Muccino, Marco. The macroscopic precession model: describing quasi-periodic oscillations including internal structures of test bodies. submitted to PRD. 2025. arXiv:2512.12242
arXiv 2025
-
[63]
Quasi-periodic oscillations in rotating and deformed space-times. , keywords =. doi:10.1093/mnras/stae1388 , archivePrefix =. 2312.03630 , primaryClass =
-
[64]
The Spin Parameter of Uniformly Rotating Compact Stars. , keywords =. doi:10.1088/0004-637X/728/1/12 , archivePrefix =. 1011.3563 , primaryClass =
-
[65]
Contemporary Physics , keywords =
Bayes in the sky: Bayesian inference and model selection in cosmology. Contemporary Physics , keywords =. doi:10.1080/00107510802066753 , archivePrefix =. 0803.4089 , primaryClass =
-
[66]
Lense-Thirring Precession and Quasi-periodic Oscillations in Low-Mass X-Ray Binaries. , keywords =. doi:10.1086/311075 , archivePrefix =. astro-ph/9709085 , primaryClass =
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