REVIEW 3 major objections 4 minor 90 references
A portable AI skill lets a general LLM agent read a nuclear model, fit its couplings, and report neutron-star and nuclear-matter observables without human intervention.
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
2026-08-02 03:16 UTC pith:VIXAULM7
load-bearing objection A genuinely useful agent-skill for RMF-to-neutron-star work, but the autonomous-fit demo returns an unstable Lagrangian and the benchmark overclaims. the 3 major comments →
NNStar: An end-to-end AI agent for nuclear matter and neutron star physics
The pith
A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.
Core claim
On the paper's own terms, the core claim is that a deterministic, model-agnostic physics stack—not the language model's parametric memory—can carry the entire forward-and-inference pipeline, and that packaging this stack as a platform-agnostic skill makes the capability transferable across any sufficiently capable LLM agent. A user makes a natural-language request; the agent reads the skill specification, invokes the bundled code for each step, and returns saturation properties, mass-radius curves, and statistical scores. The skill reproduces three established relativistic mean-field models' published saturation properties and mass-radius behavior to rounding level, and when the agent extend
What carries the argument
The central object is the NNStar skill itself: a self-contained module that pairs a specification file with executable physics code, exposing a layered forward pipeline. The pipeline starts from a general quantum hadrodynamical Lagrangian, symbolically derives the relativistic mean-field equations of motion, numerically solves for the meson fields and saturation properties, constructs beta-equilibrium matter (the charge-neutral composition reached by weak interactions), splices the high-density equation of state onto a low-density crust, integrates the Tolman–Oppenheimer–Volkoff equations for masses, radii, and tidal deformability, and scores the model through a Bayesian joint analysis again
Load-bearing premise
The load-bearing premise is that the skill's bundled physics code—the symbolic derivation, mean-field solver, crust matching, and TOV integration—faithfully implements the standard physics; if a latent bug or approximation error sits in that stack, every agent output inherits it, and the validation's main comparison is to a companion paper sharing the skill's code lineage rather than to fully independent implementations.
What would settle it
Recompute the saturation properties and mass-radius curves of the three established models with an independently written solver using the original publications' full-precision couplings, and compare point by point with the skill's Table I; a discrepancy in the incompressibility beyond the stated rounding (~7%) or a radius shift larger than ~0.1 km would show the skill's physics stack is not faithful, and with it every downstream agent result.
If this is right
- A researcher can hand the agent a published Lagrangian and receive its nuclear-matter properties, mass-radius curve, and fit quality without writing pipeline code.
- Because the capability travels as a skill, different LLM agents can load the same physics backend, making the physics independent of the reasoning model.
- Extending the physics—new interaction terms, new constraints, new observables—is a matter of editing a declarative model definition and the tool catalog, not rewriting the agent.
- Since outputs come from deterministic code, results are auditable and reproducible, and the benchmark against deterministic ground truth can be rerun for any future LLM.
- The demonstrated workflow of adding an interaction and re-optimizing can be repeated for other model extensions, including chiral effective models, hyperons, or quark degrees of freedom.
Where Pith is reading between the lines
- If such a skill becomes widely used, the practical bottleneck in dense-matter equation-of-state inference shifts from numerical implementation to model choice and interpretation; different groups' fits would share one pipeline, making disagreements traceable to physics rather than code.
- The same 'portable skill' pattern should transfer to other inference problems with a deterministic forward map and a likelihood, such as chiral effective field theory fits or gravitational-wave parameter estimation; the paper does not claim this generality.
- The validation relies most heavily on a companion paper that shares code lineage with the skill, so the strongest independent test would be reproducing the original model papers directly from their full-precision parameter tables; the paper reports agreement but does not present that comparison.
- The remaining radius tension in the sextic-augmented fit suggests an immediate testable extension the paper does not run: equipping the agent with a richer isovector sector and checking whether the agent can bring the 1.4-solar-mass radius into the observed range while keeping the maximum mass above two solar masses.
Editorial analysis
A structured set of objections, weighed in public.
Referee Report
Summary. The paper introduces NNStar, a portable LLM-agent 'skill' for automating relativistic mean-field (RMF) modeling of nuclear matter and neutron stars. The skill is designed to (i) construct an RMF model from a Lagrangian, (ii) symbolically derive and solve the mean-field equations, (iii) compute saturation properties, (iv) build a beta-equilibrium EoS, splice on the BPS crust, integrate the TOV equations, and (v) score the model via a Bayesian joint analysis. The authors validate the skill on TM1, NL3, and FSU-delta6.7, demonstrate an autonomous fit of a sigma^6-extended TM1 model, and benchmark six LLMs with and without the skill. The central claim is that the agent can read, fit, and report nuclear-matter and neutron-star observables end-to-end without human intervention.
Significance. If the pipeline is correct, the skill-based architecture is a genuinely useful contribution: it provides a deterministic, auditable physics backend that can be loaded by any compliant LLM agent, and the public code/data availability supports reproducibility. The derivation of the BJA-to-chi^2 equivalence in App. A is correct, and the separation of LLM planning from deterministic physics execution is a sensible design. However, the load-bearing demonstrations currently have weaknesses: the validation relies on a same-author reference rather than independent published values, the benchmark defines ground truth as the tool stack's own output, and the only autonomous fitting example returns a scalar potential that is unbounded below. These issues must be addressed before the end-to-end claim is fully supported.
major comments (3)
- [Sec. VI.B, Eq. (8) and Eq. (2)] The optimized Lagrangian is obtained by adding -g_s6 sigma^6/6 to TM1, and the agent reports g_s6 = -2.9e-4 MeV^-2. With the sign convention of Eq. (2), the scalar potential contains +(1/6)g_s6 sigma^6, so V(sigma) -> -infinity as |sigma| -> infinity. The optimization objective (8) has no stability constraint, and the skill does not check or flag this. The agent nevertheless reports chi^2=7.2, M_max=2.11 M_sun, R_1.4=14.3 km and describes only the radius as a limitation. Since this is the only autonomous fitting demonstration, the claim that the agent operates 'without human intervention' is not supported: a human must audit the physicality of the fitted Lagrangian. Add a vacuum-stability check (e.g., require the potential to be bounded below with a positive highest-order coefficient) to the skill and re-run the example; if the optimum remains unphysical, the sigma^6 extension should be
- [Sec. VI.A, Table I and Sec. VII.A] The validation compares the skill's output with 'Ref.' values taken from Ref. [64], which is a same-author paper (Y. Ma, Y.-L. Ma, J.-Y. Xiong, arXiv:2603.01933), not the original publications for TM1, NL3, and FSU-delta6.7. The benchmark in Sec. VII.A then defines deterministic ground truth as 'computed by the tool stack itself.' Thus the evidence that the deterministic physics stack is correct is largely internal consistency; a systematic error shared with Ref. [64] would not be detected. Please compare against the original published saturation properties and M-R curves (or an independent code), and clarify that Table I is a comparison to a same-author reference rather than to the original model papers.
- [Sec. VII.B, Tables III and IV] The text states that the skill-equipped mode is 'uniformly improved' and that grounding makes the computation 'deterministic ... largely independent of the underlying model.' The data do not fully support this. Kimi-K2.6 with the skill has 2/3 valid runs with mean errors of roughly 101% in matter, 80% in M, and 75% in R; the per-run table shows outputs that are far from the reference values (e.g., Kimi run 16). Qwen3.7-Max has only 2/3 valid runs. The benchmark is explicitly proof-of-concept, but the conclusions should be qualified to reflect that cross-model determinism is not demonstrated, especially for the weaker LLMs.
minor comments (4)
- [Sec. VI.B] The text says 'all seven couplings ... are freed' but then lists eight parameters: g_sigma, g_omega, g_rho, g_s3, g_s4, c_3, g_s6, and m_sigma. Fix the count.
- [Sec. VI.B vs. App. A] The optimization protocol states that minimizing chi^2 is 'identical, up to an additive constant, to the BJA log-likelihood of Eq. (A4).' The explicit equivalence is actually Eq. (A5); update the cross-reference.
- [Sec. VII.A] The phrase 'six observables of Sec. III' is inaccurate: Sec. III defines the model, not the observables. The six observables are enumerated in Sec. VII.A itself. Reword to avoid the incorrect cross-reference.
- [Sec. IV.C and Sec. VI.A] The skill is said to support 'import a model directly from the literature' (e.g., from a PDF), but the validation in Sec. VI.A appears to use built-in parameterizations. Clarify whether the PDF-reading capability was exercised, and if not, state that it remains to be validated.
Circularity Check
Benchmark ground truth is the tool stack's own output and Table I validates against the same authors' Ref. [64]; the central RMF/TOV/BJA derivation remains standard and externally checkable.
specific steps
-
self definitional
[Sec. VII.A (Benchmarks, Task suite and metrics)]
"dense-matter physics admits a deterministic ground truth: the correct value of any NM or NS observable for a given Lagrangian is fixed by the field equations and computed by the tool stack itself. This allows us to score the agent against exact references rather than human judgment"
The benchmark's 'exact reference' is defined as the output of the very tool stack the agent is being tested on. A skill-equipped agent that successfully invokes the bundled code returns exactly that reference by construction, so the near-zero errors in Table III demonstrate tool invocation, not independent physical correctness. The NM/NS observables treated as predictions are definitionally equal to the tool's own computation, so this protocol cannot validate the skill; it only checks whether the LLM calls the tool.
-
self citation load bearing
[Sec. VI.A (Validation on Walecka-type models), Table I]
"Table I compares the saturation properties recovered by the skill with the values obtained in Ref. [64]."
Ref. [64] is the authors' own preceding paper by Y. Ma, Y.-L. Ma, and J.-Y. Xiong. The validation's 'published values' are therefore same-author outputs, not the original independent TM1/NL3/FSU publications cited as [65]-[67]. The end-to-end correctness claim reduces to agreement with a same-lineage reference; the table never compares directly against the external original values. Because the underlying mean-field and TOV equations are standard physics, this is load-bearing self-citation rather than full definitional circularity, but it does not constitute independent confirmation.
full rationale
The central physics derivation — symbolic construction of mean-field EOMs from the Lagrangian, RMF solution, beta-equilibrium EoS, crust matching, TOV integration, and Bayesian joint analysis — is standard, self-contained, and not circular. Eq. (A5) explicitly identifies BJA with -1/2 chi^2 + C, an algebraic identity rather than a hidden fitted-input-as-prediction. The main circularity concerns are in the validation/support structure. First, Sec. VII.A defines the benchmark ground truth as the output of the tool stack itself, making a successfully tool-invoking agent's agreement with that reference tautological. Second, Sec. VI.A validates the skill against Ref. [64], the same authors' prior paper, rather than against the original TM1/NL3/FSU publications; the external papers are cited but do not supply the table's 'Ref.' values. The original Walecka-type models do provide independent anchors for the physics, and the equations of state are externally checkable, so the central workflow retains real content. However, the paper's evidence for 'validated end-to-end' operation relies on these two self-referential supports, giving partial circularity in the demonstration rather than in the physics itself. No uniqueness theorem, hidden ansatz, or renamed empirical result was found.
Axiom & Free-Parameter Ledger
free parameters (8)
- mσ =
492.4 MeV
- gσ =
-9.93
- gω =
12.86
- gρ =
3.89
- gs3 =
1743
- gs4 =
-0.62
- c3 =
107.6
- gs6 =
-2.9e-4 MeV^-2
axioms (8)
- domain assumption Mean-field (Hartree) approximation for the RMF model: meson fields replaced by their expectation values; Fock terms neglected.
- standard math TOV equations describe hydrostatic equilibrium of static neutron stars in general relativity.
- domain assumption BPS crust matched to the core at n_b = 0.08 fm^-3.
- domain assumption β-equilibrium and charge neutrality in the stellar interior.
- domain assumption Uniform priors within allowed parameter ranges in the Bayesian analysis.
- ad hoc to paper The GQHD Lagrangian (Eq. 2) is general enough to contain TM1, NL3, and FSU as special cases.
- ad hoc to paper Benchmark ground truth is defined as the output of the tool stack itself, not an external measurement.
- domain assumption The empirical constraints in Eq. (8) are imposed at 1σ and represent the complete dataset for the σ6 fit.
read the original abstract
Constraining the equation of state of dense matter requires confronting effective models with massive data that spans many orders of magnitude in scale, from sub-saturation nuclear matter properties to the masses, radii, and tidal deformabilities of neutron stars. Exploring the high-dimensional coupling space of such a model and fine tuning it against all of these constraints is a labor- and time-intensive task. We present \textsc{NNStar}, an end-to-end artificial-intelligence agent that automates this workflow. Rather than a bespoke application, \textsc{NNStar} is delivered as a portable \emph{skill} for an open large-language-model (LLM) agent platform -- a self-describing module that pairs worked usage conventions with symbolic and numerical physics engines that (i) build a relativistic mean-field model directly from a Lagrangian, (ii) solve the mean-field equations of motion and evaluate the saturation properties, (iii) construct the $\beta$-equilibrium equation of state, splice it to a crust, and integrate the Tolman--Oppenheimer--Volkoff equations, and (iv) score the resulting predictions through a Bayesian joint analysis against nuclear matter and astrophysical observations. The agent can read a model, fit its parameters, and report the full set of nuclear matter and neutron star observables without human intervention. \textsc{NNStar} therefore provides a new, AI-driven framework for analyzing nuclear matter and neutron-star observations.
Figures
Reference graph
Works this paper leans on
-
[1]
K. Fukushima and C. Sasaki, Prog. Part. Nucl. Phys.72, 99 (2013), arXiv:1301.6377 [hep-ph]
Pith/arXiv arXiv 2013
-
[2]
J. W. Holt, M. Rho, and W. Weise, Phys. Rept.621, 2 (2016), arXiv:1411.6681 [nucl-th]
Pith/arXiv arXiv 2016
-
[3]
G. Baym, T. Hatsuda, T. Kojo, P. D. Powell, Y. Song, and T. Takatsuka, Rept. Prog. Phys.81, 056902 (2018), arXiv:1707.04966 [astro-ph.HE]
Pith/arXiv arXiv 2018
-
[4]
Y.-L. Ma and M. Rho, Prog. Part. Nucl. Phys.113, 103791 (2020), arXiv:1909.05889 [nucl-th]
Pith/arXiv arXiv 2020
-
[5]
G. F. Burgio, H. J. Schulze, I. Vidana, and J. B. Wei, Prog. Part. Nucl. Phys.120, 103879 (2021), arXiv:2105.03747 [nucl-th]
Pith/arXiv arXiv 2021
-
[6]
Y.-L. Ma and M. Rho, AAPPS Bull.31, 16 (2021), arXiv:2103.00744 [nucl-th]
Pith/arXiv arXiv 2021
-
[7]
L. Brandes and W. Weise, Symmetry16, 111 (2024), arXiv:2312.11937 [nucl-th]
Pith/arXiv arXiv 2024
-
[8]
A. P. Gupta, Int. J. Sci. Res. Eng. Mgmt10, 1 (2026)
2026
-
[9]
Demorest, T
P. Demorest, T. Pennucci, S. Ransom, M. Roberts, and J. Hessels, Nature467, 1081 (2010)
2010
-
[10]
Antoniadiset al., Science340, 6131 (2013)
J. Antoniadiset al., Science340, 6131 (2013)
2013
-
[11]
Fonsecaet al., Astrophys
E. Fonsecaet al., Astrophys. J. Lett.915, L12 (2021)
2021
-
[12]
B. P. Abbottet al.(LIGO Scientific, Virgo), Phys. Rev. Lett.119, 161101 (2017)
2017
-
[13]
B. P. Abbottet al.(LIGO Scientific, Virgo), Phys. Rev. Lett.121, 161101 (2018)
2018
-
[14]
S. Vinciguerraet al., Astrophys. J.961, 62 (2024), arXiv:2308.09469 [astro-ph.HE]
Pith/arXiv arXiv 2024
-
[15]
T. Salmiet al., Astrophys. J.974, 294 (2024), arXiv:2406.14466 [astro-ph.HE]
Pith/arXiv arXiv 2024
-
[16]
D. Choudhuryet al., Astrophys. J. Lett.971, L20 (2024), arXiv:2407.06789 [astro-ph.HE]
Pith/arXiv arXiv 2024
-
[17]
A NICER view of the 1.4 solar-mass edge-on pulsar PSR J0614–3329,
L. Mauviardet al., “A NICER view of the 1.4 solar-mass edge-on pulsar PSR J0614–3329,” (2025), arXiv:2506.14883 [astro-ph.HE]
arXiv 2025
-
[18]
M. Dutra, O. Louren¸ co, S. S. Avancini, B. V. Carlson, A. Delfino, D. P. Menezes, C. Providˆ encia, S. Typel, and J. R. Stone, Phys. Rev. C90, 055203 (2014), arXiv:1405.3633 [nucl-th]
Pith/arXiv arXiv 2014
-
[19]
J. M. Lattimer and Y. Lim, The Astrophysical Journal 771, 51 (2013)
2013
-
[20]
P. Danielewicz and J. Lee, Nucl. Phys. A922, 1 (2014), arXiv:1307.4130 [nucl-th]
Pith/arXiv arXiv 2014
-
[21]
A. Le F` evre, Y. Leifels, W. Reisdorf, J. Aichelin, and C. Hartnack, Nucl. Phys. A945, 112 (2016), arXiv:1501.05246 [nucl-ex]
Pith/arXiv arXiv 2016
-
[22]
B. A. Brown, Phys. Rev. Lett.111, 232502 (2013), arXiv:1308.3664 [nucl-th]
Pith/arXiv arXiv 2013
-
[23]
B. T. Reed, F. J. Fattoyev, C. J. Horowitz, and J. Piekarewicz, Phys. Rev. Lett.126, 172503 (2021), arXiv:2101.03193 [nucl-th]
Pith/arXiv arXiv 2021
-
[24]
Vaswani, Advances in Neural Information Processing Systems (2017)
A. Vaswani, Advances in Neural Information Processing Systems (2017)
2017
-
[25]
Radovic, M
A. Radovic, M. Williams, D. Rousseau, M. Kagan, D. Bonacorsi, A. Himmel, A. Aurisano, K. Terao, and T. Wongjirad, Nature560, 41 (2018)
2018
-
[26]
G. Carleo, I. Cirac, K. Cranmer, L. Daudet, M. Schuld, N. Tishby, L. Vogt-Maranto, and L. Zdeborov´ a, Rev. Mod. Phys.91, 045002 (2019), arXiv:1903.10563 [physics.comp-ph]
Pith/arXiv arXiv 2019
-
[27]
Goodfellow, J
I. Goodfellow, J. Pouget-Abadie, M. Mirza, B. Xu, D. Warde-Farley, S. Ozair, A. Courville, and Y. Ben- gio, Communications of the ACM63, 139 (2020)
2020
-
[28]
Boehnleinet al., Rev
A. Boehnleinet al., Rev. Mod. Phys.94, 031003 (2022)
2022
-
[29]
K. Zhou, L. Wang, L.-G. Pang, and S. Shi, Prog. Part. Nucl. Phys.135, 104084 (2024), arXiv:2303.15136 [hep- ph]
Pith/arXiv arXiv 2024
-
[30]
Y. Fujimoto, K. Fukushima, and K. Murase, Phys. Rev. D101, 054016 (2020), arXiv:1903.03400 [nucl-th]
Pith/arXiv arXiv 2020
-
[31]
R. Wang, Y.-G. Ma, R. Wada, L.-W. Chen, W.-B. He, H.-L. Liu, and K.-J. Sun, Phys. Rev. Res.2, 043202 (2020), arXiv:2010.15043 [nucl-th]
Pith/arXiv arXiv 2020
-
[32]
F. Morawski and M. Bejger, Astron. Astrophys.642, A78 (2020), arXiv:2006.07194 [astro-ph.HE]
Pith/arXiv arXiv 2020
-
[33]
M. U. Anil, K. Banerjee, T. Malik, and C. Providˆ encia, JCAP01, 045 (2022), arXiv:2004.14196 [physics.comp- ph]
Pith/arXiv arXiv 2022
-
[34]
X. H. Wu, Z. X. Ren, and P. W. Zhao, Phys. Rev. C 105, L031303 (2022), arXiv:2105.07696 [nucl-th]
Pith/arXiv arXiv 2022
-
[35]
M.-Z. Han, J.-L. Jiang, S.-P. Tang, and Y.-Z. Fan, As- trophys. J.919, 11 (2021), arXiv:2103.05408 [hep-ph]
Pith/arXiv arXiv 2021
-
[36]
Y. Fujimoto, K. Fukushima, L. D. McLerran, and M. Praszalowicz, Phys. Rev. Lett.129, 252702 (2022), arXiv:2207.06753 [nucl-th]
Pith/arXiv arXiv 2022
-
[37]
S. Soma, L. Wang, S. Shi, H. St¨ ocker, and K. Zhou, JCAP08, 071 (2022), arXiv:2201.01756 [hep-ph]
Pith/arXiv arXiv 2022
-
[38]
M. Omana Kuttan, J. Steinheimer, K. Zhou, and H. Stoecker, Phys. Rev. Lett.131, 202303 (2023), arXiv:2211.11670 [hep-ph]
Pith/arXiv arXiv 2023
-
[39]
W. He, Q. Li, Y. Ma, Z. Niu, J. Pei, and Y. Zhang, Sci. China Phys. Mech. Astron.66, 282001 (2023), arXiv:2301.06396 [nucl-th]
Pith/arXiv arXiv 2023
-
[40]
L.-J. Guo, J.-Y. Xiong, Y. Ma, and Y.-L. Ma, Astrophys. J.965, 47 (2024), arXiv:2309.11227 [nucl-th]
Pith/arXiv arXiv 2024
-
[41]
S. Chatterjee, H. Sudhakaran, and R. Mallick, Eur. Phys. J. C84, 1291 (2024), arXiv:2302.13648 [astro-ph.HE]
Pith/arXiv arXiv 2024
-
[42]
W.-B. He, Y.-G. Ma, L.-G. Pang, H.-C. Song, and K. Zhou, Nucl. Sci. Tech.34, 88 (2023), arXiv:2303.06752 [hep-ph]
Pith/arXiv arXiv 2023
-
[43]
L.-J. Guo, Y. Ma, Y.-L. Ma, R.-X. Wu, and Y.-L. Wu, (2024), arXiv:2410.06088 [nucl-th]
Pith/arXiv arXiv 2024
-
[44]
E. Y¨ uksel, D. Soydaner, and H. Bahtiyar, Phys. Rev. C 109, 064322 (2024), arXiv:2401.02824 [nucl-th]
Pith/arXiv arXiv 2024
-
[45]
G. Ventagli and I. D. Saltas, JCAP01, 073 (2025), arXiv:2405.17908 [astro-ph.HE]
Pith/arXiv arXiv 2025
-
[46]
M. Ferreira and M. Bejger, Phys. Rev. D111, 023035 (2025), arXiv:2403.14266 [nucl-th]
Pith/arXiv arXiv 2025
-
[47]
W. Zhou, H. Shen, J. Hu, and Y. Zhang, Phys. Rev. D 110, 043017 (2024), arXiv:2407.11447 [nucl-th]
Pith/arXiv arXiv 2024
-
[48]
N. K. Patra, T. Malik, H. Pais, K. Zhou, B. K. Agrawal, and C. Providˆ encia, Phys. Lett. B865, 139470 (2025), arXiv:2502.20226 [nucl-th]
Pith/arXiv arXiv 2025
-
[49]
K. Kovlakas, D. De Grandis, and N. Rea, Astron. Astro- phys.701, A267 (2025), arXiv:2509.03090 [astro-ph.HE]
Pith/arXiv arXiv 2025
-
[50]
W. Liu, L. Wang, and Z. Zhu, (2026), arXiv:2604.05428 [astro-ph.HE]
Pith/arXiv arXiv 2026
-
[51]
J. D. Baker, C. A. Bertulani, and R. V. Lobato, (2026), arXiv:2604.24949 [astro-ph.HE]
Pith/arXiv arXiv 2026
-
[52]
G. Bezerra, V. Dexheimer, and R. Negreiros, (2026), arXiv:2605.31198 [astro-ph.HE]
Pith/arXiv arXiv 2026
-
[53]
S. Yao, J. Zhao, D. Yu, N. Du, I. Shafran, K. Narasimhan, and Y. Cao, (2022), arXiv:2210.03629 [cs.CL]
Pith/arXiv arXiv 2022
-
[54]
T. Schick, J. Dwivedi-Yu, R. Dess ` ı, R. Raileanu, 14 M. Lomeli, L. Zettlemoyer, N. Cancedda, and T. Scialom, (2023), arXiv:2302.04761 [cs.CL]
Pith/arXiv arXiv 2023
- [55]
-
[56]
A. M. Bran, S. Cox, O. Schilter, C. Baldassari, A. D. White, and P. Schwaller, Nature Mach. Intell.6, 525 (2024), arXiv:2304.05376 [physics.chem-ph]
Pith/arXiv arXiv 2024
-
[57]
D. A. Boiko, R. MacKnight, B. Kline, and G. Gomes, Nature624, 570 (2023)
2023
-
[58]
C. Lu, C. Lu, R. T. Lange, J. Foerster, J. Clune, and D. Ha, (2024), arXiv:2408.06292 [cs.AI]
Pith/arXiv arXiv 2024
-
[59]
Y. Yamada, R. T. Lange, C. Lu, S. Hu, C. Lu, J. Foerster, J. Clune, and D. Ha, (2025), arXiv:2504.08066 [cs.AI]
Pith/arXiv arXiv 2025
-
[60]
Introducing the Model Context Protocol,
Anthropic, “Introducing the Model Context Protocol,”https://www.anthropic.com/news/ model-context-protocol(2024)
2024
-
[61]
Equipping agents for the real world with Agent Skills,
Anthropic, “Equipping agents for the real world with Agent Skills,”https://agentskills.io(2025)
2025
-
[62]
Y. Zou, A. H. Cheng, A. Aldossary, J. Bai, S. X. Leong, J. A. Campos-Gonzalez-Angulo, C. Choi, C. T. Ser, G. Tom, A. Wang, Z. Zhang, I. Yakavets, H. Hao, C. Crebolder, V. Bernales, and A. Aspuru-Guzik, Matter (2025), 10.1016/j.matt.2025.102263, arXiv:2505.02484 [cs.AI]
arXiv 2025
-
[63]
N. J. Szymanski, B. Rendy, Y. Fei, R. E. Kumar,et al., Nature624, 86 (2023)
2023
- [64]
-
[65]
Sugahara and H
Y. Sugahara and H. Toki, Nucl. Phys. A579, 557 (1994)
1994
-
[66]
G. A. Lalazissis, J. Konig, and P. Ring, Phys. Rev. C 55, 540 (1997), arXiv:nucl-th/9607039
Pith/arXiv arXiv 1997
-
[67]
B. G. Todd-Rutel and J. Piekarewicz, Phys. Rev. Lett. 95, 122501 (2005), arXiv:nucl-th/0504034
Pith/arXiv arXiv 2005
-
[68]
P. Bedaque and A. W. Steiner, Phys. Rev. Lett.114, 031103 (2015), arXiv:1408.5116 [nucl-th]
Pith/arXiv arXiv 2015
-
[69]
L. McLerran and S. Reddy, Phys. Rev. Lett.122, 122701 (2019), arXiv:1811.12503 [nucl-th]
Pith/arXiv arXiv 2019
-
[70]
H. Tan, J. Noronha-Hostler, and N. Yunes, Phys. Rev. Lett.125, 261104 (2020), arXiv:2006.16296 [astro- ph.HE]
Pith/arXiv arXiv 2020
-
[71]
S. Altiparmak, C. Ecker, and L. Rezzolla, Astrophys. J. Lett.939, L34 (2022), arXiv:2203.14974 [astro-ph.HE]
Pith/arXiv arXiv 2022
-
[72]
J. D. Walecka, Annals Phys.83, 491 (1974)
1974
-
[73]
B. D. Serot and J. D. Walecka, Adv. Nucl. Phys.16, 1 (1986)
1986
-
[74]
Bouyssy, J
A. Bouyssy, J. F. Mathiot, N. Van Giai, and S. Marcos, Phys. Rev. C36, 380 (1987)
1987
-
[75]
R. C. Tolman, Phys. Rev.55, 364 (1939)
1939
-
[76]
J. R. Oppenheimer and G. M. Volkoff, Phys. Rev.55, 374 (1939)
1939
-
[77]
G. Baym, C. Pethick, and P. Sutherland, Astrophys. J. 170, 299 (1971)
1971
-
[78]
W. D. Arnett and R. L. Bowers, Astrophys. J. Suppl.33, 415 (1977)
1977
-
[79]
Bayes, Philosophical Transactions of the Royal Society of London53, 370 (1763)
T. Bayes, Philosophical Transactions of the Royal Society of London53, 370 (1763)
-
[80]
M. Dutra, O. Lourenco, J. S. Sa Martins, A. Delfino, J. R. Stone, and P. D. Stevenson, Phys. Rev. C85, 035201 (2012), arXiv:1202.3902 [nucl-th]
Pith/arXiv arXiv 2012
discussion (0)
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