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REVIEW 4 major objections 2 minor 3 cited by

Gravitational Instability and Fragmentation in Collapsar Disks Supports the Formation of Sub-Solar Neutron Stars

T0 review · 4 major / 2 minor · reviewed 2026-08-05 · deepseek-v4-flash

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Pith's one-line read Collapsar disks may forge neutron stars too light for supernovae.

desk verdict Plausible and potentially important formation channel, but the load-bearing step from clumps to neutron stars is explicitly not simulated, and we only have the abstract to judge. read the letter →

arxiv 2508.17183 v1 pith:D3KL54TY submitted 2025-08-24 astro-ph.HE

Yi-Xian Chen , Brian D. Metzger This is my paper · ORCID
classification astro-ph.HE
keywords collapsardisksgravitationalinstabilitydiskfragmentationsub-solarneutronstarselectronfractionneutrinocoolingshearing-boxsimulationswaves
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

This paper argues that the outer parts of neutrino-cooled disks formed from collapsing rotating massive stars (collapsars) can fragment under self-gravity into neutron-rich clumps, which then go on to form neutron stars with masses below the usual stellar-scale range. Using three-dimensional shearing-box hydrodynamical simulations with a physical equation of state and optically-thin neutrino cooling, the authors find that fragmentation happens when the disk cools quickly enough on a dynamical timescale, corresponding to accretion rates above roughly one solar mass per second. The clumps have electron fractions around 0.1 and masses between about 0.01 and 1 solar masses, and most exceed the local Chandrasekhar mass, so they are expected to collapse to nuclear densities and become sub-solar-mass neutron stars. If correct, this gives a new formation channel for compact objects that are otherwise difficult to produce, and it predicts gravitational-wave signals from mergers of these objects that coincide with the collapsar's gamma-ray burst and supernova.

What carries the argument

The argument is carried by three linked quantities: the Toomre parameter Q, which measures whether self-gravity overcomes shear and pressure in a rotating disk; the dimensionless cooling timescale tau_cool = t_cool * Omega, whose value below about 10 enables runaway cooling and fragmentation; and the Chandrasekhar mass M_Ch ~ Ye^2, which ties the ability to form a neutron star to the electron fraction Ye, a measure of neutron richness. The clump masses are set near the local Jeans mass. The 3D shearing-box hydrodynamic simulations, with neutrino cooling and an electron fraction determined by weak-interaction balance, connect these ingredients and produce the predicted clump population.

What would settle it

Run a three-dimensional simulation that follows one Jeans-mass clump with Ye ~ 0.1 through its collapse, including neutrino transport and tidal torques from the surrounding disk: if the clump is tidally disrupted or neutrino heating raises Ye above about 0.5 before nuclear densities are reached, the sub-solar neutron star claim fails. Observationally, the gravitational-wave detection of a merger with a component mass clearly below about one solar mass, or the absence of such events associated with collapsar gamma-ray bursts, would also test the channel.

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Extended reading notes

Core claim

The paper claims that gravitational instability in the outer regions of collapsar disks is not merely a transient feature but leads to genuine fragmentation into self-bound, neutron-rich clumps. In 3D shearing-box simulations started at Toomre parameter Q ~ 1, runaway cooling and fragmentation occur when the dimensionless cooling timescale tau_cool = t_cool * Omega falls below about 10, a regime reached at accretion rates larger than about one solar mass per second. The resulting clumps have electron fraction Ye ~ 0.1 and masses ~0.01-1 solar masses, scattered around the local Jeans mass. Because most clumps exceed the local Chandrasekhar mass, M_Ch ~ Ye^2, they should continue to collapse t

Load-bearing premise

The neutron-star outcome rests on the assumption that the neutron-rich clumps formed in the simulations stay bound and keep their low electron fraction while collapsing all the way to nuclear densities, a step the simulations do not actually follow.

Editorial extensions

If this is right

  • Sub-solar-mass neutron stars gain a concrete formation path outside ordinary stellar core-collapse, arising on dynamical timescales in collapsar disks.
  • The trigger condition is quantitative: disks with accretion rates above roughly one solar mass per second and cooling timescales tau_cool < 10 are the required environments.
  • If disk-formed neutron stars pair up and merge, the gravitational-wave chirps would be temporally coincident with the collapsar's gamma-ray burst and supernova, giving a multi-messenger signature.
  • Both neutron-rich disks (Ye ~ 0.1) and alpha-particle-dominated disks (Ye ~ 0.5) can fragment into neutron-rich clumps, broadening the applicability of the channel.
  • The clump mass range 0.01-1 solar masses around the Jeans value yields a predicted mass spectrum for compact remnants from this formation route.

Reading between the lines

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

  • If the clumps survive their first few orbits rather than merging into the central black hole, some may be ejected or form a population of low-mass compact objects that later merge, contributing to gravitational-wave events with extreme mass ratios.
  • The same fragmentation criterion (Q ~ 1, tau_cool < 10) plausibly applies to other rapidly accreting neutrino-cooled disks, such as those formed in compact-object mergers or tidal disruption events, making the sub-solar neutron star channel potentially broader than collapsars alone.
  • A population-synthesis calculation comparing the predicted rate of sub-solar compact-object mergers from collapsar disks with observed gravitational-wave event rates would provide a direct test of how often the clumps actually become neutron stars.
  • The paper's own caveat points to a targeted numerical experiment: follow a single clump's collapse with neutrino transport to check whether Ye stays near 0.1 or whether neutrino heating raises it, which would decide between a neutron star and a low-mass black hole.
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Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

4 major / 2 minor

Summary. The abstract claims 3D shearing-box hydrodynamical simulations of collapsar disks, using a physical equation of state and neutrino cooling, show that disks with Toomre Q ~ 1 fragment when t_cool Ω < 10, producing neutron-rich clumps (electron fraction Ye ~ 0.1, masses ~0.01–1 M⊙). It further claims that most clumps exceed the local Chandrasekhar mass and will therefore collapse to form sub-solar-mass neutron stars, potentially giving rise to detectable gravitational-wave chirps from subsequent mergers. However, the full text supplied with this submission is an unrelated manuscript on Rydberg atomic receivers for direction-of-arrival detection (arXiv:2508.17179). None of the astrophysical simulations, numerical details, equations, or results described in the abstract appear in the deposited body, making it impossible to verify any of the paper's central claims.

Significance. If substantiated, the proposed mechanism would be a novel and interesting formation channel for sub-solar-mass neutron stars, with potentially observable gravitational-wave signatures. The abstract's honest caveat that the simulations 'cannot follow this process directly' is a strength in transparency, but it also exposes the central claim to additional, untested assumptions: clump survival against shear, retention of the neutron-rich electron fraction during collapse, and actual dynamical collapse to nuclear densities. As submitted, the paper cannot be evaluated on its merits because the full text is absent and no numerical evidence is presented. The significance of the idea does not compensate for the lack of supporting content.

major comments (4)
  1. [Full Text (entire manuscript)] The deposited full text is a paper on 'Polarization-Aware DoA Detection Relying on a Single Rydberg Atomic Receiver'—a subject entirely unrelated to collapsar disks, gravitational instability, or neutron stars. The abstract of the submission describes original 3D shearing-box simulations with a physical EOS and neutrino cooling, but no such simulations, equations, figures, tables, or references appear in the body. This is a load-bearing problem: every quantitative claim in the abstract (tau_cool < 10, Ye ~ 0.1, clump masses 0.01–1 M⊙, most clumps exceeding M_Ch) is unsupported by any accessible derivation or data. The manuscript cannot be reviewed as an astrophysical simulation paper until the correct full text is supplied.
  2. [Abstract, clump-to-NS collapse step] The headline claim that clumps exceeding the local Chandrasekhar mass 'will continue to collapse to nuclear densities, forming neutron stars' is explicitly not simulated: the abstract states 'our simulations cannot follow this process directly.' Three conditions must hold for that extrapolation to be valid, and none is demonstrated: (1) clump survival against tidal shear in a Keplerian disk, which requires a quantitative condition such as t_ff Ω < 1 or a comparison with the Hill radius; (2) retention of Ye ≈ 0.1 (or further reduction by electron capture) during collapse, since weak interactions can raise or lower Ye; and (3) dynamical collapse rather than quasi-static contraction or dispersal. The M_Ch argument alone does not establish collapse; it only identifies a threshold for degeneracy-pressure support.
  3. [Abstract, mass distribution and M_Ch threshold] The statement 'most clumps exceed the local Chandrasekhar mass M_Ch ~ Ye^2' is quantitatively unsubstantiated. For Ye = 0.1, M_Ch ≈ 5.83 Ye^2 M⊙ ≈ 0.058 M⊙. The abstract reports clump masses in the range 0.01–1 M⊙ 'around the local Jeans value,' which does not imply that a majority of clumps are above 0.058 M⊙. Without the actual mass distribution or a mass-weighted statistic, the conclusion that 'most' clumps collapse is not supported even by the abstract's own numbers.
  4. [Abstract, numerical reliability] No numerical details are available anywhere in the submitted text: no grid resolution, box size, boundary conditions, neutrino-cooling implementation, equation of state details, or convergence study. Fragmentation and clump survival in shearing-box simulations of gravitationally unstable disks are known to be resolution- and cooling-rate dependent. The threshold tau_cool < 10 and the reported clump properties cannot be accepted as quantitative results without a convergence demonstration. This missing support is load-bearing, since the paper's conclusions depend on those specific thresholds and on the clump mass spectrum.
minor comments (2)
  1. [Abstract, notation] Units are written informally: 'Msun/s', 'Msun', 'M_Ch ~ Ye^2'. Please use standard notation (M⊙, M_Ch ≈ 5.83 Ye^2 M⊙) and define all symbols at first use. Also clarify whether 'around the local Jeans value' refers to the peak or the mean of the clump mass distribution.
  2. [General, manuscript completeness] The references list in the full text is entirely devoted to Rydberg atomic sensing and quantum estimation. If this is the wrong file accidentally submitted, the corrected manuscript must include the astrophysical references (e.g., on collapsar disks, shearing-box fragmentation, and proto-neutron star collapse) as well as all figures and tables referenced in the abstract.

Circularity Check

0 steps flagged · score 0.0 of 10

No circularity found in the abstract; the supplied full text is an unrelated manuscript, so body-level checks cannot be performed.

full rationale

The abstract's derivation chain is: (1) shearing-box hydrodynamical simulations with a physical equation of state, optically-thin neutrino cooling, and an electron fraction set by pair-capture balance; (2) fragmentation occurs when the dimensionless cooling timescale tau_cool < 10; (3) clumps form with Ye ~ 0.1 and masses ~0.01-1 Msun around the local Jeans value; (4) most clumps exceed M_Ch ~ Ye^2 and therefore are argued to collapse to sub-solar neutron stars. None of these steps reduces to its own input by construction. The tau_cool threshold is an emergent simulation output, not a fitted parameter; Ye ~ 0.1 follows from the assumed microphysical reaction balance, not from the target conclusion; the clump masses are simulation measurements compared with the standard Jeans and Chandrasekhar scalings. The step 'most clumps exceed M_Ch and hence will collapse to NS' is an extrapolation, explicitly disclaimed in the abstract ('our simulations cannot follow this process directly'), and it is a limitation regarding physical completeness rather than circularity: the conclusion is not used as an input to produce the simulation outcome. I also note that the full text supplied with this submission is a different, unrelated Rydberg-receiver paper (arXiv-style title and authors), so no body-level circularity check is possible from the provided material. Based on the available abstract, I find no circular reasoning, no fitted input renamed as prediction, and no load-bearing self-citation.

Assumptions & free parameters 1 free parameters · 3 assumptions · 0 invented entities

The abstract does not reveal free parameters beyond the initial Toomre setting; the main axioms are the shearing-box approximation, the pair-capture electron-fraction assumption, and the extrapolation from M_Ch to NS formation.

free parameters (1)
  • Initial Toomre parameter Q = ~1
    Simulations initialize disks in a marginally stable state with Q~1, a modeling choice selected by hand to trigger fragmentation; not fitted to data.
assumptions (3)
  • domain assumption The shearing-box approximation captures the local fragmentation physics of the outer collapsar disk.
    Simulations are 3D shearing-box, which assumes a local periodic patch; global disk structure is not modeled.
  • domain assumption Electron fraction is set by the balance of electron/positron pair-capture reactions.
    Abstract states this assumption; other processes such as neutrino absorption and nucleosynthesis are ignored.
  • domain assumption Clumps exceeding the local Chandrasekhar mass will continue to collapse to nuclear densities.
    Abstract admits simulations cannot follow this process directly; the fate of clumps is extrapolated from the M_Ch criterion.

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Cite this review

Pith. "Pith review of Gravitational Instability and Fragmentation in Collapsar Disks Supports the Formation of Sub-Solar Neutron Stars." pith.science (2026). https://pith.science/paper/D3KL54TY

@misc{pith2026250817183,
  author       = {Pith},
  title        = {Pith review of: Gravitational Instability and Fragmentation in Collapsar Disks Supports the Formation of Sub-Solar Neutron Stars},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/D3KL54TY}},
  note         = {Machine review of arXiv:2508.17183}
}
read the original abstract

We perform three-dimensional shearing-box hydrodynamical simulations to explore the outcome of gravitational instability in the outer regions of neutrino-cooled disks such as those formed from the collapse of rotating massive stars ("collapsars''). We employ a physical equation of state, optically-thin neutrino cooling, and assume an electron fraction set by the balance of electron/positron pair-capture reactions. Disks in a marginally stable initial state (Toomre parameter Q~ 1) undergo runaway cooling and fragmentation when the dimensionless cooling timescale obeys tau_cool = t_cool*Omega < 10, where Omega is the orbital frequency; these conditions correspond to accretion rates > Msun/s on the upper end of those achieved by collapsar progenitor stars. Fragmentation leads to the formation of neutron-rich clumps (electron fraction Ye ~ 0.1) spanning a range of masses ~0.01-1 Msun around the local Jeans value. Most clumps exceed the local Chandrasekhar mass M_Ch ~ Ye^2 and hence will continue to collapse to nuclear densities, forming neutron stars (NS) with sub-solar masses otherwise challenging to create through ordinary stellar core-collapse. Even cool disks dominated by alpha-particles (Ye ~ 0.5) can fragment and collapse into neutron-rich clumps capable of forming sub-solar NSs. Although our simulations cannot follow this process directly, if the disk-formed NSs subsequently pair into binaries, the gravitational wave chirps from their rapid mergers are potentially detectable by ground based observatories. The temporal coincidence of such a hierarchical NS merger chain with the collapsar gamma-ray burst and supernova would offer a uniquely spectacular multi-messenger "symphony''.

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Reference graph

Works this paper leans on

45 extracted references · 36 canonical work pages · cited by 3 Pith papers

  1. [1]

    Quantum information process- ing, sensing, and communications: Their myths, realities, and futures,

    L. Hanzo, Z. Babar, Z. Cai, D. Chandra, I. B. Djordjevic, B. Koczor, S. X. Ng, M. Razavi, and O. Simeone, “Quantum information process- ing, sensing, and communications: Their myths, realities, and futures,” Proc. IEEE, to appear, 2025

    2025

  2. [2]

    Rydberg atomic quantum receivers for classical wireless communication and sensing,

    T. Gong, A. Chandra, C. Yuen, Y . L. Guan, R. Dumke, C. M. S. See, M. Debbah, and L. Hanzo, “Rydberg atomic quantum receivers for classical wireless communication and sensing,”IEEE Wirel. Commun., to appear, 2025

    work page 2025

  3. [3]

    Rydberg states of alkali atoms in atomic vapour as SI-traceable field probes and communications receivers,

    N. Schlossberger, N. Prajapati, S. Berweger, A. P. Rotunno, A. B. Artusio-Glimpse, M. T. Simons, A. A. Sheikh, E. B. Norrgard, S. P. Eckel, and C. L. Holloway, “Rydberg states of alkali atoms in atomic vapour as SI-traceable field probes and communications receivers,”Nat. Rev. Phys., Sep. 2024

    work page 2024

  4. [4]

    Rydberg atom electric field sensors for communications and sensing,

    C. T. Fancher, D. R. Scherer, M. C. S. John, and B. L. S. Marlow, “Rydberg atom electric field sensors for communications and sensing,” IEEE Trans. Quantum Eng., vol. 2, pp. 1–13, Mar. 2021

    work page 2021

  5. [5]

    Quantum sensing,

    C. L. Degen, F. Reinhard, and P. Cappellaro, “Quantum sensing,”Rev. Mod. Phys., vol. 89, p. 035002, Jul. 2017

    work page 2017

  6. [6]

    Quantum sensing of microwave electric fields based on Rydberg atoms,

    J. Yuan, W. Yang, M. Jing, H. Zhang, Y . Jiao, W. Li, L. Zhang, L. Xiao, and S. Jia, “Quantum sensing of microwave electric fields based on Rydberg atoms,”Rep. Prog. Phys., vol. 86, no. 10, p. 106001, Sep. 2023

    work page 2023

  7. [7]

    Microwave electrometry with Rydberg atoms in a vapour cell using bright atomic resonances,

    J. A. Sedlacek, A. Schwettmann, H. K ¨ubler, R. L ¨ow, T. Pfau, and J. P. Shaffer, “Microwave electrometry with Rydberg atoms in a vapour cell using bright atomic resonances,”Nat. Phys., vol. 8, no. 11, pp. 819–824, Nov. 2012

    work page 2012

  8. [8]

    Investigating electromagnetically induced transparency spectral lineshape distortion due to non-uniform fields in Rydberg-atom electrometry,

    A. P. Rotunno, C. L. Holloway, N. Prajapati, S. Berweger, A. B. Artusio- Glimpse, R. Brown, M. Simons, A. K. Robinson, B. N. Kayim, M. A. Viray, J. F. Jones, B. C. Sawyer, R. Wyllie, T. Walker, R. W. Ziolkowski, S. R. Jefferts, S. Geibel, J. Wheeler, and E. Imhof, “Investigating electromagnetically induced transparency spectral lineshape distortion due to...

    2023

Show all 45 references
  1. [9]

    Atomic superheterodyne receiver based on microwave-dressed Rydberg spectroscopy,

    M. Jing, Y . Hu, J. Ma, H. Zhang, L. Zhang, L. Xiao, and S. Jia, “Atomic superheterodyne receiver based on microwave-dressed Rydberg spectroscopy,”Nat. Phys., vol. 16, no. 9, pp. 911–915, Jun. 2020

    2020

  2. [10]

    Continuous wideband microwave-to-optical converter based on room-temperature Rydberg atoms,

    S. Bor ´owka, U. Pylypenko, M. Mazelanik, and M. Parniak, “Continuous wideband microwave-to-optical converter based on room-temperature Rydberg atoms,”Nat. Photonics, vol. 18, no. 1, pp. 32–38, Oct. 2024

    2024

  3. [11]

    Deep learning enhanced Rydberg multifrequency microwave recognition,

    Z.-K. Liu, L.-H. Zhang, B. Liu, Z.-Y . Zhang, G.-C. Guo, D.-S. Ding, and B.-S. Shi, “Deep learning enhanced Rydberg multifrequency microwave recognition,”Nat. Commun., vol. 13, no. 1, p. 1997, Apr. 2022

    1997

  4. [12]

    Shortwave ultrahigh- sensitivity Rydberg atomic electric field sensing based on a subminiature resonator,

    R. Mao, Y . Lin, A. Zhou, K. Yang, and Y . Fu, “Shortwave ultrahigh- sensitivity Rydberg atomic electric field sensing based on a subminiature resonator,”IEEE Trans. Antennas Propag., vol. 72, no. 11, pp. 8165– 8172, Nov. 2024

    2024

  5. [13]

    Towards atomic MIMO receivers,

    M. Cui, Q. Zeng, and K. Huang, “Towards atomic MIMO receivers,” IEEE J. Sel. Areas Commun., vol. 43, no. 3, pp. 659–673, Mar. 2025

    2025

  6. [14]

    Atom- based vector microwave electrometry using Rubidium Rydberg atoms in a vapor cell,

    J. A. Sedlacek, A. Schwettmann, H. K ¨ubler, and J. P. Shaffer, “Atom- based vector microwave electrometry using Rubidium Rydberg atoms in a vapor cell,”Phys. Rev. Lett., vol. 111, p. 063001, Aug 2013

    2013

  7. [15]

    Precise measurement of microwave polarization using a Rydberg atom-based mixer,

    Y . Wang, F. Jia, J. Hao, Y . Cui, F. Zhou, X. Liu, J. Mei, Y . Yu, Y . Liu, J. Zhang, F. Xie, and Z. Zhong, “Precise measurement of microwave polarization using a Rydberg atom-based mixer,”Opt. Express, vol. 31, no. 6, pp. 10 449–10 457, Mar. 2023

    2023

  8. [16]

    Optimal state choice for Rydberg-atom microwave sensors,

    A. Chopinaud and J. Pritchard, “Optimal state choice for Rydberg-atom microwave sensors,”Phys. Rev. Appl., vol. 16, p. 024008, Aug. 2021

    2021

  9. [17]

    Polarization-insensitive microwave electrometry using Rydberg atoms,

    M. Cloutman, M. Chilcott, A. Elliott, J. S. Otto, A. B. Deb, and N. Kjærgaard, “Polarization-insensitive microwave electrometry using Rydberg atoms,”Phys. Rev. Appl., vol. 21, p. 044025, Apr. 2024

    2024

  10. [18]

    Vector magnetometry based on electromag- netically induced transparency in linearly polarized light,

    V . I. Yudin, A. V . Taichenachev, Y . O. Dudin, V . L. Velichansky, A. S. Zibrov, and S. A. Zibrov, “Vector magnetometry based on electromag- netically induced transparency in linearly polarized light,”Phys. Rev. A, vol. 82, p. 033807, Sep. 2010

    2010

  11. [19]

    Measurements of the magnetic field vector using multiple electromagnetically induced transparency resonances in Rb vapor,

    K. Cox, V . I. Yudin, A. V . Taichenachev, I. Novikova, and E. E. Mikhailov, “Measurements of the magnetic field vector using multiple electromagnetically induced transparency resonances in Rb vapor,”Phys. Rev. A, vol. 83, p. 015801, Jan. 2011

    2011

  12. [20]

    A Rydberg atom-based mixer: Measuring the phase of a radio frequency wave,

    M. T. Simons, A. H. Haddab, J. A. Gordon, and C. L. Holloway, “A Rydberg atom-based mixer: Measuring the phase of a radio frequency wave,”Appl. Phys. Lett., vol. 114, no. 11, p. 114101, Mar. 2019

    2019

  13. [21]

    Linear dynamic range of a Rydberg- atom microwave superheterodyne receiver,

    F. Wu, Q. An, Z. Sun, and Y . Fu, “Linear dynamic range of a Rydberg- atom microwave superheterodyne receiver,”Phys. Rev. A, vol. 107, p. 043108, Apr. 2023

    2023

  14. [22]

    Harnessing Rydberg atomic receivers: From quantum physics to wireless communications,

    Y . Chen, X. Guo, C. Yuen, Y . Zhao, Y . L. Guan, C. M. S. See, M. D ´ebbah, and L. Hanzo, “Harnessing Rydberg atomic receivers: From quantum physics to wireless communications,”arXiv preprint: 2501.11842, 2025. [Online]. Available: https://arxiv.org/abs/2501.11842

    2025 arXiv

  15. [23]

    Rydberg atomic quantum receivers for classical wireless communications and sensing: Their models and performance,

    T. Gong, J. Sun, C. Yuen, G. Hu, Y . Zhao, Y . L. Guan, C. M. S. See, M. Debbah, and L. Hanzo, “Rydberg atomic quantum receivers for classical wireless communications and sensing: Their models and performance,”arXiv preprint: 2412.05554, 2024. [Online]. Available: https://arxi...

    2024

  16. [24]

    Theory of dark resonances for alkali-metal vapors in a buffer-gas cell,

    A. V . Ta ˘ıchenachev, V . I. Yudin, R. Wynands, M. St ¨ahler, J. Kitching, and L. Hollberg, “Theory of dark resonances for alkali-metal vapors in a buffer-gas cell,”Phys. Rev. A, vol. 67, p. 033810, Mar 2003

    2003

  17. [25]

    Magnetic-field-induced splitting of Rydberg Electromagnet- ically Induced Transparency and Autler-Townes spectra in 87Rb vapor cell,

    X. Li, Y . Cui, J. Hao, F. Zhou, Y . Wang, F. Jia, J. Zhang, F. Xie, and Z. Zhong, “Magnetic-field-induced splitting of Rydberg Electromagnet- ically Induced Transparency and Autler-Townes spectra in 87Rb vapor cell,”Opt. Express, vol. 31, no. 23, pp. 38 165–38 178, Nov. 2023

    2023

  18. [26]

    Determining the angle-of-arrival of a radio-frequency source with a Rydberg atom-based sensor,

    A. K. Robinson, N. Prajapati, D. Senic, M. T. Simons, and C. L. Holloway, “Determining the angle-of-arrival of a radio-frequency source with a Rydberg atom-based sensor,”Appl. Phys. Lett., vol. 118, no. 11, p. 114001, Mar. 2021

    2021

  19. [27]

    Quantum-MUSIC: Multiple signal classification for quantum wireless sensing,

    H. Kim, H. Park, and S. Kim, “Quantum-MUSIC: Multiple signal classification for quantum wireless sensing,”IEEE Wireless Commun. Lett., to appear, 2025

    2025

  20. [28]

    Determining angle of arrival of radio frequency fields using subwavelength, amplitude-only measurements of standing waves in a Rydberg atom sensor,

    R. Talashila, W. J. Watterson, B. L. Moser, J. A. Gordon, A. B. Artusio-Glimpse, N. Prajapati, N. Schlossberger, M. T. Simons, and C. L. Holloway, “Determining angle of arrival of radio frequency fields using subwavelength, amplitude-only measurements of standing waves in a Ry...

    2025

  21. [29]

    Rydberg atomic quantum receivers for multi-target DOA estimation,

    T. Gong, C. Yuen, C. M. S. See, M. Debbah, and L. Hanzo, “Rydberg atomic quantum receivers for multi-target DOA estimation,”arXiv preprint: 2501.02820, 2025. [Online]. Available: https://arxiv.org/abs/ 2501.02820

    2025

  22. [30]

    Three- dimensional location system based on an L-shaped array of Rydberg atomic receivers,

    Y . Yan, J. Yuan, L. Zhang, L. Xiao, S. Jia, and L. Wang, “Three- dimensional location system based on an L-shaped array of Rydberg atomic receivers,”Opt. Lett., vol. 48, no. 15, pp. 3945–3948, Aug. 2023

    2023

  23. [31]

    Enhancing sensitivity of atomic microwave receivers based on optimal laser arrays,

    B. Wu, R. Mao, D. Sang, Z. Sun, Y . Liu, Y . Lin, Q. An, and Y . Fu, “Enhancing sensitivity of atomic microwave receivers based on optimal laser arrays,”IEEE Trans. Antennas Propag., vol. 73, no. 2, pp. 793–806, Feb. 2025

    2025

  24. [32]

    QuTiP: An open-source Python framework for the dynamics of open quantum systems,

    J. R. Johansson, P. D. Nation, and F. Nori, “QuTiP: An open-source Python framework for the dynamics of open quantum systems,”Comp. Phys. Comm., vol. 183, no. 8, pp. 1760–1772, Apr. 2012

    2012

  25. [33]

    Cramer-Rao bounds for antenna array design,

    H. Gazzah and S. Marcos, “Cramer-Rao bounds for antenna array design,”IEEE Trans. Signal Process., vol. 54, no. 1, pp. 336–345, Jan. 2006

    2006

  26. [34]

    Vector-sensor array processing for electromag- netic source localization,

    A. Nehorai and E. Paldi, “Vector-sensor array processing for electromag- netic source localization,”IEEE Trans. Signal Process., vol. 42, no. 2, pp. 376–398, Feb. 1994

    1994

  27. [35]

    Zeeman effect in parabolic quantum dots,

    R. Rinaldi, P. V . Giugno, R. Cingolani, H. Lipsanen, M. Sopanen, J. Tulkki, and J. Ahopelto, “Zeeman effect in parabolic quantum dots,” Phys. Rev. Lett., vol. 77, pp. 342–345, Jul 1996

    1996

  28. [36]

    Wigner-eckart theorem and simple lie groups,

    J. Ginibre, “Wigner-eckart theorem and simple lie groups,”J. Math. Phys., vol. 4, no. 5, pp. 720–726, May 1963

    1963

  29. [37]

    Tables of Clebsch-Gordan coeffi- cients of s� � ,

    P. McNamee, S. J., and F. Chilton, “Tables of Clebsch-Gordan coeffi- cients of s� � ,”Rev. Mod. Phys., vol. 36, pp. 1005–1024, Sep. 1964

    1964

  30. [38]

    Wigner��,��, and��symbols

    A. J. Stone, “Wigner��,��, and��symbols.” [Online]. Available: https://www-stone.ch.cam.ac.uk/wigner.shtml

  31. [39]

    Trap-induced AC Zeeman shift of the Thorium-229 nuclear clock frequency,

    K. Beloy, “Trap-induced AC Zeeman shift of the Thorium-229 nuclear clock frequency,”Phys. Rev. Lett., vol. 130, p. 103201, Mar 2023

    2023

  32. [40]

    Simple expression for the quantum Fisher information matrix,

    D. ˇSafr´anek, “Simple expression for the quantum Fisher information matrix,”Phys. Rev. A, vol. 97, p. 042322, Apr. 2018

    2018

  33. [41]

    Quantum Fisher information from randomized measurements,

    A. Rath, C. Branciard, A. Minguzzi, and B. Vermersch, “Quantum Fisher information from randomized measurements,”Phys. Rev. Lett., vol. 127, p. 260501, Dec. 2021

    2021

  34. [42]

    Quantum-enhanced mea- surements: beating the standard quantum limit,

    V . Giovannetti, S. Lloyd, and L. Maccone, “Quantum-enhanced mea- surements: beating the standard quantum limit,”Science, vol. 306, no. 5700, pp. 1330–1336, Nov. 2004

    2004

  35. [43]

    Comparison of noise temperature of Rydberg-atom and electronic microwave receivers,

    G. Santamaria-Botello, S. Verploegh, E. Bottomley, and Z. Popovic, “Comparison of noise temperature of Rydberg-atom and electronic microwave receivers,”arXiv preprint: 2209.00908, 2022. [Online]. Available: https://arxiv.org/abs/2209.00908

    2022 arXiv

  36. [44]

    Approaching the standard quantum limit of a Rydberg-atom microwave electrometer,

    H.-T. Tu, K.-Y . Liao, H.-L. Wang, Y .-F. Zhu, S.-Y . Qiu, H. Jiang, W. Huang, W. Bian, H. Yan, and S.-L. Zhu, “Approaching the standard quantum limit of a Rydberg-atom microwave electrometer,”Sci. Adv., vol. 10, no. 51, p. eads0683, Dec. 2024. 15 Yuanbin Chenis a Research Fel...

    2024

  37. [2022]

    M´erouane Debbahis Professor at Khalifa Uni- versity of Science and Technology in Abu Dhabi and founding Senior Director of KU Digital Future Institute

    He served as an Associate Editor of the IEEE Transactions on Signal Processing and as a member of the IEEE Sensor Array and Multichannel Signal Processing Technical Committee. M´erouane Debbahis Professor at Khalifa Uni- versity of Science and Technology in Abu Dhabi and found...

    2000

Pith tools

Reviewed August 5, 2026 · model on record in the stance chip above.