A Radio Pulsar Spinning at 716 Hz

Fernando Camilo (Columbia); Ingrid H. Stairs (UBC); Jason W.T. Hessels (McGill); Paulo C.C. Freire (NAIC); Scott M. Ransom (NRAO); Victoria M. Kaspi (McGill)

REVIEW

A Radio Pulsar Spinning at 716 Hz

Jason W.T. Hessels (McGill), Scott M. Ransom (NRAO), Ingrid H. Stairs (UBC), Paulo C.C. Freire (NAIC), Victoria M. Kaspi (McGill), Fernando Camilo (Columbia)

Astrophysics · Submitted 16 Jan 2006 · 34 references

Pith's verdict: A real discovery with a sound measurement, but the one load-bearing claim — that 716 Hz is the fundamental and not twice 358 Hz — rests on profile symmetry rather than a decisive test, and the authors say so themselves.

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CitationFernando Camilo (Columbia), Ingrid H. Stairs (UBC), Jason W.T. Hessels (McGill), Paulo C.C. Freire (NAIC), Scott M. Ransom (NRAO), Victoria M. Kaspi (McGill). "A Radio Pulsar Spinning at 716 Hz." arXiv:astro-ph/0601337 (2006). https://pith.science/paper/3LUOQQBE

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Bottom line: this is a genuine discovery paper and the measurement is solid, but the claim everything hangs on — that 716.35556 Hz is the fundamental and not the second harmonic of a 358-Hz pulsar — is argued from profile symmetry, not from a decisive measurement. The authors are upfront about that, which counts for a lot. What's new: PSR J1748−2446ad, a 1.0944-day circular orbit, ≥0.14 Msun companion, ~40% eclipse at 2 GHz, and the first object past B1937+21's 642 Hz in 23 years. The ephemeris is a clean Keplerian fit, the DM comes from channel delays across 600 MHz, and the signal is cross-checked against every other known Terzan 5 pulsar. The derived physics is handled with more care than most discovery papers: the 16-km radius bound is explicitly conditional on M < 2 Msun, the paper says outright that no existing equation-of-state model is excluded because the mass is unknown, and it declines to claim gravitational-wave spin-down despite the r-mode motivation. Table 1's |ν̇|, τc, Bsurf and Ė are labelled as limits because there is no phase connection. That is honest work. Where it is soft: the harmonic test. The stress-test note is right that folding at 358 Hz puts the two aliased pulses at phases 0 and 0.5 by construction, so 'two peaks 180° apart' is guaranteed under either hypothesis. What actually carries the argument is that the peaks are identical in shape and amplitude in both Spigot and GASP data — a real two-pole beam usually is not that symmetric, but 'usually' is never quantified, and at 0.08 mJy the noise could hide a difference. One correction to the note: the interpulse at phase 0.75 maps to 0.375 in the 358-Hz fold, not 0.5, so it is a third component rather than a doubled one. That mildly favours 716 Hz but does not settle it, so the note's conclusion stands. A phase-coherent timing solution would close this, and the paper says one is coming. Also, the classifier record claims the authors state no limitations; that is wrong, they state several explicitly. Who it is for: anyone working on millisecond pulsar spin distributions, r-modes, or neutron star radius constraints. It deserves a referee's time and it deserves citing as the record holder.

Referee report

Significance

If the identification holds, this is a substantial result: it raises the maximum known neutron-star spin frequency by about 12%, ends a 23-year-old record, and converts a previously open theoretical question (is there a spin ceiling near 700 Hz?) into an empirical one. The paper deserves credit for several things done well. The harmonic ambiguity is attacked with independent instrumentation rather than a single data set, and the GASP coherent-dedispersion cross-check is a genuinely independent handle because it removes interstellar smearing and yields sharper profiles. The radius bound is stated as a falsifiable, mass-conditional limit rather than a point value, and the authors are explicit that it does not exclude any existing equation of state because the mass is unknown. The confrontation with the r-mode literature is specific, names the predicted critical frequency and its temperature range, and states plainly what would have to change if the instability is real. Table 1 is honest about what cannot yet be measured, and the discussion of selection effects against fast, eclipsing binaries is a useful reframing of the B1937+21 folklore. The paper also identifies concrete follow-up

Major objections (1)

[Observations and data analysis (358-Hz disambiguation; Fig. 1)] The paragraph beginning 'We have verified that this signal is not harmonically related...' and Fig. 1 carry the load-bearing claim of the paper, and the disambiguation against a 358-Hz fundamental rests on profile morphology rather than on timing. Two of the three stated arguments do not discriminate. Folding at 358 Hz places the two aliased 716-Hz pulses at phases 0 and 0.5 by construction, so 'two identical peaks separated by 180 degrees' is guaranteed under the 716-Hz hypothesis and is equally the expected signature of a genuine two-component beam at 358 Hz; the discriminating content is entirely in the assertion that the two peaks are identical 'within the resolution and RMS noise level,' which is never quantified. The interpulse at phase 0.75 likewise does not discriminate: under the 358-Hz hypothesis it maps to phase 0.25 of the 358-Hz fold, i.e., a third emission component, which is not obviously less natural than an interpulse. The GASP cross-check is genuinely valuable because coherent dedispersion sharpens the profile, but it is applied as the same qualitative test. Note also that the ~300 microsecond effective resolution quoted in the Fig. 1 caption smears the 1.396 ms profile over roughly 21% of the period, comparable to the scale on which a main pulse and an interpulse would be expected to differ, which makes the unquantified shape comparison weaker than it first appears. I would ask the authors to (i) give a quantitative two-sided comparison of the two half-period profiles in both the Spigot and GASP data (for example a reduced chi-square or a Kolmogorov-Smirnov test on the on-pulse residuals), (ii) state an explicit upper limit on any asymmetry between the two components, and (iii) either drop the interpulse as independent support for 716 Hz or state what it would look like under each hypothesis. A short explicit argument from the known population, namely that main-pulse/interpulse pairs in millisecond pulsars are neither exactly 180 degrees apart nor identical in shape, so that the 358-Hz hypothesis requires a coincidence, would also strengthen the case at little cost. I do not regard this as threatening the conclusion, but as written the harmonic test is a plausibility judgement rather than a measurement.

Minor objections (7)

[Table 1] The quoted limits |Pdot| <= 6e-19 s/s and |nudot| <= 3e-13 Hz/s are mutually consistent through Pdot = nudot/nu^2, but the derived quantities in the same table are not: tau_c >= 2.5e7 yr, B_surf <= 1.1e9 G, and Edot <= 1.3e37 erg/s all correspond to Pdot approximately 8.8e-19 s/s, about 1.5 times the quoted limit. Using the quoted 6e-19 s/s one obtains tau_c >= 3.7e7 yr, B_surf <= 9.3e8 G, and Edot <= 8.7e36 erg/s. The limits are conservative in either case, but the table should be made self-consistent, or the caption should say which Pdot was used for the derived columns.
[Observations and data analysis (eclipse geometry)] The text states an eclipse region of 'physical size ~5-6 Rsun' for an orbital separation of '~4-5 Rsun' without defining whether 'size' is a radius or a diameter. For Porb = 1.0944 d and masses 1.4 + 0.14 Msun the separation is about 5.2 Rsun, and an eclipse fraction of 0.4 corresponds to an eclipsing radius of about 3 Rsun, i.e., a transverse extent of about 6 Rsun. The numbers are therefore consistent if 'size' means diameter, but the reader cannot tell, and the stated separation should be reconciled with the ephemeris and the minimum companion mass.
[Implications and discussion (r-mode paragraph)] The r-mode constraint is stated only qualitatively: the paper says the |nudot| limit 'is consistent with those measured for other millisecond pulsars, and does not suggest an anomalously rapid spin-down rate.' The decisive number is available and would sharpen the claim considerably. For a 716-Hz pulsar, r-mode spin-down on a timescale of order 100 yr corresponds to |nudot| of order 1e-7 Hz/s, roughly six orders of magnitude above the quoted limit of 3e-13 Hz/s, so the limit excludes active r-mode spin-down at the current epoch rather than merely failing to require it. One or two sentences making that comparison explicit would substantially strengthen the abstract's claim that the short period constrains r-mode models.
[Implications and discussion (radius limit)] The radius bound uses the Lattimer-Prakash relation, in which R is the non-rotating radius; rotation increases the equatorial radius, and the paper should say so, since the bound is quoted as a property of the object rather than of its non-rotating counterpart. The arithmetic should also be checked against the stated limits: for M = 2 Msun the relation gives R <= 16.2 km, so '< 16 km' is slightly tighter than the formula supports, while the 1.4 Msun case (14.4 km) is consistent.
[Observations and data analysis (ephemeris-folded detections)] The paper reports detection in at least 18 of 30 observations, including 'many observations where it was not initially identified through a periodicity search' after applying the orbital ephemeris. Because folding with a known ephemeris can accumulate noise into a plausible-looking peak, the signal-to-noise threshold used to count these as detections should be stated, together with the number of independent trial ephemeris phases searched.
[Implications and discussion, reference 18] The comparison with Li and Steiner's 11.5-13.6 km radius range rests on a preprint (nucl-th/0511064) rather than a published article. The comparison is not load-bearing, since the paper's own 14.4 km bound stands independently, but the citation should be flagged as unpublished or updated if a journal version now exists.
[Abstract and Fig. 1] The abstract states flatly that the object is a '716-Hz pulsar' while the text says the folding tests 'strongly suggest' 716 Hz is the true spin frequency; matching the hedge in the abstract would be more accurate. In Fig. 1, 32 phase bins across a 1.396 ms period give 43.6 microseconds per bin, so the profile is oversampled by roughly a factor of seven relative to the stated ~300 microsecond resolution; the caption should say this explicitly, since it bears directly on the shape comparison discussed above. Finally, a few typographical errors should be corrected: 'determinarion' (should be 'determination'), 'accomodates' (should be 'accommodates'), and 'On a least two epochs' (should be 'On at least two epochs').

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The paper

The paper claims

A radio pulsar in the globular cluster Terzan 5 spins 716 times a second, which would make it the fastest-spinning neutron star known and would cap its radius at 16 km for any mass below 2 solar masses.

The reading

The paper sets out to establish that a newly found radio pulsar in the globular cluster Terzan 5, PSR J1748$-$2446ad, rotates 716.35556 times a second, which would make it the fastest-spinning neutron star on record and would displace the 642-Hz pulsar B1937+21, holder of that title since 1982. The claim matters because a neutron star's spin rate sets a ceiling on how large it can be: a star turning this fast would shed mass if its non-rotating radius exceeded about 16 km at any mass below 2 $M_odot$, giving a size limit that does not depend on the unknown equation of state of dense matter. The same number bears on gravitational-wave physics, since published models put the r-mode instability — a class of fluid oscillation that radiates angular momentum away and brakes the star — at a critical frequency below 700 Hz, so a 716-Hz pulsar means either those models are wrong or the instability only bites at higher spin. The authors also argue that the object's faintness (0.08 mJy at 1950 MHz) and its 40% eclipse duty cycle are precisely the conditions that would hide even faster pulsars, making the new record a detection threshold rather than a physical ceiling.

What carries the argument

The load-bearing device is the harmonic test rather than the timing. A 716-Hz signal folded at 358 Hz must show two peaks exactly 180° apart in pulse phase, and a genuine 358-Hz pulsar with a two-component profile could mimic that. The authors argue the mimicry is implausible because the two peaks agree in shape within the noise in both the Spigot data and the coherently dedispersed GASP data, because folding at other harmonically related frequencies gives consistent results, and because a weak interpulse appears at phase 0.75 in the 716-Hz profile. The second piece of machinery is the mass-shedding relation $nu_{max} = 1045,(M/M_odot)^{1/2}(10,mathrm{km}/R)^{3/2}$ Hz, taken from Lattimer and Prakash, which converts the measured 716 Hz into a radius ceiling once a mass is assumed.

Extended reading notes

Core claim

PSR J1748$-$2446ad was found in 10 November 2004 Green Bank Telescope observations of Terzan 5 at 1950 MHz and confirmed on 8 January 2005; the authors detect it in at least 18 of 30 multi-hour observations and fit a Keplerian orbit with a period of 1.09443034(6) days, projected semi-major axis 1.10280(6) light-seconds, eccentricity below $10^{-4}$, and a companion of at least 0.14 $M_odot$. The pulsar is eclipsed for roughly 40% of each orbit at 2 GHz, an eclipse region 5–6 solar radii across for a binary separation of only 4–5 solar radii, which the authors compare to PSR J1740$-$5340 and to the 1.8-hour Terzan 5 binary PSR J1748$-$2446A. The measured pulse frequency is 716.35556(3) Hz. Because the data cannot be phase-connected across epochs, only an upper limit on the spin-down rate is available, $|dotnu| le 3times10^{-13}$ Hz/s, so the characteristic age, surface magnetic field and spin-down luminosity are limits rather than measurements. The authors' reading is that the object is a recycled millisecond pulsar spun up by accretion, and that its existence raises the empirical maximum spin frequency by about 12%.

Load-bearing premise

The claim rests on 716 Hz being the true spin frequency rather than the second harmonic of a 358-Hz pulsar, and that identification rests on pulse-profile shape in the absence of a phase-coherent timing solution.

Editorial extensions

If this is right

The maximum observed neutron star spin frequency moves from 642 Hz to 716 Hz, roughly a 12% increase, and the 23-year-old record held by B1937+21 falls.
For any mass below 2 $M_odot$ the non-rotating radius of this particular star is bounded above at 16 km; for an assumed 1.4 $M_odot$ the bound is 14.4 km, consistent with the 11.5–13.6 km range that Li and Steiner derive from laboratory nuclear measurements.
r-mode models that place the instability's critical frequency below 700 Hz across core temperatures of $10^7$–$10^{10}$ K are excluded for this object, so either the instability sets in only at higher spin or the crust-core coupling in those models needs reworking.
The authors argue that even faster pulsars exist but are hidden: their spin-down winds ablate their companions, the resulting material eclipses the radio beam, and low-frequency surveys miss them, so deeper surveys at higher radio frequencies are the way to find them.
The Bayesian spin-frequency cutoffs of 760 Hz, later revised to 730 Hz, derived from accreting millisecond pulsars become harder to sustain, since one known radio pulsar already sits at 716 Hz.

Reading between the lines

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

If the eclipse is caused by material ablated from the companion, the eclipse duration should shorten at higher radio frequencies; a 3–5 GHz observation of PSR J1748$-$2446ad would test that directly and, if it works, would supply a cheap way to find the faster pulsars the authors predict.
The radius bound is only as good as the assumed mass, and the authors note the orbit is too circular for periastron advance to help; an optical mass ratio for the companion, as was done for PSR J1740$-$5340, is the most plausible route to turning 16 km into a real equation-of-state constraint.
Because the harmonic ambiguity is the only thing standing between 358 Hz and 716 Hz, the same profile-shape test applied to other faint fast binaries in Terzan 5 could systematically hide or reveal half-frequency errors in the cluster's published spin distribution.
A 716-Hz pulsar with no measurable spin-down is also a null result for continuous gravitational-wave emission from this object: the limit $|dotnu| le 3times10^{-13}$ Hz/s implies any r-mode or crustal quadrupole is radiating well below the level that would brake the star on a $10^7$-year timescale.

Original abstract

We have discovered a 716-Hz eclipsing binary radio pulsar in the globular cluster Terzan 5 using the Green Bank Telescope. It is the fastest-spinning neutron star ever found, breaking the 23-year-old record held by the 642-Hz pulsar B1937+21. The difficulty in detecting this pulsar, due to its very low flux density and high eclipse fraction (~40% of the orbit), suggests that even faster-spinning neutron stars exist. If the pulsar has a mass less than 2 Msun, then its radius is constrained by the spin rate to be < 16 km. The short period of this pulsar also constrains models that suggest gravitational radiation, through an r-mode instability, limits the maximum spin frequency of neutron stars.

The compiled record

The paper's own sentences, arranged, kept beside the review and separate from it. Each label is drawn from a closed vocabulary; the number beside it is the probability the classifier gave that label. Numbers in the tables are the authors', checked by code. No sentence in this record was written by a model.

Compiled by classifier-1.13.0 via TypeSafe API, question bank abstract-p1-20260923, 2026-09-23: 1 request, 4,324 input tokens.

What the abstract itself states, as probabilities: claims first 0.31 · states limitation 0.84 · human participants 0.02 · controlled comparison 0.09 · randomized assignment 0.01 · states quantitative result 0.98 · compares with prior results 0.96 · mentions code or data availability 0.02.

The abstract, sentence by sentence

arXiv listing abstract v1. Results and the main claim are underlined; show every role.

We have discovered a 716-Hz eclipsing binary radio pulsar in the globular cluster Terzan 5 using the Green Bank Telescope. It is the fastest-spinning neutron star ever found, breaking the 23-year-old record held by the 642-Hz pulsar B1937+21. The difficulty in detecting this pulsar, due to its very low flux density and high eclipse fraction (~40% of the orbit), suggests that even faster-spinning neutron stars exist. If the pulsar has a mass less than 2 Msun, then its radius is constrained by the spin rate to be < 16 km. The short period of this pulsar also constrains models that suggest gravitational radiation, through an r-mode instability, limits the maximum spin frequency of neutron stars.

background contribution method result interpretation main claim

What the classifier reports for each sentence. The number is the probability it gave the label.
#	sentence	role	the authors' own work	states the main conclusion	strength
s0	We have discovered a 716-Hz eclipsing binary radio pulsar in the globular cluster Terzan 5 using the Green Bank Telescope.	result 0.74	0.98	0.55	asserted 1.00
s1	It is the fastest-spinning neutron star ever found, breaking the 23-year-old record held by the 642-Hz pulsar B1937+21.	result 0.91	0.69	0.71	asserted 1.00
s2	The difficulty in detecting this pulsar, due to its very low flux density and high eclipse fraction (~40% of the orbit), suggests that even faster-spinning neutron stars exist.	interpretation 0.99	0.57	0.12	hedged possibility 1.00
s3	If the pulsar has a mass less than 2 Msun, then its radius is constrained by the spin rate to be < 16 km.	interpretation 0.67	0.61	0.08	asserted 0.62
s4	The short period of this pulsar also constrains models that suggest gravitational radiation, through an r-mode instability, limits the maximum spin frequency of neutron stars.	interpretation 0.97	0.60	0.10	asserted 0.86

What kind of paper the classifier reports this is: empirical study 1.00 · evidence from observation or experiment 1.00.

What was examined, and what was not

sources read

arXiv listing abstract v1

not examined

full text
figures and tables
references and citing sentences
relations to other papers

levels run

P abstract

not run

S sections
T body sentences
C citations
R cross-paper relations

Every quoted sentence on this record is the authors'. Every label is from Pith's closed vocabulary, with the probability shown beside it. Every number in the measurements table is the authors', checked by code. Record as JSON

Figures

**Figure 1.** Master PSR J1748−2446ad pulse profile from the combination of eight GBT Pulsar Spigot observations at 2 GHz with particularly good detections of the pulsar. The cumulative integration time is ∼54 hrs. There are 32 phase bins across the profile, and the y-axis plots flux in arbitrary units. The one sigma error bar on the flux is shown in the lower left-hand corner. The effective time resolution of the data, ∼ 300 µs, which accounts for pulse smearing due to channelisation of the dispersed data and finite time sampling, is indicated by the horizontal bar. A weak, but statistically…

Figures reproduced from arXiv:astro-ph/0601337 by the authors.

References

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Fastest spinning millisecond pulsars: indicators for quark matter in neutron stars?
nucl-th 2024-12 conditional novelty 6.0 of 10

Hybrid stars with color-superconducting quark matter can reproduce the mass and spin of pulsar J0952-0607, whereas the hadronic-only model cannot, and the revised Kepler-frequency relation tightens radius bounds.
Multimessenger constraints for ultra-dense matter
astro-ph.HE 2021-05 accept novelty 6.0 of 10

A 1.5-million-member ensemble of interpolated neutron-star equations of state yields a maximum neutron-star mass of 2.53 solar masses (2.19 if the GW170817 remnant was hypermassive) and a maximum dimensionless spin of 0.81.
Rapidly Spinning Compact Stars with Deconfinement Phase Transition
astro-ph.HE 2020-09 conditional novelty 6.0 of 10

Holographic neutron star models with a deconfinement phase transition give Mmax/MTOV = 1.227(+0.031/-0.016), slightly above the Breu-Rezzolla bound, supporting a rapidly rotating neutron star interpretation of GW19081...
Direct Astrophysical Tests of Chiral Effective Field Theory at Supranuclear Densities
astro-ph.HE 2020-04 conditional novelty 6.0 of 10

Conditioning a nonparametric neutron-star equation-of-state prior on chiral effective field theory predictions, the authors find astrophysical data favor the theory up to nuclear saturation density and bound where it ...
Nonparametric constraints on neutron star matter with existing and upcoming gravitational wave and pulsar observations
astro-ph.HE 2020-03 conditional novelty 6.0 of 10

Joint gravitational-wave, NICER, and pulsar-mass data constrain the radius of a 1.4-solar-mass neutron star to 12.32 km (90% credible interval 10.85 to 13.41 km) and the pressure at twice nuclear density to about 3.8e...
Particle Probes with Superradiant Pulsars
hep-ph 2019-08 conditional novelty 6.0 of 10

The existence of PSR J1748-2446ad and PSR B1937+21 excludes ultralight scalars coupled to neutrons with masses near 10^-11 eV at couplings as small as 10^-6 times gravity.
Axion superradiance in rotating neutron stars
hep-ph 2019-04 conditional novelty 6.0 of 10

Axion bound states around neutron stars can superradiantly amplify by mixing with photon modes that scatter off the resistive, rotating magnetosphere, producing an exponential instability whose rate is computed pertur...
Rapid Bayesian position reconstruction for gravitational-wave transients
gr-qc 2015-08 conditional novelty 6.0 of 10

A deterministic Bayesian algorithm converts matched-filter trigger values into a gravitational-wave sky map in about ten seconds, matching full Markov chain Monte Carlo localization accuracy on 500 simulated binary ne...
Quadratic-in-spin effects in the orbital dynamics and gravitational-wave energy flux of compact binaries at the 3PN order
gr-qc 2015-01 accept novelty 6.0 of 10

The authors derive the previously unknown 3PN quadratic-in-spin contributions to the gravitational-wave energy flux of spinning compact binaries, and confirm existing 3PN spin-spin equations of motion.
Cubic order spin effects in the dynamics and gravitational wave energy flux of compact object binaries
gr-qc 2014-11 conditional novelty 6.0 of 10

A Lagrangian octupolar formalism yields the leading 3.5PN cubic-in-spin contributions to binary dynamics and gravitational-wave energy flux, checked against Kerr and black-hole perturbation results in limiting cases.
I-Love-Q, Spontaneously: Slowly Rotating Neutron Stars in Scalar-Tensor Theories
gr-qc 2014-05 accept novelty 6.0 of 10

Slowly rotating neutron stars in scalar-tensor theories with spontaneous scalarization obey I-Love-Q relations that match general relativity to within a few percent, so these observables cannot discriminate between th...
Effective No-Hair Relations for Neutron Stars and Quark Stars: Relativistic Results
gr-qc 2014-03 accept novelty 6.0 of 10

Multipole moments of rotating neutron stars and quark stars up to hexadecapole order satisfy approximately equation-of-state-independent relations, confirmed in full general relativity with two independent numerical c...
Resonant-plane locking and spin alignment in stellar-mass black-hole binaries: a diagnostic of compact-binary formation
gr-qc 2013-02 conditional novelty 6.0 of 10

A toy model of black-hole binary formation predicts that efficient tidal alignment locks spins into a resonant plane, with the preferred angle set by whether mass transfer reversed the mass ratio.
Nonparametric Inference of Neutron Star Composition, Equation of State, and Maximum Mass with GW170817
astro-ph.HE 2019-10 conditional novelty 5.5 of 10

GW170817's tidal data, combined with a 2 solar mass pulsar, prefer soft neutron-star equations of state and give factor-of-two, prior-dependent hints of quark matter and a phase transition near nuclear density.
Ranking Prompt--Plateau Correlations in Gamma-Ray Bursts with Symbolic Regression
astro-ph.HE 2026-10 conditional novelty 5.0 of 10

The Dainotti relation between GRB plateau luminosity and duration is a projection of a tighter three-parameter plane that also includes prompt peak luminosity.
Sub-Millisecond Pulsars: Missing or Impossible?
astro-ph.HE 2026-08 conditional novelty 5.0 of 10

Sub-millisecond pulsars are intrinsically rare because recycling is inefficient, suitable donor stars evolve too quickly, and fast-spinning neutron stars spin down unless their magnetic fields are extremely weak.
Hybrid Stars with Post-Merger Rotation Profiles
gr-qc 2026-06 unverdicted novelty 5.0 of 10

Differential rotation in hybrid stars with deconfinement phase transition allows quasi-toroidal configurations with quark matter rings and leads to degeneracies in rotational profiles at mass-radius curve intersections.
Magnetic Eruption and Nucleosynthesis in GR{\nu}MHD Simulations of Spinning Neutron Star Mergers
astro-ph.HE 2026-05 unverdicted novelty 5.0 of 10

3D GRMHD simulations with second-moment neutrino transport show aligned spins produce more collimated polar outflows and 2.4e-3 solar masses of proton-rich material yielding light r-process elements like 56Ni, while a...
Hybrid neutron stars among mass gap objects are excluded by twin stars at $1.4\,M_\odot$
astro-ph.HE 2026-05 unverdicted novelty 5.0 of 10

Mass-gap compact objects could be hybrid stars only with very early deconfinement and stiff quark matter; confirming 1.4 M⊙ twin stars would cap hybrid-star maximum mass below 2.2 M⊙.
Bayesian analysis of density profile of light dark matter elucidating the properties of dark matter admixed neutron stars in the presence of hyperons
nucl-th 2026-05 unverdicted novelty 5.0 of 10

Bayesian analysis finds that the likely ranges of light dark-matter fermion mass and exponential density-profile parameter in hyperon-containing neutron stars are nearly independent of the hadronic model for symmetry-...
Effective-one-body waveforms for precessing coalescing compact binaries with post-newtonian Twist
gr-qc 2021-11 conditional novelty 5.0 of 10

The TEOBResumS effective-one-body model is extended to full inspiral-merger-ringdown for precessing binaries with higher modes, reaching median mismatches of roughly 4 to 7 parts in a thousand against numerical relativity.
GW190814 as a massive rapidly-rotating neutron star with exotic degrees of freedom
astro-ph.HE 2020-07 conditional novelty 5.0 of 10

New vector interactions in the Chiral Mean Field model let hybrid neutron stars reach about 2.5 solar masses when rotating rapidly, but only with more baryons than a non-rotating star can hold.
Multiband Gravitational-Wave Astronomy: Observing binary inspirals with a decihertz detector, B-DECIGO
gr-qc 2018-02 conditional novelty 5.0 of 10

B-DECIGO alone could pin the mass ratio of a GW150914-like binary to better than 0.1 percent and its black-hole spins to better than 10 percent, with multiband follow-up sharpening neutron-star tidal measurements.
Observing and measuring the neutron-star equation-of-state in spinning binary neutron star systems
gr-qc 2018-01 conditional novelty 5.0 of 10

For rapidly spinning binary neutron stars, the spin-quadrupole deformation is degenerate with masses and spins, but combined with tidal effects it improves LIGO's ability to distinguish neutron-star equations of state.
Constraining nonperturbative strong-field effects in scalar-tensor gravity by combining pulsar timing and laser-interferometer gravitational-wave detectors
gr-qc 2017-04 conditional novelty 5.0 of 10

Five binary pulsars plus eleven neutron-star equations of state push the Damour-Esposito-Farese parameters to beta_0 above about -4.3 at 90% confidence, leaving narrow mass windows where neutron stars could still scal...
Upper limits on the rates of binary neutron star and neutron-star--black-hole mergers from Advanced LIGO's first observing run
astro-ph.HE 2016-07 accept novelty 5.0 of 10

No binary neutron star or neutron star-black hole mergers were detected in Advanced LIGO's first observing run, yielding 90% confidence rate ceilings of 12,600 and 3,600 per cubic gigaparsec per year.
Millisecond pulsar interpretation of the Galactic center gamma-ray excess
astro-ph.HE 2014-04 conditional novelty 5.0 of 10

A bulge population of roughly 13,000 millisecond pulsars, with a luminosity function calibrated on Fermi-LAT disk pulsars, can reproduce the Galactic center gamma-ray excess while staying below the point-source detect...
Pulsars Cannot Account for the Inner Galaxy's GeV Excess
astro-ph.HE 2013-05 conditional novelty 5.0 of 10

The inner Galaxy's GeV excess has a spectrum too hard, and too much flux, to come from millisecond pulsars, which can supply at most about 10 percent of it.
Correlating Surface Magnetic Field Decay with Internal Field Depth of Isolated Neutron Stars
astro-ph.HE 2026-09 conditional novelty 4.0 of 10

Magnetic fields confined to the shallow outer crust of neutron stars decay appreciably on Gyr timescales, while fields anchored deep in the inner crust remain nearly frozen, a depth sensitivity verified across three e...
Searching for links between energetic millisecond pulsars and repeating fast radio bursts
astro-ph.HE 2026-05 unverdicted novelty 4.0 of 10

Wideband observations show M28A giant pulses differ from FRB 20200120E bursts in duration, luminosity, timing statistics, and spectral structure, yielding no strong evidence for a direct link.
Rapidly Spinning Massive Pulsars as an Indicator of Quark Deconfinement
nucl-th 2025-12 conditional novelty 4.0 of 10

Within a tuned hybrid equation of state, a color-superconducting quark core—absent from the hyperonic hadronic model—is needed to reach the mass and spin of PSR J0952–0607.
Understanding the Neutron Star Population with the SKAO Telescopes
astro-ph.HE 2026-07 accept novelty 3.5 of 10

SKAO AA* and AA4 surveys are projected to discover thousands of ordinary pulsars and ~800–1000 MSPs, enabling population synthesis, mass measurements and tests of gravity and emission physics.
Probing Neutron Star Interiors and the Properties of Cold Ultra-dense Matter with the SKAO
astro-ph.HE 2026-07 accept novelty 3.5 of 10

SKAO's sensitivity, surveys and sub-arraying will deliver tighter NS mass, MoI, spin, glitch and precession constraints that, with X-ray and GW data, probe cold ultra-dense matter.
Pulsars in Globular Clusters With the SKAO
astro-ph.HE 2026-07 conditional novelty 3.0 of 10

SKA-MID and SKA-LOW are predicted to discover 150–1700 new pulsars in Galactic globular clusters, more than doubling the current population of 345.
Dark matter in compact stars
hep-ph 2023-07 conditional novelty 3.0 of 10

The paper reviews dark matter searches using white dwarfs and neutron stars, organizing capture, heating, collapse, explosion, and gravitational-wave signatures into a single reference.
Searches for Continuous-Wave Gravitational Radiation
astro-ph.HE 2022-06 accept novelty 2.0 of 10

No continuous gravitational wave has yet been detected; this review consolidates the source physics, search methods, and published upper limits, and argues that a first detection is plausible within the next several years.
Phase transitions in neutron stars and their links to gravitational waves
astro-ph.HE 2019-07 unverdicted novelty 2.0 of 10

Review of neutron star dense matter, hadron-quark phase transitions, and potential g-mode signatures in gravitational waves from multimessenger observations.
Universal Relations and Alternative Gravity Theories
gr-qc 2017-09 conditional novelty 2.0 of 10

Universal relations among neutron star observables (I-Love-Q, higher multipole moments, oscillation frequencies) survive in most alternative theories of gravity, which limits their power to discriminate between theories.
Physics of Neutron Star Crusts
astro-ph 2008-12 accept novelty 2.0 of 10

A comprehensive 2008 synthesis of neutron star crust physics that organizes crust composition, equation of state, elasticity, superfluid dynamics, transport, and observations into a single referenced framework.
Binary and Millisecond Pulsars
astro-ph 2008-11 accept novelty 2.0 of 10

A comprehensive 2008 review of binary and millisecond pulsars that consolidates Galactic population estimates, double neutron star merger rates, and pulsar-timing tests of general relativity.

How later papers used it

200 later papers cite it

Evidence: substantial. 186 of the citing papers share no author with it, and 105 of those carry a confident label from Pith's citation classifier.

Pith read 24 of the 258 citing sentences, choosing only those whose citation markers point at this paper alone, and wrote the paraphrases from them. The summary, the counts, the evidence level, the links and the quotes come from code; the summary counts the papers listed below. A later paper is listed under a label when Pith's citation classifier gives one of its sentences that label at probability 0.8 or more (0.95 for support), Pith's reading finds that the citing paper itself did it, and a second check confirms the paraphrase against the sentence. This section lists uses only. It does not list criticism or disagreement, so their absence here says nothing about how the paper has been received. Papers that share an author with this one are listed apart, under "By the same authors". A quote is the citing authors' own sentence, shown when their paper's licence is CC BY, CC BY-SA or CC0. JSON

5 later papers by other authors are listed below: 5 used its data or values. 1 more paper by the same authors is listed: 1 used its data or values.

Uses its data or values 6 of 107 papers with this label · 1 by the same authors

Used the 716 Hz pulsar PSR J1748-2446ad from this paper, along with PSR B1937+21, to constrain particles that couple to the stellar medium.

Particle Probes with Superradiant Pulsars (2019) · 0.97 · paraphrased: the licence does not allow quoting
Used the 716 Hz rotation frequency of PSR J1748-2446ad from this paper to derive an updated lower bound on the mass-radius relation of compact stars.

Rapidly Spinning Massive Pulsars as an Indicator of Quark Deconfinement (2025) · 1.00 · paraphrased: the licence does not allow quoting
For example, electromagnetic observations of millisecond pulsars place the limit for maximum rotation at $716$ Hz [ref] , a value that is significantly smaller than any of the Kepler frequencies listed in Table [ref].

Assessing the impact of uniform rotation on the structure of neutron stars (2024) · Impact of Rotation on Maximum Masses · 0.84
We evaluate the effects of uniform rotation on two millisecond pulsars observed by the NICER collaboration: PSR J0030+0451 and PSR J0740+6620, with rotational frequencies of 205 Hz [ref] , 346 Hz [ref] and the most rapid known pulsar PSR J1748-2446ad observed to date with 716 Hz [ref] .

Hyper-neutron stars from an ab initio calculation (2025) · NUMERICAL RESULTS AND DISCUSSION · 0.99
Used this paper to state that neutron stars with spin frequencies as high as 716 Hz are known to exist from pulsar observations.

Constraining the equation of state of neutron stars using multimessenger observations (2022) · 0.89 · paraphrased: the licence does not allow quoting

By the same authors

Noted that this paper's 716 Hz for PSR J1748-2446ad in Terzan 5, the largest spin frequency currently measured for a radio pulsar, may already exclude several equations of state if its mass were known to be small.

Probing Neutron Star Interiors and the Properties of Cold Ultra-dense Matter with the SKAO (2026) (same authors) · 0.92 · paraphrased: the licence does not allow quoting

How the literature uses it

92 arXiv papers cite this in 134 sentences

Each citing sentence is taken from the citing paper's LaTeX source and typed by Pith's classifier. A label appears at probability 0.8 or more (0.95 for support), a contest at 0.7 or more; the quoted words are the citing authors'. How each label was checked · JSON

Papers citing it · 59 sentences without a confident label

Uses its data or values 57 papers

We will use the pulsars PSR J1748-2446ad (716 Hz) [ref] and PSR B1937+21 (642 Hz) [ref] to constrain particles that couple to the stellar medium.

Particle Probes with Superradiant Pulsars · Results · 0.97
Using the rotation frequency of the fastest known pulsar, PSR J1748–2446ad, at 716 Hz [ref] , we derive an updated lower bound on the mass-radius relation of compact stars.

Rapidly Spinning Massive Pulsars as an Indicator of Quark Deconfinement · Results · 1.00
In Fig. [ref], we show the excluded regions in the conductivity vs dark-photon mass plane obtained by imposing $τ<τ_spindown$ for three known sources, namely pulsars J1938+2012 [ref] and J1748-2446ad [ref] , and pulsar binary B1957+20 [ref] .

Superradiance in rotating stars and pulsar-timing constraints on dark photons · Pulsar-Timing Constraints on Dark Photons · 0.95

Compares with it 1 paper

It is interesting that the fastest known pulsar PSR J1748-2446ad (716Hz) [ref] may be spinning marginally faster than the limit here, when canonical mass $1.5M_⊙$ and radius $12$km are assumed.

Fermionic dark stars spin slowly · Timescale of r-mode instability and critical angular frequency · 0.82

Cites it as background 2 papers

Although other macroscopic properties of may also be observable, such as the moment of inertia [ref] and the maximum attainable spin frequency [ref] , our current knowledge of the at densities above $$ is dominated by observations of massive , , and X-ray timing.

Direct Astrophysical Tests of Chiral Effective Field Theory at Supranuclear Densities · Introduction · 0.86
Other possible future probes of NS structure include moment of inertia (MoI) measurements via pulsar timing [ref] , postmerger signals from BNS coalescences [ref] , coalescences of NSs and black holes (BHs) [ref] , or pulsar spin measurements [ref] .

Nonparametric constraints on neutron star matter with existing and upcoming gravitational wave and pulsar observations · Introduction · 0.94

Discussion

Disagree with the review, or know something it missed? Leave a comment, highlight any passage above to comment on it, or challenge this review formally.

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