{"id":"165fe0cc-ed73-46ec-bbc8-8f3b0f73afc0","arxiv_id":"2608.06593","paper_version":1,"verdict":"CONDITIONAL","confidence":"MODERATE","novelty_score":6.0,"correctness_risk":"high","formal_verification":"none","parameter_count":9,"one_line_summary":"The thesis derives a conditional 90% limit |d_n| < 4.42e-25 e cm from the spin-down budget of PSR J0437-4715 via an effective magnetic-quadrupole channel, the first astrophysical bound of this kind.","lead":"A physics thesis models the nearby millisecond pulsar PSR J0437-4715 and uses its measured spin-down to set a new upper limit on the neutron electric dipole moment, about 25 times weaker than the best laboratory bound. The work is a proof of concept for using neutron stars as complementary laboratories for strong CP violation.","discovery_kind":"new_method","skeptic_critique":{"model":"deepseek-v4-flash","headline":"The residual-power estimator's denominator N_pol is calibrated through the spin-down-inferred dipole, so the claimed positive branch may be partly a self-consistency artifact rather than an independent bound.","rationale":"The reader's weakest_assumption centers on the r_pol prior, which the paper itself flags as not theorem-derived and as capable of eliminating the positive residual if the outer freeze-out branch is used. That is real but explicitly conditional. I find the more load-bearing concern in the covariance between the residual numerator and the polarized-neutron denominator: N_pol is built from a polarization fraction introduced in Chapter 2 via the spin-down-inferred dipole, and B_surf inherits timing dependence through the pair-luminosity prior. The estimator Q divides a Pdot-dependent residual by the square of a Pdot-dependent reservoir, so the positive branch and its percentile are not a clean measurement of power left over after independent standard losses. This does not require rejecting the paper: the authors are candid about many of their prescriptions, and the work is a legitimate proof-of-concept that should be read strictly as benchmark limits. It does, however, mean the conditional verdict is warranted and that the headline bound should not be quoted as an independent CP constraint until the N_pol calibration is separated from timing data. The proposed test is straightforward to run with the existing Monte Carlo machinery and would settle whether the effect is numerically important.","tokens_in":54252,"tokens_out":5472,"duration_ms":56715,"concrete_test":"Re-run the Monte Carlo with N_pol and f_pol drawn from a prior derived solely from local polarization physics, completely independent of B_sd and Pdot (for example, a uniform or physics-motivated prior on f_pol, or the random-phase incoherence ensemble of Eq. 6.7), while keeping all other priors identical. Then recompute P(Q>0) and the 90th percentile of M_n^0. If the positive-branch fraction drops below roughly 0.5, or if the quoted 7.47e-38 e cm^2 shifts by more than a factor of 2, the headline bound is dominated by the circular calibration rather than by independent spin-down energetics. As a secondary check, report the Monte Carlo correlation coefficient between Δ and N_pol; a strong positive correlation confirms the common-mode dependence.","verdict_should_be":"UNCHANGED","load_bearing_attack":"The central numerical result is the 90th percentile of the positive branch of Q = 3c^3 Δ / (2 N_pol^2 Ω^4 sin^2 α) (Eq. 5.28). The numerator Δ = Edot - L_dip - L_GW and the denominator N_pol are not shown to be independent. Chapter 2 introduces the global polarization fraction P_req = μ_NS / (N_n,crust |μ_n|) (Eq. 2.6) with μ_NS derived from the spin-down-inferred dipole field B_p (Eq. 2.3). Section 5.2 then constructs the refined reservoir N_pol by applying an adjusted polarization weighting f_pol to the free-neutron integral (Eq. 5.18), but the text does not demonstrate that f_pol is fixed by local crustal physics rather than by matching P_req. In addition, the propagation-based B_surf that sets L_dip retains timing dependence through the pair-luminosity prior L_pair = 10^-2 Edot_int (Eq. 3.16), which enters κ and Γ± in Eq. 3.24. Thus high-Edot realizations can simultaneously raise N_pol (lowering the implied d_n) and raise L_dip (lowering Δ), while low-Edot realizations do the opposite. This common-mode dependence can create a positive residual branch and bias the reported 90th percentile even if no CP-odd neutron moment exists. The paper's caveats acknowledge general model dependence, but not this specific covariance between the subtracted standard losses and the polarized-neutron inventory used to interpret the residual.","agreement_with_reader":"partial"},"referee_report":{"model":"deepseek-v4-flash","summary":"The paper develops a source-specific framework for translating the measured spin-down of PSR J0437-4715 into a constraint on CP-odd neutron electromagnetic moments. It combines a reduced-form density model (Ch. 2), a propagation-informed surface field from UWL polarimetry (Ch. 3), and NICER hot-spot geometry fits (Ch. 4) to construct a present-day luminosity budget. The residual Δ = Ė_int − L_dip − L_GW (Eq. 5.24) is first assigned to coherent electric-dipole radiation (Ch. 5) and then to an effective magnetic-quadrupole channel whose radiating frequency is identified with the OPM transition (Ch. 6). The central numerical results are the conditional 90th-percentile limits |M_n^0| < 7.47×10^-38 e cm^2, |θ̄| < 2.99×10^-9, and |d_n| < 4.42×10^-25 e cm (Eqs. 6.21–6.23), which the paper itself notes are weaker than the current laboratory bound.","tokens_in":54656,"tokens_out":10571,"duration_ms":99428,"significance":"If the method were validated, it would demonstrate that neutron-star spin-down can provide a complementary astrophysical probe of strong-CP violation, albeit one that is not competitive with ultracold-neutron experiments. The paper deserves credit for attempting a P-dot-independent magnetic-field estimate, for propagating many source-specific uncertainties in a Monte Carlo framework, and for being unusually explicit about screening, coherence, and branch-dependence caveats. However, no code or data products are shipped, so the numerical Monte Carlo results cannot be independently checked. More importantly, the central bound is not yet supported: the polarized-neutron inventory in the denominator of the estimator is not shown to be independent of the spin-down budget being analyzed, and the headline branch depends on an underived polarization-limiting-radius prior whose outer-branch alternatives eliminate the positive residual. The work is therefore more convincing as a methodological exercise than as a measurement, and the abstract's quoted limits should not be taken at face value without substantial additional validation.","major_comments":[{"comment":"The polarized-neutron inventory is not shown to be independent of the spin-down budget. Chapter 2 defines 𝒫_req = μ_NS/(N_n,crust |μ_n|) with μ_NS obtained from the timing-based B_p of Eq. (2.3). Section 5.2 then introduces the adjusted polarization fraction f_pol^adj = 1.26×10^-4 in Eq. (5.21) and uses it in Eq. (5.18) to obtain N_pol. The text does not derive f_pol^adj from an independent crustal-magnetization calculation; it appears to inherit the Chapter 2 timing calibration. Because the final estimator Q = 3c^3Δ/(2N_pol^2Ω^4 sin^2 α) has N_pol in the denominator while Δ = Ė_int − L_dip − L_GW, a common dependence on Ė_int can create or erase the positive residual. The manuscript must either derive f_pol from local microphysics or report the correlation between N_pol and Δ and demonstrate that the quoted 90th percentile is robust to this covariance.","section":"§5.2, Eqs. (2.3)–(2.6), (5.18)–(5.28)"},{"comment":"The polarization-limiting radius is a load-bearing prior that is not derived. The adopted r_pol = 0.15–0.22 R_LC (Eq. 3.7) is described as a 'trimmed interior subset' of the emission-height ladder, and the paper explicitly states that it does not follow from a theorem requiring r_pol < 0.30 R_LC. Since B_surf ∝ r_pol^3 (Eq. 3.32), the outer edge of the emission envelope raises the median field by ≈4.3 and an outer freeze-out branch by factors of 20–33; as §3.6 notes, those fields make L_dip exceed Ė_int and remove the positive residual on which both the EDR and MQM bounds depend. The central 90% limits are therefore conditional on a branch that the paper's own sensitivity analysis shows is not excluded. A physics-based derivation of r_pol, or a quantitative report of the final limits under the outer-branch systematics, is required before the headline numbers can be assessed.","section":"§3.2, §3.6, Eqs. (3.7), (3.32), (3.33)"},{"comment":"The reported bound is the 90th percentile of the positive-residual subsample, not a 90% upper limit over the full model. Equation (5.29) gives P(Q>0)=0.787, so 21.3% of Monte Carlo draws produce Δ<0, meaning the modeled standard losses already exceed the observed spin-down. Conditioning on Q>0 selects the branch on which the prior stack leaves power; it does not provide posterior coverage for the null hypothesis of no CP-odd channel. The paper should report the full signed posterior, including the mass associated with Δ<0 realizations, before using '90% upper limit' language.","section":"§5.3.1, Eqs. (5.29)–(5.32)"},{"comment":"The magnetic-quadrupole channel is an invented effective model rather than a derived neutron property. The luminosity formula introduces an effective single-neutron MQM M_n^0 with K_quad = 1/(60π) and sets the radiating mode frequency to ω_rad = 2πν_OPM without a microscopic calculation connecting a GHz magnetospheric scale to a CP-odd neutron quadrupole. The paper is transparent about this prescription, but the consequence is that Eqs. (6.21)–(6.23) are not measurements of d_n; they are conversions of an assumed residual power through an unvalidated channel. The manuscript should either provide a microscopic derivation or present the numerical values explicitly as an illustrative translation rather than as a bound.","section":"§6.3, Eqs. (6.15)–(6.18), (6.16)–(6.17)"},{"comment":"The propagation-based field is not fully independent of the spin-down budget. The pair-luminosity prior L_pair = 10^-2 Ė_int (Eq. 3.16) enters κ and Γ± in Eq. (3.24), so B_surf inherits timing dependence even though B_sd is not used. The paper acknowledges 'limited timing dependence,' but this dependence is load-bearing because the same Ė_int defines the residual that the field is used to interpret. The sensitivity of the final limit to the 10^-2 normalization and to the ±0.25 dex width should be quantified explicitly.","section":"§3.3–3.4, Eq. (3.16)"}],"minor_comments":[{"comment":"The piecewise density profile is written with explicit r^4 factors and, in the core branch, a leading 4π^2; as printed the equation has inconsistent dimensions unless the coefficients are understood to absorb all scales. Please rewrite in a dimensionally transparent form and define the units of a, b, c, d.","section":"Eq. (2.1)"},{"comment":"The ray–field angle θ is listed as an adopted input θ=15°, but §3.4 derives it as 11.9°–14.9° from dipolar geometry for the fiducial r_pol branch. The table should state whether θ is a derived quantity or an independently assigned prior.","section":"Table 3.2 and §3.4"},{"comment":"The notation '90% C.L.' is used for a percentile of a conditional positive branch; consider using '90th percentile of the Q>0 subsample' throughout to avoid implying standard frequentist coverage.","section":"Fig. 5-2 and §5.3.1"},{"comment":"Q is introduced first as a signed estimator and then as d_n^2 on the positive branch; the figure and text should define Q90 consistently and make clear that Q has units of (e cm)^2.","section":"Eqs. (5.28), (5.31)"},{"comment":"The statement that 'the large fraction of unphysical Monte Carlo draws' suggests the force-free normalization over-assigns power is important; please move this caveat into the main results section rather than leaving it only in the future-work section.","section":"§7.1.1"}],"recommendation":"major_revision","confidential_remarks":"The manuscript is an undergraduate thesis, and its ambition is commendable, but the central quantitative claim is not ready for publication as stated. The reader's stress-test concern lands: Eqs. (2.6) and (5.21) connect the polarized-neutron reservoir to the same timing-based spin-down budget used to define the residual, and §3.6 shows that the alternative r_pol branches destroy the positive residual. I would advise the editor that the most defensible path is either a major revision adding an independent N_pol calibration and a full branch/systematic reporting, or a reframing as a methods paper in which the quoted limits are explicitly illustrative rather than asserted as bounds."},"author_rebuttal":null,"desk_editor":{"model":"deepseek-v4-flash","letter":"Here's the short version: this bachelor's thesis proves a concept, not a measurement. It is the first attempt I know of to turn a pulsar's spin-down budget into an upper bound on a neutron CP-odd moment, and the construction is genuinely source-specific. But the headline number is roughly 25 times weaker than the current laboratory nEDM limit, and the route from residual power to neutron moment has a load-bearing prior and a partial circularity that a referee will need to see addressed.\n\nWhat's good: the paper is honest about its own fragility. It repeatedly labels the field 'not model-free', calls the MQM channel 'a phenomenological mode prescription', and admits the r_pol prior 'does not follow from a theorem'. The magnetic field normalization comes from radio-polarization propagation (OPM transition, pair-plasma priors), not from P-Pdot, which avoids the most obvious version of circularity. The NICER hot-spot geometry decomposition into dipole and quadrupole fractions is clean and the two allowed families give nearly identical dipolar luminosities. Monte Carlo propagation is used throughout and the uncertainty budget is reported.\n\nThe soft spots are real. First, B_surf scales as r_pol^3; the paper's own outer freeze-out branch raises the median field by factors of 4-33, which pushes L_dip over the total spin-down and destroys the positive residual. The r_pol prior is a choice, not a measurement. Second, and more serious, the stressed covariance is there. N_pol is calibrated through the spin-down-inferred dipole moment (Eqs. 2.3-2.6, the P_req bookkeeping), and the pair-luminosity prior L_pair = 10^-2 Edot_int keeps timing dependence in B_surf and hence L_dip. So high-Edot realizations simultaneously inflate the denominator N_pol and deflate the numerator Delta of the estimator Q = 3c^3 Delta/(2 N_pol^2 Omega^4 sin^2 alpha). The 21.3% of draws with Delta<0 are a symptom; the 90th percentile of the positive branch is a selected statistic. That doesn't make the paper worthless, but it means the quoted limit is an illustration of the framework under adopted prescriptions, not an independent astrophysical constraint.\n\nWho is this for? Someone working on neutron-star magnetospheres or on new ways to bound hadronic CP violation might read it for the pipeline. It deserves a serious referee, not a desk reject, because the framework is novel and the author has flagged most of the red flags themselves. The referee's main job should be to verify whether N_pol can be decoupled from the timing budget, or whether the result should be reframed as a demonstration.","headline":"A novel proof-of-concept for an astrophysical nEDM channel, but the headline bound is 25x weaker than lab and rests on an r_pol prior and a N_pol/spin-down covariance that a referee must probe.","tokens_in":55296,"tokens_out":3049,"would_cite":false,"duration_ms":27949,"reading_group":"maybe","serious_thinker":"yes","would_accept_peer_review":true},"rs_alignment":null,"lean_confirmation":null,"pith_extraction":{"msc":[],"pacs":[],"model":"deepseek-v4-flash","headline":"The spin-down energy budget of PSR J0437-4715 can constrain the neutron's CP-odd moments, yielding a 90th-percentile bound $|M_n^0| < 7.47\\times 10^{-38}\\,e\\,\\mathrm{cm}^2$ and an equivalent $|d_n| < 4.42\\times 10^{-25}\\,e\\,\\mathrm{cm}$.","keywords":["neutron electric dipole moment","CP violation","strong CP problem","millisecond pulsars","PSR J0437-4715","pulsar spin-down","magnetic quadrupole moment","neutron star magnetosphere"],"falsifier":"Recompute the same spin-down budget under an outer freeze-out branch, r_pol > 0.30 R_LC (for example 0.50-0.59 R_LC): the paper's own scaling B_surf proportional to $r_pol^{3}$ raises the field to roughly $10^{9}$-$10^{10}$ G, the modeled magnetic torque exceeds the pulsar's spin-down, and both the electric-dipole-radiation and magnetic-quadrupole bounds disappear. A direct measurement of r_pol from single-pulse polarization-angle sweeps across the OPM transition would decide whether the fiducial branch survives.","tokens_in":53886,"feed_emoji":"🧲","tokens_out":9405,"duration_ms":83959,"temperature":0.7,"pith_summary":"The paper tries to show that a well-measured millisecond pulsar can act as a macroscopic laboratory for the neutron electric dipole moment, a CP-violating quantity that laboratory searches bound directly. Using PSR J0437-4715, it builds a star-specific model: mass and radius from X-ray pulse-profile modeling, a magnetic-field normalization from radio polarization propagation rather than from the standard $P\\dot P$ torque, and a surface geometry from X-ray hot-spot observations. It then subtracts the modeled electromagnetic and gravitational-wave losses from the observed spin-down, interprets the leftover positive power as a CP-odd radiation channel, and converts that into limits. The headline result is a 90th-percentile bound on an effective neutron magnetic quadrupole moment, $|M_n^0| < 7.47\\times 10^{-38}\\,e\\,\\mathrm{cm}^2$, translating to $|\\bar{\\theta}| < 2.99\\times 10^{-9}$ and $|d_n| < 4.42\\times 10^{-25}\\,e\\,\\mathrm{cm}$. The limits are weaker than ultracold-neutron experiments, so the paper's significance is the method: a source-specific energy budget can probe strong-CP physics astrophysically.","feed_headline":"Pulsar spin-down yields nEDM bound of 4.42e-25 e cm","feed_subtitle":"Using PSR J0437-4715's spin-down budget, an MQM channel links residual power to a strong-CP bound.","key_machinery":"The engine is a residual-power identity, $\\Delta = \\dot E_{\\rm int} - L_{\\rm dip} - L_{\\rm GW}$, where the force-free dipolar luminosity $L_{\\rm dip} = \\mu_{\\rm dip}^2\\Omega^4(1+\\sin^2\\alpha)/c^3$ is evaluated from a propagation-informed surface field multiplied by the dipole fraction of a spherical-harmonic decomposition, not from the standard $P\\dot P$ field. The residual is carried by $N_{\\rm pol}$, the number of inner-crust free neutrons weighted by local polarization response, and by the quadrupolar surface-field fraction $f_{\\ell=2} \\simeq 0.18$-$0.23$ obtained from fitting low-order field families to X-ray hot-spot geometry. For the magnetic-quadrupole bound, the radiation formula is $P_{\\rm MQM} = K_{\\rm quad}\\omega_{\\rm rad}^6 (f_{\\ell=2}N_{\\rm pol}M_n^0)^2/c^5$ with $K_{\\rm quad}=1/(60\\pi)$ and $\\omega_{\\rm rad}=2\\pi\\nu_{\\rm OPM}$, where $\\nu_{\\rm OPM}=2.472$-$2.680$ GHz is the frequency at which orthogonal polarization modes merge into a stable high-frequency branch. The polarization-limiting radius prior $r_{\\rm pol} = 0.15$-$0.22\\,R_{\\rm LC}$ carries the field inference through $B_{\\rm surf}\\propto r_{\\rm pol}^3$.","core_discovery":"The central claim is that the present-day spin-down power of PSR J0437-4715, after standard losses are subtracted with a field normalization that does not come from the torque law being tested, leaves a positive residual that any nonstandard CP-odd radiation channel must fit inside. An unscreened assignment to coherent electric-dipole radiation gives the benchmark $|d_n| < 5.783\\times 10^{-25}\\,e\\,\\mathrm{cm}$ at the 90th percentile of the positive branch. Because crustal electrons and magnetospheric plasma screen static electric dipoles, the paper instead promotes a screening-aware channel: an effective neutron magnetic quadrupole moment radiating at the observed orthogonal-polarization-mode transition frequency. With the aligned inner-crust neutron reservoir and the quadrupolar surface-field fraction, the residual gives $|M_n^0| < 7.47\\times 10^{-38}\\,e\\,\\mathrm{cm}^2$; assuming a pure-$\\bar{\\theta}$ origin, this becomes $|\\bar{\\theta}| < 2.99\\times 10^{-9}$ and an equivalent $|d_n| < 4.42\\times 10^{-25}\\,e\\,\\mathrm{cm}$. The paper is explicit that these are conditional, effective bounds, not screening-independent measurements.","pith_inferences":["Editorial extension: since the inferred $d_n$ scales roughly as $\\sqrt{\\Delta}/N_{\\rm pol}$, a better inner-crust microphysical calculation that raises the reliably aligned neutron reservoir has a direct linear payoff, and a factor-of-ten reduction in residual uncertainty would tighten the bound by about a factor of 3.2.","Editorial extension: if future single-pulse polarimetry places $r_{\\rm pol}$ outside the fiducial interval, the paper's own logic says the branches should not be averaged; a physical measurement of the freeze-out radius would select which branch applies.","Editorial extension: applying the same budget to a younger, higher-field star could improve the bound only if the larger aligned-neutron reservoir outgains the larger torque systematics; the paper identifies this as an open question rather than a prediction."],"forward_implications":["If the residual-power logic is right, any well-timed pulsar with independent mass, radius, and field constraints can be audited for nonstandard CP-odd energy losses, not just PSR J0437-4715.","The direct electric-dipole-radiation bound is only as good as the unscreened assumption; under crustal or magnetospheric screening the same spin-down corresponds to a larger microscopic neutron electric dipole moment.","The magnetic-quadrupole channel sidesteps electrostatic Schiff screening, so the MQM bound is the more robust output of the framework.","Because the field posterior scales as $r_{\\rm pol}^3$, constraining the polarization-limiting radius is the single highest-leverage observational step; without it the positive residual can vanish."],"supporting_citations":[{"why":"Supplies the precise spin frequency, spin-period derivative, distance, inclination, and white-dwarf age used for the spin-down budget and kinematic corrections.","marker":"[14]"},{"why":"Provides the NICER-inferred mass and radius plus the hot-region posterior that anchor the structure model and the surface-geometry fit.","marker":"[19]"},{"why":"Provides the emission-altitude ladder for PSR J0437-4715 from which the r_pol = 0.15-0.22 R_LC prior is trimmed.","marker":"[81]"},{"why":"Defines the Goldreich-Julian density n_GJ = Omega B/(2 pi e c) that fixes the pair-plasma density reference in the propagation scaling.","marker":"[79]"},{"why":"Motivates the pair-luminosity prior L_pair ~ 10^-2 L_sd for millisecond pulsars, which sets the pair multiplicity entering the field inference.","marker":"[83]"},{"why":"Supplies the force-free oblique-rotator luminosity formula used to subtract the standard electromagnetic torque from the spin-down budget.","marker":"[58]"},{"why":"Provides the hadronic relation M_n^0 = 2.5e-29 theta_bar e cm^2 that converts the residual power into a neutron magnetic quadrupole moment and a theta_bar value.","marker":"[104]"},{"why":"Provides the pure-theta_bar neutron EDM relation d_n = 1.48e-16 theta_bar e cm used for the equivalent d_n comparison.","marker":"[106]"}],"fun_headline_variants":["Pulsar spin-down sets conditional bound on neutron EDM","Neutron star spin-down probes CP violation beyond Standard Model","Spin-down of PSR J0437-4715 constrains strong CP angle","PSR J0437-4715 spin-down limits neutron EDM to 4e-25 e cm"],"cache_read_input_tokens":3200,"weakest_assumption_plain":"The argument hinges on the assumed polarization-limiting radius: if the radio polarization freezes out farther than about a third of the light-cylinder radius, the inferred magnetic field is large enough that ordinary magnetic-dipole spin-down alone exceeds the pulsar's measured spin-down, wiping out the residual that the bounds are built on.","fun_headline_variants_meta":{"raw":{"variants":["Pulsar spin-down sets conditional bound on neutron EDM","Neutron star spin-down probes CP violation beyond Standard Model","Spin-down of PSR J0437-4715 constrains strong CP angle","PSR J0437-4715 spin-down limits neutron EDM to 4e-25 e cm"]},"model":"deepseek-v4-flash","effort":"low","cost_usd":0.000643,"raw_usage":{"total_tokens":3044,"prompt_tokens":1120,"completion_tokens":1924,"prompt_tokens_details":{"cached_tokens":384},"prompt_cache_hit_tokens":384,"prompt_cache_miss_tokens":736,"completion_tokens_details":{"reasoning_tokens":1839}},"tokens_in":736,"tokens_out":1924,"duration_ms":14435,"temperature":1.0,"reasoning_tokens":1839,"cache_read_input_tokens":384,"cache_creation_input_tokens":0},"cache_creation_input_tokens":0},"created_at":"2026-08-10T04:18:09.620748+00:00","model_set":{"reader":"deepseek-v4-flash"},"falsifier":"Recompute the same spin-down budget under an outer freeze-out branch, r_pol > 0.30 R_LC (for example 0.50-0.59 R_LC): the paper's own scaling B_surf proportional to $r_pol^{3}$ raises the field to roughly $10^{9}$-$10^{10}$ G, the modeled magnetic torque exceeds the pulsar's spin-down, and both the electric-dipole-radiation and magnetic-quadrupole bounds disappear. A direct measurement of r_pol from single-pulse polarization-angle sweeps across the OPM transition would decide whether the fiducial branch survives.","supporting_citations":[{"cited_title":"Millisecond Pulsar Emission Altitude from Relativistic Phase Shift: PSR J0437-4715","cited_arxiv_id":"astro-ph/0604559","evidence_quote":"Provides the emission-altitude ladder for PSR J0437-4715 from which the r_pol = 0.15-0.22 R_LC prior is trimmed."},{"cited_title":"Pulsar Electrodynamics","cited_arxiv_id":null,"evidence_quote":"Defines the Goldreich-Julian density n_GJ = Omega B/(2 pi e c) that fixes the pair-plasma density reference in the propagation scaling."},{"cited_title":"Time-dependent Force-free Pulsar Magnetospheres: Ax- isymmetric and Oblique Rotators","cited_arxiv_id":null,"evidence_quote":"Supplies the force-free oblique-rotator luminosity formula used to subtract the standard electromagnetic torque from the spin-down budget."},{"cited_title":"Time reversal violating Magnetic Quadrupole Moment in heavy deformed nuclei","cited_arxiv_id":"1810.02477","evidence_quote":"Provides the hadronic relation M_n^0 = 2.5e-29 theta_bar e cm^2 that converts the residual power into a neutron magnetic quadrupole moment and a theta_bar value."}],"review_version":1}