Pulse profile modeling of XTE J1814-338's thermonuclear burst oscillations yields a radius near 7 km and a mass near 1.2 solar masses
Assessment
The evidence, examined directly, establishes the claim.
Kini and collaborators applied the X-PSI pulse-profile modeling code to the thermonuclear burst oscillations observed during XTE J1814-338's 2003 RXTE outburst and reported an equatorial radius of 7.0 ± 0.4 km, a mass of 1.21 ± 0.05 solar masses, and a distance of about 7.2 kpc (MNRAS 535, 1507, 2024). The reported values are exactly as the claim states, and subsequent papers on the object consistently cite the same numbers.
Two qualifications matter for how the result should be read. The analysis assumes a single uniform-temperature hotspot adequately describes the oscillations, and the authors themselves flag this assumption, together with the treatment of the non-burst emission, as a significant source of systematic uncertainty, so the quoted error bars are statistical and conditional on the model. The result also sits in sharp tension with earlier pulse-shape modeling of the same star's accretion-powered pulsations, which indicated a radius of roughly 12 to 22 km. Whether the star truly is as compact as 7 km, which would challenge conventional neutron star models, is a separate and contested question; what is established here is that the burst-oscillation pulse-profile analysis produced these values.
Full reasoning: the evidence and decisions behind this verdict
The verdict rests on direct reading of the primary source. The conclusion of Kini et al. 2024 (arxiv.org/abs/2405.10717, published as MNRAS 535, 1507, academic.oup.com/mnras/article/535/2/1507/7829277) states the analysis yielded a mass of 1.21 (+0.05/-0.05) solar masses, a radius of 7.0 (+0.4/-0.4) km, and a distance of 7.2 (+0.3/-0.4) kpc, from X-PSI pulse-profile modeling of the 28 bursts with oscillations detected during the 2003 outburst, under a single uniform-temperature hotspot model. The ADS abstract record and multiple independent citing papers (the core-corona analysis at arxiv.org/abs/2506.10032, the hybrid-star paper at arxiv.org/abs/2410.18498, and a dark-matter-admixed strange star paper in Astrophysics and Space Science) quote identical values, so there is no sign of an erratum or revision. All recorded source instances affirm; none deny.
The adversarial reading considered was whether "yields" overstates robustness: the values are conditional on the modeling assumptions, and the subclaim that the single-hotspot model adequately describes the pulse profiles for mass-radius inference is genuinely open, with the original authors flagging it and follow-up pulse-profile work on 4U 1636-536 (arxiv.org/abs/2506.03033) showing background assumptions directly constrain inferred compactness. That subclaim enters as a framing assumption rather than a premise whose failure would falsify the claim: even if the model proves inadequate, the analysis still produced these numbers; what would fail is their interpretation as the star's true properties, which is the business of the parent claim. No published re-analysis of this source with alternative assumptions yet exists; if one appears and yields materially different values, the claim's wording ("pulse profile modeling ... yields") would need revisiting, since the yield would then be shown to be assumption-specific rather than generic to the technique. Credence 0.97 reflects the small residual chance of a misreading or unnoticed correction, not any live dispute.
Decomposition
The claims this one rests on directly. ↗︎ opens a subclaim; the map shows how they fit together.
The claims this one rests on directly, not gathered into a named line of reasoning.
- assumesbackground the parent's framing takes as givensteward instructions →The single uniform-temperature hotspot model adequately describes XTE J1814-338's burst oscillation pulse profiles for mass-radius inference ↗︎
Provenance
Where this claim has been said, linked to its canonical form.
Our analysis yielded the following results for XTE J1814–338: a mass of $1.21^{+0.05}_{-0.05}~M_{\odot}$, a radius of $7.0^{+0.4}_{-0.4}~km$, and a distance of $7.2^{+0.3}_{-0.4}~kpc$.
The primary analysis: applying the X-PSI pulse-profile modeling code to burst oscillations from XTE J1814-338's 2003 RXTE outburst under a single uniform-temperature hotspot model, and reporting the inferred mass, radius, and distance in the conclusion.
A recent analysis on the properties of the XTE J1814-338 pulsar yielded a small radius value around ~ 7 km. Notably, this estimation is significantly lower compared to the currently inferred values for the radius of neutron stars.
A paper proposing hybrid-star equations of state to explain the object; it asserts the recent ~7 km radius yield as the empirical starting point of its analysis.
The recent work of Kini et al. [17], using pulse profile modeling technique to investigate the thermonuclear burst variations from accreting NSs has revealed a striking mass (M) and radius (R) measurement for XTE J1814-338 pulsar.
A theory paper modeling XTE J1814-338 as a dark-matter-admixed neutron star; it opens by asserting the Kini et al. pulse-profile-modeling mass and radius measurement (M = 1.21 solar masses, R = 7.0 km) as the observational input its models must accommodate.
In this paper, I discuss the macroscopic properties of the ultracompact object XTE J1814-338, whose inferred mass and radius read M = 1.21 ± 0.05 M⊙ and R = 7.0 ± 0.4 km, as a dark matter-admixed strange star.
A theory paper treating the object as a dark-matter-admixed strange star; it asserts the inferred mass and radius values as the observational input it models.
The pulse-profile modeling of the accretion-powered millisecond pulsar XTE J1814-338 by a single uniform-temperature hot-spot resulted in mass (M) and radius (R) parameters of $(R/\text{km}, M/M_{\odot}) = (7.0^{+0.4}_{-0.4}, 1.21^{+0.05}_{-0.05})$ [1].
A theory paper motivated by the measurement: it opens by asserting the pulse-profile modeling result and then explores core-corona models that could accommodate so compact a star.
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