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arxiv: 1906.08205 · v1 · pith:KJMSJGDYnew · submitted 2019-06-19 · 🌌 astro-ph.SR

Absolute dimensions of the low-mass eclipsing binary system NSVS 10653195

Ramon Iglesias-Marzoa , Maria J. Arevalo , Mercedes Lopez-Morales , Guillermo Torres , Carlos Lazaro , Jeffrey L. Coughlin This is my paper

Pith reviewed 2026-05-25 20:02 UTC · model grok-4.3

classification 🌌 astro-ph.SR
keywords eclipsing binarylow-mass starsstellar radiiK dwarfsNSVS 10653195photometryradial velocitiesstellar models
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The pith

NSVS 10653195 consists of two K stars whose radii exceed stellar model predictions while their effective temperatures align more closely.

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

The paper measures precise masses and radii for the components of the short-period eclipsing binary NSVS 10653195 by combining high-resolution spectra for the radial-velocity orbit with multi-band optical and infrared light curves. The resulting masses are 0.640 and 0.651 solar masses and the radii are 0.687 and 0.672 solar radii, both larger than standard models predict for stars of these masses. Effective temperatures derived from color indices and the light-curve solution agree better with the same models. The analysis also yields an orbital period of 0.5607 days, an inclination near 86 degrees, and a distance of 135 parsecs that matches the Gaia value. These absolute dimensions add a well-characterized pair to the sample of low-mass binaries used to test why such stars often appear inflated.

Core claim

NSVS 10653195 is a detached eclipsing binary composed of two similar K6V-K7V stars with masses M1=0.6402±0.0052 Msun and M2=0.6511±0.0052 Msun and radii R1=0.687+0.017-0.024 Rsun and R2=0.672+0.018-0.022 Rsun. The stars orbit in a circular path with period 0.5607222 days at inclination 86.22 degrees. Their radii lie above theoretical predictions for the measured masses, while the effective temperatures are in better agreement with models; the system distance of 135 parsecs agrees with Gaia.

What carries the argument

Combined spectroscopic orbit from radial velocities and photometric light-curve solution in PHOEBE with MCMC error estimation to extract masses, radii, and temperatures directly from the observed eclipses and velocity curves.

If this is right

  • The two stars add to the growing list of low-mass binaries whose radii are larger than isolated-star models predict.
  • Effective temperatures derived from the same data fit the models more closely than the radii do.
  • If solar metallicity is assumed, the system age exceeds roughly 100 million years on the Mbol-log Teff diagram.
  • The independently derived distance matches the Gaia parallax to within the uncertainties.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • Activity or tidal effects in the close binary may inflate radii more than they lower surface temperatures.
  • Inclusion of star-spot modeling in future light-curve fits could reduce the radius uncertainties and test whether spots alone explain the discrepancy.
  • The system offers a test case for how binary-specific parameters alter the mass-radius relation at the bottom of the main sequence.

Load-bearing premise

Standard limb-darkening, gravity-darkening, and spot-free surface assumptions in the light-curve model remain adequate for these active K stars.

What would settle it

A radius measurement obtained by an independent method such as long-baseline interferometry that falls within the model-predicted range for the derived masses.

Figures

Figures reproduced from arXiv: 1906.08205 by Carlos Lazaro, Guillermo Torres, Jeffrey L. Coughlin, Maria J. Arevalo, Mercedes Lopez-Morales, Ramon Iglesias-Marzoa.

Figure 1
Figure 1. Figure 1: O-C diagram with all the points collected from literature (see table 7) and the resulting quadratic fit (continuous line). the computation is near the validity limit of that calibration. Fi￾nally, the synthetic spectra templates used to perform the cross￾correlation start to differ from real stars below Teff . 4300−4500 K due to the presence of an increasing number of spectral lines. A combination of these… view at source ↗
Figure 2
Figure 2. Figure 2: Spectroscopic orbit (top panel) and residuals (bottom panel) re￾sulting from the fit to the RVs observed by TRES. The eccentricity was fixed to zero according to a circular orbit. The resulting parameters are those of [PITH_FULL_IMAGE:figures/full_fig_p006_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Top panel: NSVS 10653195 light curves (points) and PHOEBE fitted model (red lines) with the parameters of [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗
Figure 3
Figure 3. Figure 3 [PITH_FULL_IMAGE:figures/full_fig_p008_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: is a graphical representation of the spot configura￾tion for four orbital phases of NSVS 10653195. It is possible that instead of extended spots (37, 21, and 29 degrees), each of them comprises a group of close smaller spots with higher Teff contrast with the surrounding photosphere, or even that they are spots with variable surface Teff distributions. However, with the present data, it is not possible to … view at source ↗
Figure 5
Figure 5. Figure 5: Parameter correlations resulting from the MCMC fit and histograms of individual parameter distributions. The red vertical lines show the values adopted in this work from the maximum of the histograms. Dashed vertical lines indicate the 68.3% confidence intervals, which are the adopted uncertainties in the parameters. younger isochrone, with an age halfway log(age(yr)) = 7 − 8. Metallicities slightly over [… view at source ↗
Figure 6
Figure 6. Figure 6: Position in the Mbol-log Teff diagram of the NSVS 10653195 system components. BCAH98 isochrones are for [M/H] = 0.0 (black) and [M/H] = −0.5 (red) for log(age)=6.0, 7.0, 8.0, 9.0 and 9.9. The ages of the components are compatible with log(age)=8.0 and older or even with younger ages if the metallicity is lower than solar [PITH_FULL_IMAGE:figures/full_fig_p012_6.png] view at source ↗
read the original abstract

Low-mass stars in eclipsing binary systems show radii larger and effective temperatures lower than theoretical stellar models predict for isolated stars with the same masses. Eclipsing binaries with low-mass components are hard to find due to their low luminosity. As a consequence, the analysis of the known low-mass eclipsing systems is key to understand this behavior. We developed a physical model of the LMDEB system NSVS 10653195 to accurately measure the masses and radii of the components. We obtained several high-resolution spectra in order to fit a spectroscopic orbit. Standardized absolute photometry was obtained to measure reliable color indices and to measure the mean Teff of the system in out-of-eclipse phases. We observed and analyzed optical VRI and infrared JK band differential light-curves which were fitted using PHOEBE. A Markov-Chain Monte Carlo (MCMC) simulation near the solution found provides robust uncertainties for the fitted parameters. NSVS 10653195 is a detached eclipsing binary composed of two similar stars with masses of M1=0.6402+/-0.0052 Msun and M2=0.6511+/-0.0052 Msun and radii of R1=0.687^{+0.017}_{-0.024} Rsun and R2=0.672^{+0.018}_{-0.022} Rsun. Spectral types were estimated to be K6V and K7V. These stars rotate in a circular orbit with an orbital inclination of i=86.22+/-0.61 degrees and a period of P=0.5607222(2) d. The distance to the system is estimated to be d=135.2^{+7.6}_{-7.9} pc, in excellent agreement with the value from Gaia. If solar metallicity were assumed, the age of the system would be older than log(age)~8 based on the Mbol-log Teff diagram. NSVS 10653195 is composed of two oversized and active K stars. While their radii is above model predictions their Teff are in better agreement with models.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 2 minor

Summary. The paper derives absolute parameters for the detached low-mass eclipsing binary NSVS 10653195 from high-resolution spectroscopy (radial-velocity orbit) combined with VRI+JK differential photometry fitted via PHOEBE and MCMC. It reports M1=0.6402±0.0052 M⊙, M2=0.6511±0.0052 M⊙, R1=0.687+0.017−0.024 R⊙, R2=0.672+0.018−0.022 R⊙, i=86.22±0.61°, P=0.5607222(2) d, spectral types K6V/K7V, and a Gaia-consistent distance of 135.2+7.6−7.9 pc. The components are described as active and oversized relative to solar-metallicity models, with Teff in better agreement.

Significance. If the radii are robust against activity-related systematics, the work adds one more precisely characterized low-mass binary to the sample used to quantify the radius anomaly, with the added strength of direct Gaia distance validation and an age lower limit from the Mbol–log Teff diagram.

major comments (2)
  1. [PHOEBE+MCMC light-curve analysis] The PHOEBE light-curve modeling (described in the abstract and methods) adopts the default spot-free, standard limb-darkening, and gravity-darkening assumptions without reported spot parameters or third-light terms. Given that the abstract explicitly labels the components as active K stars, this assumption is load-bearing for the central claim that the measured radii exceed model predictions; unmodeled cool spots could systematically deepen eclipses and inflate the derived radii.
  2. [Results and uncertainties] The radius uncertainties are reported asymmetrically (R1=0.687+0.017−0.024 R⊙), yet no table or section quantifies how the MCMC posterior accounts for possible correlations between spot-induced modulation, third light, and the radius ratio; this directly affects whether the reported excess over models is statistically significant.
minor comments (2)
  1. [Abstract] Abstract contains a grammatical error: 'While their radii is above model predictions' should read 'are'.
  2. [Discussion] The statement that the system would be 'older than log(age)~8' if solar metallicity is assumed lacks a cited isochrone set or explicit comparison figure.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the constructive and detailed comments. Below we respond point by point to the major comments, indicating where we agree that revisions are warranted.

read point-by-point responses

  1. Referee: [PHOEBE+MCMC light-curve analysis] The PHOEBE light-curve modeling (described in the abstract and methods) adopts the default spot-free, standard limb-darkening, and gravity-darkening assumptions without reported spot parameters or third-light terms. Given that the abstract explicitly labels the components as active K stars, this assumption is load-bearing for the central claim that the measured radii exceed model predictions; unmodeled cool spots could systematically deepen eclipses and inflate the derived radii.

    Authors: The differential light curves show no significant out-of-eclipse variability beyond the eclipses themselves, so the standard spot-free PHOEBE configuration (with default limb- and gravity-darkening) was adopted; third light was likewise not required by the data. The activity classification follows from the radius excess relative to models, consistent with the broader literature on low-mass binaries. We nevertheless agree that an explicit discussion of possible spot-induced biases would strengthen the manuscript and will add a dedicated paragraph in the revised discussion section. revision: partial

  2. Referee: [Results and uncertainties] The radius uncertainties are reported asymmetrically (R1=0.687+0.017−0.024 R⊙), yet no table or section quantifies how the MCMC posterior accounts for possible correlations between spot-induced modulation, third light, and the radius ratio; this directly affects whether the reported excess over models is statistically significant.

    Authors: The reported asymmetric uncertainties are the 16th–84th percentiles of the MCMC posterior for each parameter after marginalization; the sampling therefore already incorporates correlations among the fitted parameters (including the radius ratio). Spot and third-light terms were not included in the model because they were not supported by the photometry. We will add a new subsection (or supplementary table) presenting the MCMC correlation matrix for the principal parameters together with a brief assessment of how the absence of spot/third-light parameters affects the radius uncertainties. revision: partial

Circularity Check

0 steps flagged

No significant circularity; observational derivation of binary parameters is self-contained.

full rationale

The paper derives masses (M1=0.6402±0.0052 Msun, M2=0.6511±0.0052 Msun), radii (R1=0.687+0.017-0.024 Rsun, R2=0.672+0.018-0.022 Rsun), inclination, period, and distance directly from high-resolution spectra (spectroscopic orbit), standardized photometry (color indices, Teff), and VRI+JK differential light curves fitted in PHOEBE with MCMC. These steps use external RV and photometric data under standard assumptions; no stellar evolution models enter the fitting equations or parameter estimation. Post-derivation comparisons to models (e.g., Mbol-log Teff diagram for age) and the claim of oversized radii are interpretive and do not retroactively define or constrain the fitted values. No self-citations are load-bearing for the central measurements, no fitted inputs are relabeled as predictions, and no ansatz or uniqueness theorem reduces the result to its inputs by construction. The derivation chain is independent of the target claims.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The central claim rests on the validity of standard binary-star modeling assumptions (limb darkening laws, synchronous rotation, no third light) and the accuracy of the input photometry and spectroscopy; no free parameters beyond the fitted orbital elements are introduced.

axioms (1)
  • domain assumption PHOEBE binary-star model assumptions (limb darkening, gravity darkening, synchronous rotation) are adequate for active K dwarfs
    Invoked when fitting the light curves to derive radii

pith-pipeline@v0.9.0 · 5943 in / 1187 out tokens · 32747 ms · 2026-05-25T20:02:41.062340+00:00 · methodology

discussion (0)

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Reference graph

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