Pith. sign in

REVIEW 4 major objections 4 minor 97 references

Pulsating and Non-pulsating Components of Detached Eclipsing Binaries in the $\delta$ Scuti instability strip

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

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗

Pith's one-line read In four detached eclipsing binaries, the metal-rich component is always the non-pulsator, supporting the theory that metallicity damps delta Scuti oscillations.

desk verdict A plausible, well-designed study of four eclipsing binaries with a striking 4/4 metallicity pattern that hinges entirely on ruling out pulsation-biased abundances. read the letter →

arxiv 2508.14464 v1 pith:AAGIMOIB submitted 2025-08-20 astro-ph.SR

Filiz Kahraman Aliçavuş , Fahri Aliçavuş , Zeynep Çelik Orhan , Eda Çelik , Giovanni Catanzaro , Marina Giarrusso This is my paper · ORCID
classification astro-ph.SR
keywords deltaScutistarseclipsingbinariesstellarpulsationmetallicityeffectinstabilitystripspectraldisentanglingTESSphotometryevolution
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 examines four detached eclipsing binaries whose component stars all fall inside the delta Scuti instability strip, a region where stars of a certain mass and temperature are expected to pulsate. In each of the four systems, only one component is observed to pulsate; the other is quiet. Comparing the two components within each binary, the paper finds the distinguishing variable is measured metallicity: the non-pulsating star is systematically metal-richer than its pulsating companion. Because the two stars in a detached binary formed together from the same material, this differential comparison isolates metallicity as the controlling factor. The result supports the theoretical prediction that higher metal abundance damps delta Scuti-type pulsations.

What carries the argument

The key object is the detached eclipsing binary pair used as a controlled astrophysical experiment: two stars born from the same cloud, at the same distance, with the same age, whose orbits allow precise masses and radii. The load-bearing technique is spectral disentangling (or synthetic composite spectra), which separates the blended spectrum of the pair into individual stellar spectra, allowing the iron abundance and other atmospheric parameters of each component to be measured separately.

What would settle it

Re-derive the iron abundance of the pulsating and non-pulsating components of HD 117476, 205 Dra, HY Vir, and V1031 Ori using an independent analysis method (e.g., equivalent widths on disentangled spectra, or a different spectrum synthesis code) and check whether the non-pulsator remains systematically metal-richer. A more direct falsifier would be to find a detached eclipsing binary inside the delta Scuti strip where the metal-rich component pulsates and the metal-poor one does not, or to observe a pulsating component's [Fe/H] changing with pulsation phase, which would indicate the abundance

Watch

Extended reading notes

Core claim

The central claim is that, within a single detached eclipsing binary lying in the delta Scuti instability strip, the component with the higher measured iron abundance is the non-pulsator, while the lower-metallicity component shows delta Scuti oscillations. This pattern holds in all four systems studied: HD 117476, 205 Dra, HY Vir, and V1031 Ori. The paper derives each component's atmospheric parameters through spectral disentangling or synthetic composite spectra, models the light and radial-velocity curves to obtain masses and radii, and identifies the pulsating component with three independent approaches. On the author's argument, the binary arrangement cancels age, distance, and initial

Load-bearing premise

The measured iron-abundance difference between the two components of each binary is real, rather than a systematic error introduced by analyzing the spectrum of a star whose oscillations shift and distort its spectral lines; additionally, both components began with the same initial composition.

Editorial extensions

If this is right

  • If the pattern holds, delta Scuti pulsations should be preferentially found in the lower-metallicity components of binary pairs, and metal-rich field stars inside the instability strip should show suppressed pulsation amplitudes.
  • The precise masses, radii, and pulsation frequencies of these four systems provide empirical benchmarks for stellar models that include metallicity-dependent opacity driving and damping.
  • The result strengthens the use of pulsating eclipsing binaries as asteroseismic testbeds: the non-pulsating companion serves as a built-in control for each pulsator.
  • A larger survey of detached eclipsing binaries with one pulsating component could convert this four-system pattern into a statistical test of metallicity's role.

Reading between the lines

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

  • The same binary-pair comparison could be applied to gamma Doradus or hybrid pulsators to ask whether metallicity plays a similar damping role for other pulsation classes.
  • If the abundance difference is genuine, it implies a physical mechanism—such as atomic diffusion or selective mass loss—must have separated the two components chemically, since both formed from the same birth cloud; the paper does not address this mechanism.
  • A phase-resolved spectroscopic campaign of the pulsating components could check whether the inferred [Fe/H] varies with pulsation phase; if it does, the reported metallicity difference would be an artifact of oscillation-induced line-profile distortion.
  • The metallicity-damping claim could be tested outside binaries by asking whether delta Scuti stars in low-metallicity stellar populations systematically show higher pulsation amplitudes or incidence rates.
Share X Bluesky LinkedIn Reddit HN

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

4 major / 4 minor

Summary. The paper analyzes four detached eclipsing binaries (HD 117476, 205 Dra, HY Vir, V1031 Ori) that show delta Scuti-type oscillations, using TESS photometry, high-resolution spectroscopy, radial-velocity measurements, binary light-curve/RV modeling, and spectral disentangling or synthetic composite spectra. For each system, the authors identify a single pulsating component and report that the non-pulsating component is more metal-rich. They interpret this 4/4 pattern as differential empirical support for the theoretical prediction that higher metallicity damps delta Scuti pulsation in otherwise similar binary components.

Significance. If the reported metallicity pattern is real, the four systems constitute a valuable differential test of metallicity effects on delta Scuti pulsation, since binary components share distance, age, and initial composition. The analysis plan is coherent: three independent pulsation-identification approaches, detailed binary modeling, and per-component atmospheric parameter determination. The study also explicitly targets systems whose components lie in the instability strip, which is an appropriate design. However, the central claim rests on small differential [Fe/H] measurements and on null detections of pulsation in the companions; both need to be demonstrated with quantified uncertainties and detection limits. The paper does not currently provide those, so the key result is not yet established at the level claimed.

major comments (4)
  1. [Abstract] The central claim is that metal-rich components are non-pulsators, but the abstract gives no numerical [Fe/H] values, no error bars, and no significance level for the 4/4 pattern. The paper must report the measured [Fe/H] for each component with uncertainties, the formal significance of each intra-binary difference, and a combined significance across the four systems. Without this, the correlation cannot be evaluated against measurement noise.
  2. [Abstract; spectral analysis (spectral disentangling/synthetic composite spectra)] The main systematic risk is that the abundance analysis of the pulsating component is biased by pulsation-induced line-profile and continuum variations. Delta Scuti oscillations change Teff, log g, and line shapes with phase; if these are not modeled self-consistently in the spectral disentangling or synthetic composite fits, the pulsator's [Fe/H] can be systematically underestimated while the non-pulsating companion is unaffected. This one-sided bias would produce exactly the reported pattern. The paper needs a phase-resolved abundance check, e.g., deriving abundances in separate pulsation phases, or injecting synthetic pulsation signals into the non-pulsating component spectrum to quantify the bias. Without such a test, the central claim is not robust.
  3. [Pulsation identification; 'non-pulsating' components] The designation 'non-pulsating' currently appears to mean 'no pulsations detected' rather than a demonstrated null. The paper must quantify detection thresholds: for each companion, give the noise level in the frequency domain, the significance threshold used, and the upper limit on pulsation amplitude that can be excluded. The 4/4 pattern is only meaningful if the companion amplitudes are constrained to be much smaller than the pulsating components.
  4. [Discussion of component composition] Binary components are generally assumed to form from the same material, so a true [Fe/H] difference between the components of a detached binary is itself a surprising result that requires a physical mechanism (e.g., atomic diffusion, mass transfer history, or external accretion). The paper does not address this expectation or propose such a mechanism. If the measured differences are real, the interpretation in terms of pulsation metallicity dependence is incomplete; if the differences are artifacts, the central conclusion fails. Either way, this issue must be discussed explicitly.
minor comments (4)
  1. [Abstract] The phrase 'the key difference' overstates the result before uncertainties are presented. A more cautious wording, e.g., 'the most notable difference found in our sample,' would better match the evidence level.
  2. [Introduction] The introductory statements about 'supporting theoretical studies' lack specific citations; please name the theoretical works and describe what they predict quantitatively.
  3. [Section on instability strip placement] The 'preliminary investigation' that placed all components in the delta Scuti instability strip should be described with quantitative criteria (e.g., the Teff-log g boundaries used) and a figure or table, so the reader can assess whether the selection biases the sample.
  4. [Throughout] Several LaTeX/typographical artifacts (e.g., 'X Scuti' in the header and abstract) appear in the compiled text; please correct these in the final version.

Circularity Check

0 steps flagged · score 2.0 of 10

No circular derivation: the metal-rich/non-pulsator pattern is an empirical result compared against, not derived from, theoretical metallicity studies.

full rationale

The paper's central claim is an empirical correlation, not a derived prediction. The authors selected four detached eclipsing binaries already known to show delta Scuti oscillations, used TESS photometry and high-resolution spectroscopy (spectral disentangling or synthetic composite spectra) to derive atmospheric parameters and model light/RV curves, and used three approaches to assign pulsation to one component per system. The abstract explicitly frames the theoretical metallicity studies as something the observations 'support,' i.e., an external comparison, not an input. The instability-strip selection ('all binary components of these targets lie within the delta Scuti instability strip') cannot force the pulsation identification because it is common to both components; it only ensures both are in the same pulsation-relevant region. No equation in the provided text defines metallicity in terms of pulsation status or vice versa, and no fitted parameter is relabeled as a prediction. The self-citations in the introduction (Kahraman Aliçavuş et al. 2022a, 2023a) are routine context, not load-bearing. The main fragility is a possible systematic bias from pulsation-phase line-profile distortions affecting the pulsator's inferred [Fe/H], but that is a data-analysis correctness risk, not circular reasoning; no evidence in the text shows the abundance difference is an artifact of the pulsation identification. Score is low, reflecting only minor self-citation and an acknowledged non-circular residual risk.

Assumptions & free parameters 3 free parameters · 4 assumptions · 0 invented entities

The central claim rests almost entirely on the differential metallicity measurement and its interpretation. No new physical entities are introduced; the paper works with known classes (delta Scuti stars, detached eclipsing binaries) and standard parameters. Four background assumptions carry the analysis: unbiased spectral fitting, shared initial composition at birth, the metallicity-damping theory, and the reliability of the pulsation identification. The small number of systems (four) means the empirical pattern has limited statistical weight on its own.

free parameters (3)
  • per-component [Fe/H] for eight stars (four pairs) = not reported in abstract
    The differential metallicities are the quantities the central claim is built on; they are fitted outputs of the synthetic composite spectrum or disentangling analysis, and their error bars and systematics determine whether the pulsator is really metal-poor.
  • binary orbital and physical parameters (mass ratio, inclination, component masses and radii) = not reported in abstract
    Fitted from TESS light curves and radial velocity curves via standard binary modeling; needed to confirm both components lie in the instability strip and to anchor the analysis.
  • pulsation identification thresholds and mode parameters = not reported in abstract
    The three approaches used to label a component pulsating or non-pulsating involve frequency and amplitude criteria; a non-detection threshold determines the non-pulsator label.
assumptions (4)
  • domain assumption Standard 1D/LTE spectral modeling via spectral disentangling or synthetic composite spectra yields unbiased atmospheric parameters for both components.
    Stated in the abstract as the derivation method; if pulsation-driven line-profile variations or non-LTE effects break this, the differential metallicity is biased.
  • domain assumption Both components of each detached binary share the same initial birth composition.
    Standard binary formation assumption; it makes the reported metallicity difference physically surprising and means the difference must arise from surface processes or measurement effects.
  • domain assumption The theoretical instability strip and the opacity-driven models in which higher metallicity damps delta Scuti oscillations are correct.
    The interpretation supporting theoretical studies adopts this theory; it is cited from the literature, not derived in the paper.
  • domain assumption A component labeled non-pulsating truly has no delta Scuti pulsation, meaning amplitude below the detection limit, not merely modes hidden by geometric cancellation or low amplitude.
    Pulsation identification rests on TESS photometry and RV methods; low-amplitude or misaligned modes could be missed, which would weaken the pulsating/non-pulsating dichotomy.

how reviews work

0 comments
Cite this review

Pith. "Pith review of Pulsating and Non-pulsating Components of Detached Eclipsing Binaries in the $\delta$ Scuti instability strip." pith.science (2026). https://pith.science/paper/AAGIMOIB

@misc{pith2026250814464,
  author       = {Pith},
  title        = {Pith review of: Pulsating and Non-pulsating Components of Detached Eclipsing Binaries in the $\delta$ Scuti instability strip},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/AAGIMOIB}},
  note         = {Machine review of arXiv:2508.14464}
}
abstract

Pulsating detached eclipsing binary systems are crucial for studying the internal structure of oscillating stars. These systems are advantageous because binary effects on pulsations are minimal, allowing for more accurate determinations of fundamental stellar parameters such as mass and radius. They serve as unique laboratories for detailed investigations of pulsating stars. In this study, we focused on four detached eclipsing binaries exhibiting $\delta$ Scuti-type oscillations: HD 117476, 205 Dra, HY Vir, and V1031 Ori. Our preliminary investigation showed that all binary components of these targets lie within the $\delta$ Scuti instability strip. Therefore, we aimed to determine which components are pulsating and which are not, and to explore the differences between them. To achieve this, we analyzed TESS photometric data and high-resolution spectra of the targets. Radial velocity variations were measured, and atmospheric parameters for each component were derived using spectral disentangling or synthetic composite spectra. We also modeled the binary light and radial velocity curves to determine the fundamental physical parameters of the components. Furthermore, we examined pulsation properties using three different approaches to identify the pulsating components. The evolutionary status of the targets was also assessed. Our analysis revealed that, in each system, only one component exhibits $\delta$ Scuti-type pulsations, while the others are non-pulsating. Interestingly, we found that the key difference between pulsating and non-pulsating components within the same binary is metallicity: the metal-rich components were found to be non-pulsators, supporting theoretical studies on the effect of metallicity on $\delta$ Scuti-type pulsations.

Discussion (0). Continue with ORCID to comment.

Reference graph

Works this paper leans on

97 extracted references · 30 canonical work pages

  1. [1]

    Adelman, S. J. & Unsuree, N.\ 2007, Baltic Astronomy, 16, 183

    2007

  2. [2]

    Am \^o res, E. B. & L \'e pine, J. R. D.\ 2005, , 130, 2, 659. doi:10.1086/430957

    doi:10.1086/430957 2005

  3. [3]

    V., & Nordstrom, B.\ 1990, , 228, 365

    Andersen, J., Clausen, J. V., & Nordstrom, B.\ 1990, , 228, 365

    1990

  4. [4]

    doi:10.1088/0004-637X/796/2/118

    Antoci, V., Cunha, M., Houdek, G., et al.\ 2014, , The Role of Turbulent Pressure as a Coherent Pulsational Driving Mechanism: The Case of the Scuti Star HD 187547, 796, 2, 118. doi:10.1088/0004-637X/796/2/118

    doi:10.1088/0004-637x/796/2/118 2014

  5. [5]

    S., Bowman, D

    Antoci, V., Cunha, M. S., Bowman, D. M., et al.\ 2019, , The first view of Scuti and Doradus stars with the TESS mission, 490, 3, 4040. doi:10.1093/mnras/stz2787

    doi:10.1093/mnras/stz2787 2019

  6. [6]

    J., et al.\ 2009, , The Chemical Composition of the Sun, 47, 1, 481

    Asplund, M., Grevesse, N., Sauval, A. J., et al.\ 2009, , The Chemical Composition of the Sun, 47, 1, 481. doi:10.1146/annurev.astro.46.060407.145222

    arXiv 2009

  7. [7]

    Baran, A. S. & Koen, C.\ 2021, , A Detection Threshold in the Amplitude Spectra Calculated from TESS Time-Series Data, 71, 2, 113. doi:10.32023/0001-5237/71.2.3

    doi:10.32023/0001-5237/71.2.3 2021

  8. [8]

    doi:10.1088/0004-6256/145/5/132

    Chang, S.-W., Protopapas, P., Kim, D.-W., et al.\ 2013, , Statistical Properties of Galactic Scuti Stars: Revisited, 145, 5, 132. doi:10.1088/0004-6256/145/5/132

    doi:10.1088/0004-6256/145/5/132 2013

Show all 97 references
  1. [9]

    H.\ 2004, , Balmer lines as T _ eff and log g indicators for non-solar composition atmospheres

    Catanzaro, G., Leone, F., & Dall, T. H.\ 2004, , Balmer lines as T _ eff and log g indicators for non-solar composition atmospheres. An application to the extremely helium-weak star HR 6000, 425, 641. doi:10.1051/0004-6361:20040558

    2004 doi

  2. [10]

    doi:10.1093/mnras/stz080

    Catanzaro, G., Bus \`a , I., Gangi, M., et al.\ 2019, , The behaviour of chemical elements in 62 Am star candidates, 484, 2, 2530. doi:10.1093/mnras/stz080

    2019 doi

  3. [11]

    doi:10.1093/mnras/stz1312

    Catanzaro, G., Gangi, M., Giarrusso, M., et al.\ 2019, , HD 226766: a hierarchical SB3 system with two twin Am stars, 487, 1, 919. doi:10.1093/mnras/stz1312

    2019 doi

  4. [12]

    doi:10.1051/0004-6361/202449332

    Catanzaro, G., Frasca, A., Alonso-Santiago, J., et al.\ 2024, , TESS photometry and CAOS spectroscopy of six eclipsing binaries with Am components, 685, A133. doi:10.1051/0004-6361/202449332

    2024 doi

  5. [13]

    doi:10.3847/1538-4365/aca284

    Chen, X., Ding, X., Cheng, L., et al.\ 2022, , Detection of Scuti Pulsators in the Eclipsing Binaries Observed by TESS, 263, 2, 34. doi:10.3847/1538-4365/aca284

    2022 doi

  6. [14]

    N.\ 2000, , Allen's astrophysical quantities

    Cox, A. N.\ 2000, , Allen's astrophysical quantities

    2000

  7. [15]

    Dupret, M.-A., Grigahc \`e ne, A., Garrido, R., et al.\ 2005, , Convection-pulsation coupling. II. Excitation and stabilization mechanisms in Sct and Dor stars, 435, 3, 927. doi:10.1051/0004-6361:20041817

    2005 doi

  8. [16]

    doi:10.1051/0004-6361/202349076

    D \"u rfeldt-Pedros, O., Antoci, V., Smalley, B., et al.\ 2024, , Variability and stellar pulsation incidence in Am and Fm stars using TESS and Gaia data, 690, A104. doi:10.1051/0004-6361/202349076

    2024 doi

  9. [17]

    doi:10.1093/mnras/staa1659

    Eker, Z., Soydugan, F., Bilir, S., et al.\ 2020, , Empirical bolometric correction coefficients for nearby main-sequence stars in the Gaia era, 496, 3, 3887. doi:10.1093/mnras/staa1659

    2020 doi

  10. [18]

    G., Kurtz, D

    Elkin, V. G., Kurtz, D. W., & Nitschelm, C.\ 2012, , Magnetic stars from a FEROS cool Ap star survey, 420, 3, 2727. doi:10.1111/j.1365-2966.2011.20253.x

    2012

  11. [19]

    & North, P.\ 2003, , 398, 1121

    Erspamer, D. & North, P.\ 2003, , 398, 1121. doi:10.1051/0004-6361:20021711

    2003 doi

  12. [20]

    Eze, C. I. & Handler, G.\ 2024, , Cephei Pulsators in Eclipsing Binaries Observed with TESS, 272, 2, 25. doi:10.3847/1538-4365/ad39c5

    2024 doi

  13. [21]

    S.\ 1981, , L=0, 1, 2, and 3 pulsation constants for evolutionary models of del SCT stars., 249, 218

    Fitch, W. S.\ 1981, , L=0, 1, 2, and 3 pulsation constants for evolutionary models of del SCT stars., 249, 218. doi:10.1086/159278

    1981 doi

  14. [22]

    Fossati, L., Bagnulo, S., Monier, R., et al.\ 2008, Contributions of the Astronomical Observatory Skalnate Pleso, 38, 2, 123

    2008

  15. [23]

    doi:10.1051/0004-6361/200811561

    Fossati, L., Ryabchikova, T., Bagnulo, S., et al.\ 2009, , 503, 3, 945. doi:10.1051/0004-6361/200811561

    2009 doi

  16. [24]

    F.\ 2005,

    Gray, D. F.\ 2005, . doi:10.1017/CBO9781316036570

    2005 doi

  17. [25]

    doi:10.1051/0004-6361/200913273

    Gebran, M., Vick, M., Monier, R., et al.\ 2010, , 523, A71. doi:10.1051/0004-6361/200913273

    2010 doi

  18. [26]

    doi:10.1051/0004-6361/202244122

    Graczyk, D., Pietrzy \'n ski, G., Galan, C., et al.\ 2022, , 666, A128. doi:10.1051/0004-6361/202244122

    2022 doi

  19. [27]

    doi:10.1016/j.newast.2023.102161

    G \"u rol, B.\ 2024, , BD UMi: Eccentric detached binary with Doradus type component, 107, 102161. doi:10.1016/j.newast.2023.102161

    2024

  20. [28]

    A., Bradley, P

    Guzik, J. A., Bradley, P. A., Jackiewicz, J., et al.\ 2015, The Astronomical Review, The occurrence of non-pulsating stars in the Dor and Sct pulsation instability regions: results from Kepler quarter 14-17 data, 11, 1, 1. doi:10.1080/21672857.2015.1023120

    2015

  21. [29]

    W., Rappaport, S

    Handler, G., Kurtz, D. W., Rappaport, S. A., et al.\ 2020, Nature Astronomy, Tidally trapped pulsations in a close binary star system discovered by TESS, 4, 684. doi:10.1038/s41550-020-1035-1

    2020 doi

  22. [30]

    G., Olszewska, J

    He miniak, K. G., Olszewska, J. M., Puciata-Mroczynska, M., et al.\ 2024, , 691, A170. doi:10.1051/0004-6361/202450607

    2024 doi

  23. [31]

    doi:10.1086/682056

    Iglesias-Marzoa, R., L \'o pez-Morales, M., & Jes \'u s Ar \'e valo Morales, M.\ 2015, , The rvfit Code: A Detailed Adaptive Simulated Annealing Code for Fitting Binaries and Exoplanets Radial Velocities, 127, 952, 567. doi:10.1086/682056

    2015 doi

  24. [32]

    Ilijic, S., Hensberge, H., Pavlovski, K., et al.\ 2004, Spectroscopically and Spatially Resolving the Components of the Close Binary Stars, Obtaining normalised component spectra with FDBinary, 318, 111

    2004

  25. [33]

    G., et al.\ 2024, , Single-lined eclipsing binaries with Scuti components: GQ Dra, RR Lep, and TYC 683-640-1, 527, 2, 4076

    Kahraman Ali c avu s , F., Ali c avu s , F., C oban, C . G., et al.\ 2024, , Single-lined eclipsing binaries with Scuti components: GQ Dra, RR Lep, and TYC 683-640-1, 527, 2, 4076. doi:10.1093/mnras/stad3467

    2024 doi

  26. [34]

    G., C elik, E., et al.\ 2023, , Discovery of delta Scuti variables in eclipsing binary systems II

    Kahraman Ali c avu s , F., C oban, C . G., C elik, E., et al.\ 2023, , Discovery of delta Scuti variables in eclipsing binary systems II. Southern TESS field search, 524, 1, 619. doi:10.1093/mnras/stad1898

    2023 doi

  27. [35]

    G., et al.\ 2023, , Comprehensive spectroscopic and photometric study of pulsating eclipsing binary star AI Hya, 520, 2, 1601

    Kahraman Ali c avu s , F., Pawar, T., He miniak, K. G., et al.\ 2023, , Comprehensive spectroscopic and photometric study of pulsating eclipsing binary star AI Hya, 520, 2, 1601. doi:10.1093/mnras/stad137

    2023 doi

  28. [36]

    doi:10.1093/mnras/stab3515

    Kahraman Ali c avu s , F., Handler, G., Ali c avu s , F., et al.\ 2022, , Mass transfer and tidally tilted pulsation in the Algol-type system TZ Dra, 510, 1, 1413. doi:10.1093/mnras/stab3515

    2022 doi

  29. [37]

    u m \"u s , D., K rm z ta s , \

    Kahraman Ali c avu s , F., G \"u m \"u s , D., K rm z ta s , \"O ., et al.\ 2022, Research in Astronomy and Astrophysics, Candidate Eclipsing Binary Systems with a Scuti Star in Northern TESS Field, 22, 8, 085003. doi:10.1088/1674-4527/ac71a4

    2022 doi

  30. [38]

    & Ali c avu s , F.\ 2020, Research in Astronomy and Astrophysics, The evolutionary status of chemically peculiar eclipsing binary star DV Boo, 20, 9, 150

    Kahraman Ali c avu s , F. & Ali c avu s , F.\ 2020, Research in Astronomy and Astrophysics, The evolutionary status of chemically peculiar eclipsing binary star DV Boo, 20, 9, 150. doi:10.1088/1674-4527/20/9/150

    2020 doi

  31. [39]

    doi:10.1093/mnras/stx1241

    Kahraman Ali c avu s , F., Soydugan, E., Smalley, B., et al.\ 2017, , Eclipsing binary stars with a Scuti component, 470, 1, 915. doi:10.1093/mnras/stx1241

    2017 doi

  32. [40]

    Comprehensive atmospheric parameters and abundance analysis of Doradus stars, 458, 3, 2307

    Kahraman Ali c avu s , F., Niemczura, E., De Cat, P., et al.\ 2016, , Spectroscopic survey of Doradus stars - I. Comprehensive atmospheric parameters and abundance analysis of Doradus stars, 458, 3, 2307. doi:10.1093/mnras/stw393

    2016 doi

  33. [41]

    M.\ 2004, , Up-to-Date Linear Elements of Eclipsing Binaries, 54, 207

    Kreiner, J. M.\ 2004, , Up-to-Date Linear Elements of Eclipsing Binaries, 54, 207

    2004

  34. [42]

    W.\ 1976, , Metallicism and pulsation: an analysis of the Delta Delphini stars., 32, 651

    Kurtz, D. W.\ 1976, , Metallicism and pulsation: an analysis of the Delta Delphini stars., 32, 651. doi:10.1086/190411

    1976 doi

  35. [43]

    doi:10.48550/arXiv.2201.11629

    Kurtz, D.\ 2022, Annual Conference and General Assembly of the, 1. doi:10.48550/arXiv.2201.11629

    2022 doi arXiv

  36. [44]

    Kurucz, R. L. & Avrett, E. H.\ 1981, SAO Special Report, Solar Spectrum Synthesis. I. A Sample Atlas from 224 to 300 nm, 391

    1981

  37. [45]

    Kurucz, R.\ 1993, Robert Kurucz CD-ROM, ATLAS9 Stellar Atmosphere Programs and 2 km/s grid., 13

    1993

  38. [46]

    E., Sajina, A., et al.\ 2015, , The Spitzer Mid-infrared AGN Survey

    Lacy, M., Ridgway, S. E., Sajina, A., et al.\ 2015, , The Spitzer Mid-infrared AGN Survey. II. The Demographics and Cosmic Evolution of the AGN Population, 802, 2, 102. doi:10.1088/0004-637X/802/2/102

    2015 doi

  39. [47]

    W.\ 2021, , Tidally perturbed oblique pulsations in the hierarchical triple system V1031 Orionis, 73, 4, 809

    Lee, J. W.\ 2021, , Tidally perturbed oblique pulsations in the hierarchical triple system V1031 Orionis, 73, 4, 809. doi:10.1093/pasj/psab044

    2021 doi

  40. [48]

    & Breger, M.\ 2005, Communications in Asteroseismology, Period04 User Guide, 146, 53

    Lenz, P. & Breger, M.\ 2005, Communications in Asteroseismology, Period04 User Guide, 146, 53. doi:10.1553/cia146s53

    2005 doi

  41. [49]

    doi:10.3847/0004-6256/151/5/116

    Leone, F., Avila, G., Bellassai, G., et al.\ 2016, , A Method to Calibrate the High-resolution Catania Astrophysical Observatory Spectropolarimeter, 151, 5, 116. doi:10.3847/0004-6256/151/5/116

    2016 doi

  42. [50]

    B.\ 1967, , 65, 89

    Lucy, L. B.\ 1967, , 65, 89

    1967

  43. [51]

    G., Ar \'e valo, M

    Mart \' nez-Pais, I. G., Ar \'e valo, M. J., & L \'a zaro, C.\ 2008, , Absolute parameters of the short-period binary HY Virginis from JHK light curves and spectroscopy, 13, 5, 304. doi:10.1016/j.newast.2007.11.001

    2008 doi

  44. [52]

    Mayor, M., Pepe, F., Queloz, D., et al.\ 2003, The Messenger, Setting New Standards with HARPS, 114, 20

    2003

  45. [53]

    Montgomery, M. H. & O'Donoghue, D.\ 1999, Delta Scuti Star Newsletter, vol. 13, p.28, A derivation of the errors for least squares fitting to time series data, 13, 28

    1999

  46. [54]

    J., Hey, D., Van Reeth, T., et al.\ 2019, , Gaia-derived luminosities of Kepler A/F stars and the pulsator fraction across the Scuti instability strip, 485, 2, 2380

    Murphy, S. J., Hey, D., Van Reeth, T., et al.\ 2019, , Gaia-derived luminosities of Kepler A/F stars and the pulsator fraction across the Scuti instability strip, 485, 2, 2380. doi:10.1093/mnras/stz590

    2019 doi

  47. [55]

    doi:10.1007/978-3-319-06956-2

    Niemczura, E., Smalley, B., & Pych, W.\ 2014, , Determination of Atmospheric Parameters of B-, A-, F- and G-Type Stars. doi:10.1007/978-3-319-06956-2

    2014 doi

  48. [56]

    doi:10.1088/0067-0049/192/1/3

    Paxton, B., Bildsten, L., Dotter, A., et al.\ 2011, , Modules for Experiments in Stellar Astrophysics (MESA), 192, 1, 3. doi:10.1088/0067-0049/192/1/3

    2011 doi

  49. [57]

    doi:10.1088/0067-0049/208/1/4

    Paxton, B., Cantiello, M., Arras, P., et al.\ 2013, , Modules for Experiments in Stellar Astrophysics (MESA): Planets, Oscillations, Rotation, and Massive Stars, 208, 1, 4. doi:10.1088/0067-0049/208/1/4

    2013 doi

  50. [58]

    doi:10.1088/0067-0049/220/1/15

    Paxton, B., Marchant, P., Schwab, J., et al.\ 2015, , Modules for Experiments in Stellar Astrophysics (MESA): Binaries, Pulsations, and Explosions, 220, 1, 15. doi:10.1088/0067-0049/220/1/15

    2015 doi

  51. [59]

    & Hensberge, H.\ 2010, Binaries - Key to Comprehension of the Universe, 435, 207

    Pavlovski, K. & Hensberge, H.\ 2010, Binaries - Key to Comprehension of the Universe, 435, 207. doi:10.48550/arXiv.0909.3246

    2010 doi arXiv

  52. [60]

    Accurate fundamental properties and surface chemical composition for V1034 Sco, GL Car, V573 Car, and V346 Cen, 671, A139

    Pavlovski, K., Southworth, J., Tkachenko, A., et al.\ 2023, , High-mass eclipsing binaries: A testbed for models of interior structure and evolution. Accurate fundamental properties and surface chemical composition for V1034 Sco, GL Car, V573 Car, and V346 Cen, 671, A139. doi:...

    2023 doi

  53. [61]

    B., Miszuda, A., He miniak, K

    Pawar, T. B., Miszuda, A., He miniak, K. G., et al.\ 2025, , arXiv:2502.20626. doi:10.48550/arXiv.2502.20626

    2025 doi

  54. [62]

    G., Moharana A., Pawar G., Pyatnytskyy M., Lala H

    Pawar T., He miniak K. G., Moharana A., Pawar G., Pyatnytskyy M., Lala H. N., Konacki M., 2024, A&A, 691, A101. doi:10.1051/0004-6361/202451126

    2024 doi

  55. [63]

    E., et al.\ 2022, , TESS Eclipsing Binary Stars

    Pr s a, A., Kochoska, A., Conroy, K. E., et al.\ 2022, , TESS Eclipsing Binary Stars. I. Short-cadence Observations of 4584 Eclipsing Binaries in Sectors 1-26, 258, 1, 16. doi:10.3847/1538-4365/ac324a

    2022 doi

  56. [64]

    A., Kurtz, D

    Rappaport, S. A., Kurtz, D. W., Handler, G., et al.\ 2021, , A tidally tilted sectoral dipole pulsation mode in the eclipsing binary TIC 63328020, 503, 1, 254. doi:10.1093/mnras/stab336

    2021 doi

  57. [65]

    doi:10.1051/0004-6361/201015435

    Raskin, G., van Winckel, H., Hensberge, H., et al.\ 2011, , HERMES: a high-resolution fibre-fed spectrograph for the Mercator telescope, 526, A69. doi:10.1051/0004-6361/201015435

    2011 doi

  58. [66]

    R., Winn, J

    Ricker, G. R., Winn, J. N., Vanderspek, R., et al.\ 2014, , Transiting Exoplanet Survey Satellite (TESS), 9143, 914320. doi:10.1117/12.2063489

    2014 doi

  59. [67]

    Rogers, F. J. & Nayfonov, A.\ 2002, , Updated and Expanded OPAL Equation-of-State Tables: Implications for Helioseismology, 576, 2, 1064. doi:10.1086/341894

    2002 doi

  60. [68]

    Rosanski, T., Niemczura, E., & Posilek, N.\ 2022, Astronomical Data Analysis Software and Systems XXX, Neural Network for Stellar Spectrum Normalization, 532, 251

    2022

  61. [69]

    M.\ 1969, , The Proximity Effects in Close Binary Systems

    Ruci \'n ski, S. M.\ 1969, , The Proximity Effects in Close Binary Systems. II. The Bolometric Reflection Effect for Stars with Deep Convective Envelopes, 19, 245

    1969

  62. [70]

    doi:10.1093/mnras/stae2258

    Sarkar, M., Joshi, S., Dupret, M.-A., et al.\ 2024, , Asteroseismology of the mild Am Sct star HD 118660: TESS photometry and modelling, 534, 4, 3211. doi:10.1093/mnras/stae2258

    2024 doi

  63. [71]

    Sandberg Lacy, C. H. & Fekel, F. C.\ 2011, , Absolute Properties of the Eclipsing Binary Star HY Virginis, 142, 6, 185. doi:10.1088/0004-6256/142/6/185

    2011 doi

  64. [72]

    Simon, K. P. & Sturm, E.\ 1994, , 281, 286

    1994

  65. [73]

    L., et al.\ 2017, , 465, 3, 2662

    Smalley, B., Antoci, V., Holdsworth, D. L., et al.\ 2017, , 465, 3, 2662. doi:10.1093/mnras/stw2903

    2017 doi

  66. [75]

    doi:10.1051/0004-6361/201322195

    Southworth, J.\ 2013, , The solar-type eclipsing binary system LL Aquarii, 557, A119. doi:10.1051/0004-6361/201322195

    2013 doi

  67. [76]

    doi:10.48550/arXiv.1411.1219

    Southworth, J.\ 2015, Living Together: Planets, Host Stars and Binaries, DEBCat: A Catalog of Detached Eclipsing Binary Stars, 496, 164. doi:10.48550/arXiv.1411.1219

    2015 doi arXiv

  68. [77]

    Paper 1: the totally-eclipsing B-type system zeta Phoenicis, 140, 247

    Southworth, J.\ 2020, The Observatory, Rediscussion of eclipsing binaries. Paper 1: the totally-eclipsing B-type system zeta Phoenicis, 140, 247. doi:10.48550/arXiv.2012.05559

    2020 doi arXiv

  69. [78]

    doi:10.3390/universe7100369

    Southworth, J.\ 2021, Universe, 7, 10, 369. doi:10.3390/universe7100369

    2021 doi

  70. [79]

    & Bowman, D

    Southworth, J. & Bowman, D. M.\ 2022, The Observatory, 142, 161. doi:10.48550/arXiv.2205.08841

    2022 doi arXiv

  71. [80]

    M., 2022, MNRAS, 513, 3191

    Southworth J., Bowman D. M., 2022, MNRAS, 513, 3191. doi:10.1093/mnras/stac875

    2022 doi

  72. [81]

    & Van Reeth, T.\ 2022, , 515, 2, 2755

    Southworth, J. & Van Reeth, T.\ 2022, , 515, 2, 2755. doi:10.1093/mnras/stac1993

    2022 doi

  73. [82]

    G., Oelkers, R

    Stassun, K. G., Oelkers, R. J., Paegert, M., et al.\ 2019, , The Revised TESS Input Catalog and Candidate Target List, 158, 4, 138. doi:10.3847/1538-3881/ab3467

    2019 doi

  74. [83]

    doi:10.1093/mnras/stz449

    Takeda, Y., Han, I., Kang, D.-I., et al.\ 2019, , 485, 1, 1067. doi:10.1093/mnras/stz449

    2019 doi

  75. [84]

    TESS Science Office (2020), TESS‑SPOC FFI Light Curves, Accessed on 2025‑08‑01, MAST, doi:10.17909/t9‑wpz1‑8s54

    2020 doi

  76. [85]

    doi:10.1117/12.968154

    Tody, D.\ 1986, , The IRAF Data Reduction and Analysis System, 627, 733. doi:10.1117/12.968154

    1986 doi

  77. [86]

    doi:10.1007/s00159-009-0025-1

    Torres, G., Andersen, J., & Gim \'e nez, A.\ 2010, , 18, 1-2, 67. doi:10.1007/s00159-009-0025-1

    2010 doi

  78. [87]

    Townsend, R. H. D. & Teitler, S. A.\ 2013, , GYRE: an open-source stellar oscillation code based on a new Magnus Multiple Shooting scheme, 435, 4, 3406. doi:10.1093/mnras/stt1533

    2013 doi

  79. [88]

    Townsend, R. H. D., Goldstein, J., & Zweibel, E. G.\ 2018, , Angular momentum transport by heat-driven g-modes in slowly pulsating B stars, 475, 1, 879. doi:10.1093/mnras/stx3142

    2018 doi

  80. [89]

    doi:10.48550/arXiv.astro-ph/0006272

    Turcotte, S., Richer, J., Michaud, G., et al.\ 2000, , The effect of diffusion on pulsations of stars on the upper main sequence --- Scuti and metallic A stars, 360, 603. doi:10.48550/arXiv.astro-ph/0006272

    2000 doi arXiv

  81. [90]

    Uytterhoeven, K., Moya, A., Grigahc \`e ne, A., et al.\ 2011, , The Kepler characterization of the variability among A- and F-type stars. I. General overview, 534, A125. doi:10.1051/0004-6361/201117368

    2011 doi

  82. [91]

    doi:10.1111/j.1365-2966.2005.08921.x

    Yushchenko, A., Gopka, V., Kim, C., et al.\ 2005, , 359, 3, 865. doi:10.1111/j.1365-2966.2005.08921.x

    2005

  83. [92]

    Wilson, R. E. & Devinney, E. J.\ 1971, , Realization of Accurate Close-Binary Light Curves: Application to MR Cygni, 166, 605. doi:10.1086/150986

    1971 doi

  84. [93]

    doi:10.1086/116788

    van Hamme, W.\ 1993, , New Limb-Darkening Coefficients for Modeling Binary Star Light Curves, 106, 2096. doi:10.1086/116788

    1993 doi

  85. [94]

    doi:10.1093/mnras/84.9.665

    von Zeipel, H.\ 1924, , The radiative equilibrium of a rotating system of gaseous masses, 84, 665. doi:10.1093/mnras/84.9.665

    1924 doi

  86. [95]

    V., Gopka, V

    Yushchenko, A. V., Gopka, V. F., Kang, Y.-W., et al.\ 2015, , The Chemical Composition of Puppis and the Signs of Accretion in the Atmospheres of B-F-Type Stars, 149, 2, 59. doi:10.1088/0004-6256/149/2/59

    2015 doi

  87. [96]

    M., Baran, A., et al.\ 2004, , Physical Parameters of Components in Close Binary Systems: III, 54, 299

    Zola, S., Rucinski, S. M., Baran, A., et al.\ 2004, , Physical Parameters of Components in Close Binary Systems: III, 54, 299

    2004

  88. [97]

    M., et al.\ 2010, , Physical parameters of components in close binary systems - VII, 408, 1, 464

    Zola, S., Gazeas, K., Kreiner, J. M., et al.\ 2010, , Physical parameters of components in close binary systems - VII, 408, 1, 464. doi:10.1111/j.1365-2966.2010.17129.x

    2010

  89. [98]

    oeQ!s8W#lrrW0!qYgEorV?Huqu?Nls7lWmq>UHnrVlrqs8D`m

    thebibliography [1] 20pt to REFERENCES 6pt =0pt \@twocolumntrue 12pt -12pt 10pt plus 3pt =0pt =0pt =1pt plus 1pt =0pt =0pt -12pt =13pt plus 1pt =20pt =13pt plus 1pt \@M =10000 =-1.0em =0pt =0pt 0pt =0pt =1.0em @enumiv\@empty 10000 10000 `\.\@m \@noitemerr \@latex@warning Empty...

    2017

Pith tools

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