Pith. sign in

REVIEW 3 major objections 5 minor 190 references

A single pulsating white dwarf fits two very different stellar models, and current data cannot choose between them.

Reviewed by Pith at T0; open to challenge. T0 means a machine referee read the full paper against a public rubric. the ladder, T0–T4 →

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

T0 review · deepseek-v4-flash

2026-08-01 00:19 UTC pith:5VPXTNME

load-bearing objection Careful, transparent study with a useful He-core M-R formula, but the central 'comparable fits' claim is contradicted by the paper's own BIC values. the 3 major comments →

arxiv 2607.26258 v1 pith:5VPXTNME submitted 2026-07-28 astro-ph.SR

Asteroseismic study of KUV03442+0719 with parallax constraints

Agn\`{e}s Bischoff-Kim This is my paper
classification astro-ph.SR
keywords asteroseismologywhite dwarf pulsationsZZ Ceti starshelium-core white dwarfslow-mass white dwarfsmass-radius relationparallax constraintsmode identification
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

This paper attempts to determine the interior of the pulsating white dwarf KUV03442+0719, whose parallax suggests a larger, lower-mass star than spectroscopy alone indicates. The author models it in two competing ways: a normal-mass carbon/oxygen-core white dwarf with an unresolved companion adding light, and a low-mass helium-core white dwarf where the measured brightness comes entirely from the star itself. After fitting the same six observed pulsation periods, both models match nearly equally well, so the present data cannot tell the two scenarios apart. The paper also derives a temperature-dependent mass-radius relation for helium-core white dwarfs that can be used with parallax data in future studies. The stakes are how low-mass white dwarfs form: in binary systems or as single stars that lost mass.

Core claim

Grid models refined by simplex minimization fit the observed periods under two interior hypotheses. The carbon/oxygen-core fit (mass ~0.465 solar masses, effective temperature ~10900 K) reproduces the six periods with a weighted RMS residual of 0.43 s; the helium-core fit (~0.27 solar masses, ~10440 K) achieves 1.31 s. The helium-core model requires the parallax-derived magnitude to come entirely from the white dwarf; the carbon/oxygen model requires an unseen companion adding light. Statistical penalties for extra parameters bring the fits close, and the paper concludes that more pulsation data are needed to distinguish the scenarios.

What carries the argument

The central tool is a grid of white-dwarf models with parameterized chemical composition profiles, computed with a stellar evolution and pulsation code, which allows the interior profiles themselves to be varied rather than evolved. The fits are scored by a weighted RMS period residual and by two forms of the Bayes Information Criterion. A temperature-dependent mass-radius relation derived from the helium-core models converts parallax and magnitude into a mass–temperature constraint band used to anchor the helium-core fit. The asymptotic period-spacing relation for l=1 and l=2 g-modes guides the assignment of spherical-degree labels to the six periods.

Load-bearing premise

The six periods used in the fit (plus one from the discovery paper) are the star's true pulsation spectrum: the paper discards most of the 31 periods reported earlier on signal-to-noise grounds and drops mode 116 as a possible duplicate of 117, so if the real spectrum contains additional independent modes, the fits and the comparability conclusion could change.

What would settle it

Take a longer, higher-cadence light curve of KUV03442+0719 and test whether any new independent period fits both models; alternatively, deep high-resolution imaging or radial-velocity monitoring that detects or rules out a companion would settle which interior scenario is correct.

Watch this falsifier — get emailed when new claim-graph text bears on it.

If this is right

  • KUV03442+0719 cannot currently be assigned to either the single helium-core white dwarf class or the carbon/oxygen-core-with-companion class on pulsation grounds alone.
  • A longer or higher signal-to-noise pulsation campaign that yields additional independent periods is the direct path to distinguishing the two scenarios.
  • The supplied mass-radius relation for helium-core white dwarfs (valid 9000–14000 K, 0.25–0.45 solar masses) lets future parallax-based studies estimate masses without re-deriving models.
  • If the helium-core interpretation is right, the star is an example of a low-mass white dwarf outside a binary system, carrying implications for how such stars form.
  • The best carbon/oxygen fits require central oxygen abundances below 50%, difficult to reconcile with stellar evolution; a fit constrained to higher oxygen is acceptable but fits slightly worse.

Where Pith is reading between the lines

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

  • A rotationally split triplet or quintuplet in future data would fix the l identification of one mode, and the two models predict different period spacings, so even one securely identified mode could break the degeneracy.
  • The same ambiguity may afflict other warm ZZ Ceti stars whose parallax photometry implies low mass: asteroseismic fitting alone can leave single low-mass and unresolved-binary carbon/oxygen interpretations equally viable.
  • The mass-radius relation's sensitivity to envelope mass means parallax masses for helium-core white dwarfs carry a structural-model dependence; independent radius measurements, e.g., from eclipsing binaries, would test it.
  • If the unresolved-companion scenario is correct, high-resolution imaging or radial-velocity monitoring should eventually reveal the companion; its absence after deep searches would tilt the balance toward the helium-core model.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 5 minor

Summary. The paper presents an asteroseismic analysis of the pulsating hydrogen-atmosphere white dwarf KUV03442+0719. Because Gaia parallax/photometry suggest a radius larger than expected for a normal-mass white dwarf, the authors consider two scenarios: (i) a carbon/oxygen-core white dwarf of otherwise normal mass with an unresolved line-of-sight companion that contaminates the Gaia photometry, and (ii) a single low-mass helium-core white dwarf. They fit the observed periods with a grid of WDEC models refined by simplex minimization, using spectroscopic effective-temperature constraints for the C/O case and a WDEC-derived mass–radius relation plus Gaia data for the He-core case. The paper concludes that both scenarios produce best-fit models of comparable quality and that more pulsation data are needed to distinguish them. It also provides analytic mass–radius relations for helium-core white dwarfs.

Significance. If its central claim were fully supported, the paper would document a valuable ambiguous case in white-dwarf asteroseismology, where two physically distinct interior structures (C/O core with companion vs. single He core) cannot be separated by current data. The study also makes a useful contribution by providing analytic, temperature-dependent mass–radius coefficients for helium-core white dwarfs, and the WDEC code used is open source. The period-list reduction and the explicit use of two information criteria are methodologically transparent. However, as detailed below, the paper's own reported statistics contradict the 'comparable fit quality' claim, so the main conclusion as stated is not justified by the presented numbers.

major comments (3)
  1. [Abstract; §5; Table 1] The central claim that the two fits are 'comparable in terms of quality of fit' is contradicted by the paper's own Table 1. For the C/O global best fit, σ_RMS = 0.43 s and BIC_Liddle = -1.07; for the He-core fit, σ_RMS = 1.31 s and BIC_Liddle = 12.2. The Liddle BIC difference is ΔBIC ≈ 13.3, which by the standard Kass & Raftery (1995) scale is very strong evidence against the worse (He-core) model. The extra parameter in the He fit contributes only ln(6) ≈ 1.8 to the penalty, far too little to offset the 13-point gap. Thus §5's statement that the C/O model fits better 'only marginally so' is unsupported by the reported Liddle BIC. The authors should either revise the abstract/conclusion or re-evaluate the fitting statistic. Note that the Koen & Laney BIC difference is much smaller (≈0.96), so the paper needs to state which criterion it regards as primary and why.
  2. [§2.1, §2.3] The period list is reduced from the 31 periods of Su et al. (2014) to six (plus one from the discovery paper) based on visual inspection of S/N and spectral windows, and mode 116 is excluded as a possible duplicate of 117. This is a defensible judgment call, but it is a strong filtering step: the entire subsequent comparison rests on these seven periods. Moreover, the mode identifications are chosen by trying all possible ℓ=1/ℓ=2 combinations and selecting those that land in the spectroscopic box. This search over identifications is not accounted for in the reported BIC values, which treat the chosen identifications as fixed. If the real spectrum contains additional independent modes, the fits and the relative quality-of-fit could change. The paper should at least discuss this model-selection uncertainty explicitly, and ideally test robustness by, e.g., fitting with the full Su et al. li
  3. [§2.2, Eq. (5), §3.3] The He-core fit uses a mass–radius relation derived from the same WDEC model family used for the asteroseismic fits. The Gaia parallax constraint is therefore filtered through the same theoretical framework, making the He-core fit partially self-referential. While the paper states this is intentional for self-consistency, the independence of the Gaia constraint is weakened. A systematic error in the WDEC mass–radius relation (e.g., due to envelope structure assumptions) could artificially make the He-core scenario appear more compatible than it is. The authors should quantify the sensitivity of the He-core fit to the choice of mass–radius relation, e.g., by comparing with an independent relation from full evolutionary models.
minor comments (5)
  1. [Throughout] Numerous typos: 'perfom', 'constrast', 'T able', 'V¨ais¨ail¨a', 'Bayes Information Criterion' should be 'Bayesian Information Criterion'. Please proofread.
  2. [Eqs. (9)–(10)] The notation n_obs and n_par is used in the BIC definitions but should be explicitly defined where the equations are introduced (they are defined only later in Table 1).
  3. [Table 1] The column headers distinguish 'Global best fit' and 'Constrained XO' for the C/O model, but the table caption does not explain that the constrained fit requires central oxygen abundance > 0.50. Please clarify.
  4. [Figure 6] The caption states 'other parameters have a negligible effect on the mass-radius relation,' but a quantitative comparison of curve deviations would help support this claim.
  5. [§2.1] The statement 'We also check for beat frequencies and find none' is not accompanied by any details of the check. A short description of the procedure would improve reproducibility.

Circularity Check

1 steps flagged

Mild self-consistency loop in the He-core parallax constraint; no hard circularity in the period fits

specific steps
  1. other [Section 2.2, Eq. (5); Section 3.3; Figure 2]
    "This requires the use of a mass-radius relationship. We derive one from our own grid of helium core models (see section 3), allowing us to obtain constraints that are self-consistent."

    The He-core fit is anchored by a Gaia-based mass-Teff band that is not an independent external check: Eq. (5) is a polynomial fit to WDEC helium-core models, the same code/model family used for the asteroseismic fits. The parallax+magnitude data are thus converted into a mass constraint using the same theoretical structure parameterization (M_env2) that the period fit later adjusts, and this band is used to select the preferred mode identification and unique best fit. This is a self-consistency loop rather than a definitional reduction: the observed periods are still matched independently by WDEC models and no fitted parameter is relabeled as a prediction. It is therefore only a mild self-reference, not full circularity.

full rationale

I find no circular step that makes the central result equivalent to its inputs by construction. The period list (Table 1) is an external input (Su et al. 2014; Gianninas et al. 2006), and the C/O-core fit minimizes sigma_RMS against those periods with WDEC models in a standard grid+simplex search; the prediction (model periods) is compared with observed periods, not derived from a fitted constant. The one self-referential element is the He-core parallax constraint: Eq. (5) is a mass-radius relation fitted to the authors' own WDEC helium-core grid, and the resulting mass-Teff band (Fig. 2) is used to disambiguate mode identifications and select the best fit. This makes the He-core scenario's Gaia consistency depend on the model class under test, but it does not make the fit a tautology. I also flag, as a non-circularity correctness issue, that the paper's own Table 1 statistics contradict the abstract's 'comparable quality of fit' wording: BIC_Liddle is -1.07 for the C/O model versus 12.2 for the He model, Delta-BIC about 13.3, which is usually considered very strong evidence; Section 5's 'only marginally so' is therefore internally unsupported. The manuscript's explicit limitations (reduced period selection in Section 2.1, the assumption that observed hydrogen lines belong to the white dwarf in Section 2.2, and the need for more pulsation data in Section 5) are acknowledged assumptions, not hidden circularities. Under the hard rules, this is a 2, not a 6+: the central derivation is self-contained with respect to external constraints apart from the mild WDEC-based M-R self-reference.

Axiom & Free-Parameter Ledger

13 free parameters · 7 axioms · 1 invented entities

The analysis rests on WDEC models with parameterized chemical profiles, standard asymptotic pulsation theory, and several stated assumptions about the target's multiplicity and photometric interpretation. The helium-core fit additionally uses a mass-radius relation derived from the same modeling code, creating a mild self-referential loop. No new physical entity beyond the hypothesized companion is introduced.

free parameters (13)
  • C/O fit: h1 (oxygen profile position) = 0.43 (global best fit)
    Varied in grid; sets the location of the inner oxygen profile transition.
  • C/O fit: h2 (oxygen profile width) = 0.92
    Varied in grid; sets the width of the oxygen profile.
  • C/O fit: xhe_bar (helium abundance) = 0.14
    Helium abundance in the mixed He/C-O region.
  • C/O fit: alpha1 (profile sharpness) = 20
    Sharpness of chemical composition transitions in the envelope.
  • C/O fit: Teff = 10905 K
    Effective temperature; grid ranged 10100–11500 K.
  • He fit: Menv2 (envelope mass) = 10^-4.84
    Mass at the base of the He/H envelope; strongly constrained by the Gaia-based lines in Fig. 2.
  • He fit: MH (hydrogen layer mass) = 10^-6.51
    Thickness of the pure hydrogen layer; fixed in the refined grid but varied in the master grid.
  • He fit: XH (hydrogen abundance) = 0.65
    Hydrogen abundance in the mixed He/H region.
  • He fit: alpha1 = 9.1
    Sharpness of the He/H transition.
  • He fit: alpha2 = 18.7
    Sharpness of the He/H transition.
  • He fit: Teff = 10438 K
    Effective temperature.
  • He fit: M = 0.270 M_sun
    Stellar mass; constrained by the Gaia parallax via the derived M-R relation.
  • M-R polynomial coefficients a(T), b(T), c(T), d(T) = Table 5 coefficients
    Fitted to the WDEC He-core model grid; used to convert Gaia parallax and G magnitude into mass constraints.
axioms (7)
  • domain assumption WDEC model frequencies accurately represent g-mode pulsations of white dwarfs with parameterized chemical profiles
    The entire fitting uses WDEC (Bischoff-Kim & Montgomery 2018) as ground truth; no independent code cross-check is provided.
  • standard math Asymptotic period spacing formula (Eq. 6) is valid for the observed long-period modes
    Used to assign l=1 vs l=2 mode identifications in §2.3.
  • domain assumption All observed modes are m=0, i.e., no rotational splitting
    Stated at the start of §2.3; no triplets or quintuplets are observed to justify m assignment.
  • ad hoc to paper In the C/O scenario, an unresolved companion contributes to the Gaia G magnitude but not to the hydrogen-line spectrum
    Necessary to reconcile the Gaia-based radius with a normal-mass C/O white dwarf; no companion is detected.
  • domain assumption In the He scenario, the Gaia G magnitude is entirely from the white dwarf
    Required for the parallax-based mass constraint; contradicts the companion hypothesis.
  • domain assumption The hydrogen lines used for spectroscopic Teff/logg belong to the pulsating white dwarf
    Acknowledged by the author in §2.2 as an assumption.
  • domain assumption The WDEC-derived He-core mass-radius relation is accurate enough for the parallax mass constraint
    The relation is self-derived from the same model family used in the fits, with no external validation against measured He-core WD masses.
invented entities (1)
  • Unresolved companion / line-of-sight object no independent evidence
    purpose: Explains the Gaia photometric excess in the C/O-core scenario without contaminating the spectrum
    Postulated to reconcile the Gaia-based radius with a normal-mass C/O white dwarf; no direct detection, radial velocity, or imaging evidence is presented.

pith-pipeline@v1.3.0-alltime-deepseek · 11907 in / 15389 out tokens · 135531 ms · 2026-08-01T00:19:46.920638+00:00 · methodology

0 comments
read the original abstract

Hydrogen atmosphere white dwarf KUV03442+0719 was first reported as a pulsator by Gianninas et al. in 2006. Follow up campaigns by Su et al. (2014) revealed more periods. Some spectroscopic results suggest that KUV03442+0719 has a slightly below average mass and an effective temperature of 11000 K. But Gaia data (parallax and magnitude) suggest that it may be a low mass white dwarf. Such an object would have a helium core. We perform the asteroseismic fitting of KUV03442+0719, modeling it both as a carbon/oxygen normal mass white dwarf, and a helium core, low mass white dwarf. To perform the study, we perfom a grid search with WDEC models, refined by simplex minimization of the best fits. Both analyses result in best fit models that are comparable in terms of quality of fit. More pulsation data would be required to allow us to distinguish between the two scenarios. We present and constrast our results with expectations from stellar evolution. We also provide analytic formulae for a temperature dependent mass-radius relationship for helium core white dwarfs.

Figures

Figures reproduced from arXiv: 2607.26258 by Agn\`{e}s Bischoff-Kim.

Figure 1
Figure 1. Figure 1: Core profiles for the fiducial model that serves as a basis for the mass-radius relationship (dashed lines, section 2), best fit model (solid lines), and interior profile based on the 0.2724 M⊙, 16481 K model of (Calcaferro et al. 2017) (dash-dotted line). The center is on the left. The core is composed of helium, while the envelope of hydrogen. The fiducial model, listed in table 4, was chosen to have thi… view at source ↗
Figure 2
Figure 2. Figure 2: Constraints for the asteroseismic fitting, along with a contour plot of the quality of fit of models comprising the master grid for helium core white dwarfs (see table 4). The color scale is in tenths of seconds. The red box indicates the boundaries in effective temperature and mass based on the spectroscopy of Gentile Fusillo et al. (2021). The diagonal lines with positive slope are constructed by combini… view at source ↗
Figure 3
Figure 3. Figure 3: Parameter sensitivity for KUV03442+0719 ’s pulsation spectrum. For a description of the parameters, see text and Bischoff-Kim (2018a). The lightly colored boxes highlight parameters that we varied in the grid search. For that fiducial model, we varied one parameter at a time and observed the effect of varying that parameter on the quality of the fit. We tried his exercise for every possible ℓ identificatio… view at source ↗
Figure 4
Figure 4. Figure 4: Location of the best fits in three cuts in parameter space for C/O model 1. All five parameters varied in the C/O core fitting are featured. C/O model 2 present very similar contour plots. The vertical lines indicate the range of effective temperatures that correspond to the spectroscopy (2). The third graph was produced using only the models that had effective temperatures in the spectroscopic range [PIT… view at source ↗
Figure 5
Figure 5. Figure 5: Chemical composition profiles for the global best fit model of table 3 (solid lines, top panel) and for the best fit model constrained to have a central oxygen abundance greater than 0.50 (solid lines, bottom panel). The center of the model is on the left. For each, we also graph chemical profiles from Althaus et al. (2010). The models compare very closely in effective temperature, not in mass. The best fi… view at source ↗
Figure 6
Figure 6. Figure 6: Mass-radius relationships for different effective temperatures or structure parameters. The base model is the fiducial model listed in table 4. The other parameters have a negligible effect on the mass-radius relation. Bischoff-Kim, A., & Montgomery, M. H. 2018, AJ, 155, 187, doi: 10.3847/1538-3881/aab70e Bischoff-Kim, A. & Montgomery, M. H. 2018b, White Dwarf Evolution Code, 1.0, Zenodo, doi: 10.5281/zeno… view at source ↗

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

190 extracted references · 23 linked inside Pith

  1. [1]

    New evolutionary models for massive ZZ Ceti stars. I. First results for their pulsational properties. , eprint =. doi:10.1051/0004-6361:20030472 , adsurl =

    doi:10.1051/0004-6361:20030472

  2. [2]

    A&A , eprint =

    The formation and evolution of hydrogen-deficient post-AGB white dwarfs: The emerging chemical profile and the expectations for the PG 1159-DB-DQ evolutionary connection. A&A , eprint =. doi:10.1051/0004-6361:20041965 , adsurl =

    doi:10.1051/0004-6361:20041965

  3. [3]

    ApJ , archivePrefix = "arXiv", eprint =

    New Chemical Profiles for the Asteroseismology of ZZ Ceti Stars. ApJ , archivePrefix = "arXiv", eprint =. doi:10.1088/0004-637X/717/2/897 , adsurl =

    doi:10.1088/0004-637x/717/2/897

  4. [4]

    Homogeneous mass and age determinations and asteroseismic prospects

    New evolutionary sequences for extremely low-mass white dwarfs. Homogeneous mass and age determinations and asteroseismic prospects. , keywords =. doi:10.1051/0004-6361/201321868 , archivePrefix =. 1307.1882 , primaryClass =

    Pith/arXiv arXiv

  5. [5]

    , keywords =

    The evolution of white dwarfs resulting from helium-enhanced, low-metallicity progenitor stars. , keywords =. doi:10.1051/0004-6361/201629909 , archivePrefix =. 1611.06191 , primaryClass =

    Pith/arXiv arXiv

  6. [6]

    Nuclear Physics A , year = 1999, month = aug, volume = 656, pages =

    A compilation of charged-particle induced thermonuclear reaction rates. Nuclear Physics A , year = 1999, month = aug, volume = 656, pages =. doi:10.1016/S0375-9474(99)00030-5 , adsurl =

    doi:10.1016/s0375-9474(99)00030-5 1999

  7. [7]

    , keywords =

    Acoustic fluxes in white dwarfs. , keywords =. doi:10.1086/158551 , adsurl =

    doi:10.1086/158551

  8. [8]

    Journal of Cosmology and Astro-Particle Physics , keywords =

    First axion bounds from a pulsating helium-rich white dwarf star. Journal of Cosmology and Astro-Particle Physics , keywords =. doi:10.1088/1475-7516/2016/08/062 , primaryClass =

    doi:10.1088/1475-7516/2016/08/062 2016

  9. [9]

    ApJ , year = 1999, month = may, volume = 516, pages =

    Spectroscopic Studies of DB White Dwarfs: The Instability Strip of the Pulsating DB (V777 Herculis) Stars. ApJ , year = 1999, month = may, volume = 516, pages =. doi:10.1086/307148 , adsurl =

    doi:10.1086/307148 1999

  10. [10]

    , archivePrefix = "arXiv", eprint =

    KIC 4552982: Outbursts and Asteroseismology from the Longest Pseudo-continuous Light Curve of a ZZ Ceti. , archivePrefix = "arXiv", eprint =. doi:10.1088/0004-637X/809/1/14 , adsurl =

    doi:10.1088/0004-637x/809/1/14

  11. [11]

    , eprint =

    On the Purity of the ZZ Ceti Instability Strip: Discovery of More Pulsating DA White Dwarfs on the Basis of Optical Spectroscopy. , eprint =. doi:10.1086/379808 , adsurl =

    doi:10.1086/379808

  12. [12]

    , archivePrefix = "arXiv", eprint =

    A Comprehensive Spectroscopic Analysis of DB White Dwarfs. , archivePrefix = "arXiv", eprint =. doi:10.1088/0004-637X/737/1/28 , adsurl =

    doi:10.1088/0004-637x/737/1/28

  13. [13]

    A&A , eprint =

    New evolutionary calculations for the born again scenario. A&A , eprint =. doi:10.1051/0004-6361:20053804 , adsurl =

    doi:10.1051/0004-6361:20053804

  14. [14]

    Probing exotic physics with pulsating white dwarfs

  15. [15]

    ApJ , eprint =

    Fine Grid Asteroseismology of G117-B15A and R548. ApJ , eprint =. doi:10.1086/527287 , adsurl =

    doi:10.1086/527287

  16. [16]

    ApJ , eprint =

    Strong Limits on the DFSZ Axion Mass with G117-B15A. ApJ , eprint =. doi:10.1086/526398 , adsurl =

    doi:10.1086/526398

  17. [17]

    Communications in Asteroseismology , year = 2008, month = jun, volume = 154, pages =

    Preliminary Asteroseismology of EC20058-5234 and Limits on Plasmon Neutrinos. Communications in Asteroseismology , year = 2008, month = jun, volume = 154, pages =

    2008

  18. [18]

    American Institute of Physics Conference Series , year = 2009, series =

    Asteroseismological Analysis of Rich Pulsating White Dwarfs. American Institute of Physics Conference Series , year = 2009, series =. doi:10.1063/1.3246573 , adsurl =

    doi:10.1063/1.3246573 2009

  19. [20]

    It is a Hot One

    Asteroseismology of the Kepler Field DBV White Dwarf. It is a Hot One. , archivePrefix = "arXiv", eprint =. doi:10.1088/2041-8205/742/1/L16 , adsurl =

    doi:10.1088/2041-8205/742/1/l16 2041

  20. [21]

    Progress in Physics of the Sun and Stars: A New Era in Helio- and Asteroseismology , year = 2013, editor =

    Decoding the Rich Pulsation Spectrum of EC 14012-1446. Progress in Physics of the Sun and Stars: A New Era in Helio- and Asteroseismology , year = 2013, editor =

    2013

  21. [22]

    ApJ , keywords =

    Seven-period Asteroseismic Fit of the Kepler DBV. ApJ , keywords =. doi:10.1088/0004-637X/794/1/39 , adsurl =

    doi:10.1088/0004-637x/794/1/39

  22. [23]

    19th European Workshop on White Dwarfs , year = 2015, series =

    Patterns Emerging from the Asteroseismic Studies of DBVs. 19th European Workshop on White Dwarfs , year = 2015, series =

    2015

  23. [24]

    , author=

    Bischoff-Kim, Agnès and Provencal, Judith L. , author=. Asteroseismology of GD358 with complex core carbon and oxygen profiles , journal=. 2015 , month=. doi:10.1017/S1743921316005950 , url=

    doi:10.1017/s1743921316005950 2015

  24. [25]

    20th European Workshop on White Dwarfs , year = 2017, series =

    Semi-chaotic behaviors observed in the asteroseismic fitting of GD358. 20th European Workshop on White Dwarfs , year = 2017, series =

    2017

  25. [27]

    , keywords =

    WDEC: A Code for Modeling White Dwarf Structure and Pulsations. , keywords =. doi:10.3847/1538-3881/aab70e , primaryClass =

    doi:10.3847/1538-3881/aab70e

  26. [28]

    doi:10.5281/zenodo.1188445 , version =

    doi:10.5281/zenodo.1188445

  27. [29]

    doi:10.5281/zenodo.1715917 , url =

    doi:10.5281/zenodo.1715917

  28. [30]

    U ber die Wasserstoffkonvektionszone in Sternen verschiedener Effektivtemperaturen und Leuchtkr \

    \" U ber die Wasserstoffkonvektionszone in Sternen verschiedener Effektivtemperaturen und Leuchtkr \" a fte. Zeitschrift f\"ur Astrophysik , year = 1958, volume = 46, pages =

    1958

  29. [31]

    , year = 1971, month = apr, volume = 12, pages =

    Convective Envelopes and Acoustic Noise Generation in White Dwarfs. , year = 1971, month = apr, volume = 12, pages =

    1971

  30. [32]

    I - Adiabatic results

    Asteroseismology of white dwarf stars. I - Adiabatic results. , keywords =. doi:10.1086/191539 , adsurl =

    doi:10.1086/191539

  31. [33]

    , keywords =

    The potential for asteroseismology of DB white dwarf stars. , keywords =. doi:10.1086/172477 , adsurl =

    doi:10.1086/172477

  32. [34]

    , keywords =

    Theoretical Models for Asteroseismology of DA White Dwarf Stars. , keywords =. doi:10.1086/177696 , adsurl =

    doi:10.1086/177696

  33. [35]

    ApJ , keywords =

    An asteroseismological determination of the structure of the DBV white dwarf GD 358. ApJ , keywords =. doi:10.1086/174456 , adsurl =

    doi:10.1086/174456

  34. [36]

    IAU Colloq

    Analysis of Long-Term Single-Site Observations of the Pulsating DB White Dwarf GD 358. IAU Colloq. 193: Variable Stars in the Local Group , year = 2004, series =

    2004

  35. [37]

    1: Basic theory and semianalytic expressions for the emergent flux , journal =

    The modeling of energy distributions and light curves of ZZ Ceti stars. 1: Basic theory and semianalytic expressions for the emergent flux , journal =

  36. [38]

    Brickhill , A. J. The Pulsations of Zz-Ceti Stars - Part Six - the Amplitude Spectra

  37. [39]

    The ELM Survey. IX. A Complete Sample of Low-mass White Dwarf Binaries in the SDSS Footprint. , keywords =. doi:10.3847/1538-4357/ac72ac , archivePrefix =. 2207.02998 , primaryClass =

    Pith/arXiv arXiv

  38. [40]

    Pulsating low-mass white dwarfs in the frame of new evolutionary sequences. IV. The secular rate of period change. , keywords =. doi:10.1051/0004-6361/201630376 , archivePrefix =. 1701.08880 , primaryClass =

    Pith/arXiv arXiv

  39. [41]

    , keywords =

    On the use of Gaia magnitudes and new tables of bolometric corrections. , keywords =. doi:10.1093/mnrasl/sly104 , archivePrefix =. 1806.01953 , primaryClass =

    Pith/arXiv arXiv

  40. [42]

    14th European Workshop on White Dwarfs , year = 2005, series =

    Revisiting the DBs Instability Strip Using UV Spectra. 14th European Workshop on White Dwarfs , year = 2005, series =

    2005

  41. [43]

    , keywords =

    HST observations of the pulsating white dwarf GD 358. , keywords =. doi:10.1051/0004-6361:20041573 , adsurl =

    doi:10.1051/0004-6361:20041573

  42. [45]

    , archivePrefix = "arXiv", eprint =

    New developments of the ZZ Ceti instability strip: the discovery of 11 new variables. , archivePrefix = "arXiv", eprint =. doi:10.1111/j.1365-2966.2010.16633.x , adsurl =

    arXiv 2010

  43. [46]

    Testing the forward modeling approach in asteroseismology. II. Structure and internal dynamics of the hot B subdwarf component in the close eclipsing binary system PG 1336-018. , keywords =. doi:10.1051/0004-6361:200809907 , adsurl =

    doi:10.1051/0004-6361:200809907

  44. [47]

    European Physical Journal Web of Conferences , year = 2017, series =

    Determining the core stratification in white dwarfs with asteroseismology. European Physical Journal Web of Conferences , year = 2017, series =. doi:10.1051/epjconf/201715205005 , adsurl =

    arXiv 2017

  45. [48]

    , year = 1964, month = Jul, volume =

    Evidence for the 2 Decay of the K20 Meson. , year = 1964, month = Jul, volume =. doi:10.1103/PhysRevLett.13.138 , adsurl =

    doi:10.1103/physrevlett.13.138 1964

  46. [49]

    , keywords =

    The potential of the variable DA white dwarf G117-B15A as a tool for fundamental physics. , keywords =. doi:10.1016/S1384-1076(01)00055-0 , archivePrefix =. astro-ph/0104103 , primaryClass =

    Pith/arXiv arXiv

  47. [50]

    , eprint =

    The rate of period change in pulsating DB white dwarf stars. , eprint =. doi:10.1051/0004-6361:20041372 , adsurl =

    doi:10.1051/0004-6361:20041372

  48. [51]

    A& A , eprint =

    Asteroseismic inferences on GW Virginis variable stars in the frame of new PG 1159 evolutionary models. A& A , eprint =. doi:10.1051/0004-6361:20054199 , adsurl =

    doi:10.1051/0004-6361:20054199

  49. [52]

    Hydrogen-Deficient Stars , year = 2008, series =

    Asteroseismological Modeling of PG 1159-035, the Prototype of the GW Vir Variable Stars. Hydrogen-Deficient Stars , year = 2008, series =

    2008

  50. [53]

    JCAP , archivePrefix = "arXiv", eprint =

    An independent limit on the axion mass from the variable white dwarf star R548. JCAP , archivePrefix = "arXiv", eprint =. doi:10.1088/1475-7516/2012/12/010 , adsurl =

    doi:10.1088/1475-7516/2012/12/010 2012

  51. [54]

    , archivePrefix = "arXiv", eprint =

    Asteroseismology of the Kepler V777 Herculis variable white dwarf with fully evolutionary models. , archivePrefix = "arXiv", eprint =. doi:10.1051/0004-6361/201118736 , adsurl =

    doi:10.1051/0004-6361/201118736

  52. [55]

    , keywords =

    The rate of cooling of the pulsating white dwarf star G117-B15A: a new asteroseismological inference of the axion mass. , keywords =. doi:10.1111/j.1365-2966.2012.21401.x , archivePrefix =. 1205.6180 , primaryClass =

    arXiv 2012

  53. [56]

    Journal of Cosmology and Astroparticle Physics , archivePrefix = "arXiv", eprint =

    An independent constraint on the secular rate of variation of the gravitational constant from pulsating white dwarfs. Journal of Cosmology and Astroparticle Physics , archivePrefix = "arXiv", eprint =. doi:10.1088/1475-7516/2013/06/032 , adsurl =

    doi:10.1088/1475-7516/2013/06/032 2013

  54. [57]

    , archivePrefix = "arXiv", eprint =

    An asteroseismic constraint on the mass of the axion from the period drift of the pulsating DA white dwarf star L19-2. , archivePrefix = "arXiv", eprint =. doi:10.1088/1475-7516/2016/07/036 , adsurl =

    doi:10.1088/1475-7516/2016/07/036 2016

  55. [58]

    , keywords =

    Pulsating white dwarfs: new insights. , keywords =. doi:10.1007/s00159-019-0118-4 , archivePrefix =. 1907.00115 , primaryClass =

    Pith/arXiv arXiv 1907

  56. [59]

    , archivePrefix = "arXiv", eprint =

    The pulsation modes of the pre-white dwarf PG 1159-035. , archivePrefix = "arXiv", eprint =. doi:10.1051/0004-6361:20053470 , adsurl =

    doi:10.1051/0004-6361:20053470

  57. [60]

    American Institute of Physics Conference Series , year = 2010, series =

    The O-C Diagram of EC20058-5234: Detection of Neutrino Emission?. American Institute of Physics Conference Series , year = 2010, series =. doi:10.1063/1.3527883 , adsurl =

    doi:10.1063/1.3527883 2010

  58. [61]

    , keywords =

    Periodic Variations in the O - C Diagrams of Five Pulsation Frequencies of the DB White Dwarf EC 20058-5234. , keywords =. doi:10.1088/0004-637X/765/1/5 , archivePrefix =. 1302.2693 , primaryClass =

    Pith/arXiv arXiv

  59. [62]

    19th European Workshop on White Dwarfs , year = 2015, editor =

    Quasi-Periodic Variations of the Pulsation Frequencies of Three White Dwarfs. 19th European Workshop on White Dwarfs , year = 2015, editor =

    2015

  60. [63]

    ApJl , eprint =

    Thick to thin: The evolutionary connection between PG 1159 stars and the thin helium-enveloped pulsating white dwarf GD 358. ApJl , eprint =. doi:10.1086/187909 , adsurl =

    doi:10.1086/187909

  61. [64]

    Physics Letters B , year = 1981, month = Aug, volume =

    A simple solution to the strong CP problem with a harmless axion. Physics Letters B , year = 1981, month = Aug, volume =. doi:10.1016/0370-2693(81)90590-6 , adsurl =

    doi:10.1016/0370-2693(81)90590-6 1981

  62. [65]

    A&A , keywords =

    Spectral analyses of PG 1159 star: constraints on the GW Virginis pulsations from HST observations. A&A , keywords =

  63. [66]

    , keywords =

    Light and radial velocity variations in a nonradially oscillating star. , keywords =

  64. [67]

    Outer layers of white dwarf stars

  65. [68]

    , keywords =

    Convective white-dwarf envelope model grids for H-, He-, and C-rich compositions. , keywords =. doi:10.1086/190388 , adsurl =

    doi:10.1086/190388

  66. [69]

    ApJs , year = 1977, volume = 35, pages =

    Equations of State for Stellar Partial Ionization Zones. ApJs , year = 1977, volume = 35, pages =. doi:10.1086/190482 , adsurl =

    doi:10.1086/190482 1977

  67. [70]

    Apj Letters , keywords =

    Can White Dwarf Asteroseismology Really Constrain the ^ 12 C( , )^ 16 O Reaction Rate?. Apj Letters , keywords =. doi:10.1086/345787 , adsurl =

    doi:10.1086/345787

  68. [71]

    Summary of the astrometric, photometric, and survey properties

    Gaia Data Release 1. Summary of the astrometric, photometric, and survey properties. , keywords =. doi:10.1051/0004-6361/201629512 , archivePrefix =. 1609.04172 , primaryClass =

    Pith/arXiv arXiv

  69. [72]

    Summary of the contents and survey properties

    Gaia Early Data Release 3. Summary of the contents and survey properties. , keywords =. doi:10.1051/0004-6361/202039657 , archivePrefix =. 2012.01533 , primaryClass =

    Pith/arXiv arXiv 2012

  70. [73]

    , keywords =

    A catalogue of white dwarfs in Gaia EDR3. , keywords =. doi:10.1093/mnras/stab2672 , archivePrefix =. 2106.07669 , primaryClass =

    Pith/arXiv arXiv

  71. [74]

    A New Analysis of the Two Classical ZZ Ceti White Dwarfs GD 165 and Ross 548. II. Seismic Modeling. ApJS , keywords =. doi:10.3847/0067-0049/223/1/10 , adsurl =

    doi:10.3847/0067-0049/223/1/10

  72. [75]

    20th European Workshop on White Dwarfs , year = 2017, series =

    The core stratification of Kepler white dwarf pulsators: towards constraints on nuclear burning and chemical mixing of He-Core-Burning phases. 20th European Workshop on White Dwarfs , year = 2017, series =

    2017

  73. [76]

    Apj , archivePrefix = "arXiv", eprint =

    Toward High-precision Seismic Studies of White Dwarf Stars: Parametrization of the Core and Tests of Accuracy. Apj , archivePrefix = "arXiv", eprint =. doi:10.3847/1538-4357/834/2/136 , adsurl =

    doi:10.3847/1538-4357/834/2/136

  74. [77]

    , keywords =

    Mapping the ZZ Ceti Instability Strip: Discovery of Six New Pulsators. , keywords =. doi:10.1086/506516 , archivePrefix =. astro-ph/0606135 , primaryClass =

    Pith/arXiv arXiv

  75. [78]

    , keywords =

    A Spectroscopic Survey and Analysis of Bright, Hydrogen-rich White Dwarfs. , keywords =. doi:10.1088/0004-637X/743/2/138 , archivePrefix =. 1109.3171 , primaryClass =

    Pith/arXiv arXiv

  76. [80]

    , eprint =

    The White Dwarf Luminosity Function from Sloan Digital Sky Survey Imaging Data. , eprint =. doi:10.1086/497966 , adsurl =

    doi:10.1086/497966

  77. [81]

    New Astronomy Review , eprint =

    Massive star evolution: nucleosynthesis and nuclear reaction rate uncertainties. New Astronomy Review , eprint =

  78. [82]

    A&A , eprint =

    On the formation of hydrogen-deficient post-AGB stars. A&A , eprint =

  79. [83]

    ApJ , keywords =

    On the evolution of those nuclei of planetary nebulae that experience a final helium shell flash. ApJ , keywords =. doi:10.1086/160631 , adsurl =

    doi:10.1086/160631

  80. [84]

    ApJ , year = 1996, month = jun, volume = 464, pages =

    Updated Opal Opacities. ApJ , year = 1996, month = jun, volume = 464, pages =. doi:10.1086/177381 , adsurl =

    doi:10.1086/177381 1996

Showing first 80 references.