Pith. sign in

REVIEW 6 minor 45 references

Blackbody atmospheres for hot compact stars understate optical light by about 25 percent and force unphysical binary parameters; TMAP and Tremblay tables plus blending remove the bias.

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 · grok-4.5

2026-07-10 15:36 UTC pith:2VUEJN6K

load-bearing objection Solid engineering paper that removes a known ~25% optical-intensity bias for hot compact stars in PHOEBE; the blackbody demonstration is quantitative and the new tables are immediately usable.

arxiv 2607.07909 v1 pith:2VUEJN6K submitted 2026-07-08 astro-ph.SR astro-ph.IM

Physics of Eclipsing Binaries. VI. Hot, compact stars

David Jones , Nicole Reindl , Kyle Conroy , James Munday , Pier-Emmanuel Tremblay , Michael Abdul-Masih , Matthias Fabry , Joseph Giammarco
show 4 more authors
Kelly Hambleton Herbert Pablo Marcin Wrona Andrej Prsa
This is my paper
classification astro-ph.SR astro-ph.IM
keywords eclipsing binariesmodel atmosphereswhite dwarfslimb darkeningirradiationTMAPPHOEBElight curves
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.

Eclipsing-binary light-curve codes assign an emergent intensity to every surface element of each star. For hot, compact objects those intensities have long been taken from blackbodies or from atmosphere grids that do not cover the relevant temperatures and gravities. The paper shows that a blackbody is systematically too bright in the optical by roughly 25 percent (sometimes 40 percent). When such a blackbody is used for a hot primary, the fitted temperature is forced too low and the companion's albedo is forced above unity simply to recover the observed irradiation amplitude. Version 2.5 of the modelling code therefore adds non-LTE TMAP grids (sdO, DA, DAO, DO) and LTE Tremblay DA grids, together with a blending/extrapolation scheme that lets a few surface elements slide smoothly off-grid rather than aborting the calculation. The same tables also supply ready-to-use limb-darkening coefficients for other codes. A concrete synthetic binary (127 kK pre-white-dwarf plus K5V) demonstrates that the new atmospheres recover physical parameters while the blackbody solution does not.

Core claim

Approximating hot compact stars as blackbodies underestimates optical passband intensities by about 25 percent (up to 40 percent). That single systematic forces the fitted effective temperature of the hot star too low by roughly one-quarter and drives the irradiated companion's bolometric albedo to unphysical values greater than one. Incorporating TMAP and Tremblay model atmospheres, together with linear blending/extrapolation when a few mesh points leave the grid, removes the bias and restores physical parameters.

What carries the argument

Sparse-grid ndpolation (nearest fully-defined hypercube, unit-hypercube transformation, sequential dimensionality reduction) followed by distance-weighted blending into a blackbody; the mechanism that lets model atmospheres be used even when a minority of surface elements fall outside the tabulated Teff–log g–abundance range.

Load-bearing premise

That linear extrapolation or nearest-node lookup from the nearest complete hypercube of a sparse atmosphere table, then a gradual blend into a blackbody, remains a good enough approximation for the handful of surface elements that leave the grid.

What would settle it

Re-model an observed hot-compact binary both with pure blackbody atmospheres and with the new TMAP/Tremblay tables plus blending; if the blackbody solution still yields albedos above unity while the new solution yields albedos near the expected value and temperatures consistent with independent spectroscopy, the central claim holds.

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

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

0 major / 6 minor

Summary. The manuscript describes the PHOEBE 2.5 release, which incorporates TMAP (sdO, DA, DAO, DO) and Montréal/Tremblay model atmospheres for hot, compact stars, complements existing PHOENIX and Castelli & Kurucz grids, and adds blending/extrapolation so that a minority of surface elements outside the tabulated Teff–log g–abundance range need not force a full blackbody fallback. It also re-enables user-supplied Doppler boosting factors and introduces portable user-defined features. Consistency among the four TMAP grids, agreement of normal intensities and linear limb-darkening coefficients with Tremblay and Claret et al. (2020a) at the ~10 % level, and a synthetic 127 kK pre-WD + K5V binary that quantifies the blackbody bias (~25 % optical intensity overestimate, ~26 % Teff underestimate, unphysical albedos) are presented. Tables of limb-darkening coefficients for standard filters are supplied as an added-value product.

Significance. The work removes a well-documented systematic that has affected light-curve modelling of hot white dwarfs, subdwarfs and pre-WDs. The synthetic demonstration (Fig. 7) makes the practical impact concrete, and the public release of both the atmospheres inside PHOEBE and the LD tables for other codes is immediately useful. The ndpolator library and the blending machinery are engineering contributions that broaden the usable domain of atmosphere grids without requiring new atmosphere calculations. The paper is a solid, incremental advance in the PHOEBE series and will improve parameter fidelity for a growing class of compact binaries.

minor comments (6)
  1. Abstract and §2.1: “incorporation model atmospheres” and “Tübingen” / “Montréal” spelling and diacritics should be made consistent throughout the text and keywords.
  2. §2.2 / footnote 1: the correction of the logarithmic LD law (ln rather than log10) is useful; a brief cross-reference to the Klinglesmith & Sobieski (1970) definition would help readers who still use the older notation.
  3. Fig. 1 caption and white spaces: a short note that the gaps are both sampling density and Eddington-limit exclusions (already stated in Table 1) would prevent misreading as missing data.
  4. §2.5: the conversion of Claret et al. (2020a) intensities (mW m−2 Hz−1 plus the ×2 factor) is described; stating the effective-wavelength assumption more explicitly would aid reproducibility.
  5. Appendix A: the description of sequential dimensionality reduction and incomplete hypercubes is clear, but a one-sentence statement that the blend is intended only for a minority of surface elements (and is not claimed to be spectroscopically accurate) would forestall over-interpretation.
  6. Software and data availability: the LD coefficient tables are mentioned as a .tar.gz package; a permanent DOI or repository link would strengthen long-term usability.

Circularity Check

0 steps flagged

No significant circularity: methods paper implements external atmosphere grids and demonstrates their impact via direct comparison and synthetic binaries.

full rationale

The paper's load-bearing claims rest on incorporation of independently computed TMAP (Reindl et al. 2016, 2023) and Montréal/Tremblay (Tremblay & Bergeron 2009) model atmospheres, consistency checks between those grids and published LD coefficients (Figs. 3–5), and a transparent synthetic binary demonstration that blackbody atmospheres produce ~25% higher optical intensities, forcing ~26% lower Teff and unphysical albedos >1 to match irradiation amplitudes (Fig. 7, §3). No quantity is defined in terms of a fitted parameter later presented as a prediction; LD coefficients are ordinary least-squares fits to the external angle-dependent intensities and are supplied only as an added-value product. Self-citations are to prior PHOEBE releases that supply the code framework (mesh, passband integration, etc.) but do not supply or presuppose the new atmosphere tables or the blackbody-bias result. Blending/extrapolation (Appendix A) is an engineering prescription for out-of-grid surface elements and is not required for the on-grid intensity comparisons that underwrite the strongest claim. The derivation chain is therefore self-contained against external benchmarks and exhibits none of the enumerated circularity patterns.

Axiom & Free-Parameter Ledger

0 free parameters · 3 axioms · 0 invented entities

The work is an engineering implementation of existing non-LTE atmosphere codes. Load-bearing premises are the physical validity of the TMAP and Tremblay grids themselves and the adequacy of linear blending outside those grids; no free parameters are fitted to observational data to support the central claim.

axioms (3)
  • domain assumption TMAP and Tremblay model atmospheres correctly predict angle-dependent specific intensities for pure-H and H/He atmospheres in the stated Teff–log g ranges.
    Invoked throughout §2; the paper treats the published grids as ground truth and only checks internal consistency.
  • ad hoc to paper Linear interpolation/extrapolation on the nearest fully-defined hypercube, followed by distance-weighted blending to a blackbody, is an acceptable approximation when a minority of surface elements leave the grid.
    Defined in §4 and Appendix A; no external validation of the blending function is provided.
  • standard math Passband-integrated intensities can be obtained by multiplying the model SED by the filter transmission and integrating.
    Standard photometric practice used for all atmosphere tables in PHOEBE.

pith-pipeline@v1.1.0-grok45 · 19620 in / 2097 out tokens · 23207 ms · 2026-07-10T15:36:14.536769+00:00 · methodology

0 comments
read the original abstract

Models of eclipsing binaries require the assignment of appropriate emergent intensities to the surface elements of the binary components. For distance-dependent modelling of flux-calibrated light curves, this necessitates an approximation of the absolute normal intensities of both components of the binary, as well as how their brightness varies across the stellar disks (limb darkening). Such surface intensities are often inferred from other physical properties of the synthetic binary (effective temperature, surface gravity, etc.) through the use of model atmospheres, which in turn are generally suited to a particular range of stellar types or parameters. Here, we present the major developments included in the PHOEBE 2.5 release (publicly available from http://phoebe-project.org), which improve the fidelity of model binaries comprising hot, compact stars. These developments include the incorporation model atmospheres produced using the Tubingen Model Atmosphere Package (TMAP) and Montreal/Tremblay codes (complementing the already incorporated PHOENIX and Castelli & Kurucz models, primarily suited to main sequences stars and low-temperature giants). Similarly, PHOEBE v2.5 now allows for blending/extrapolation of model atmospheres, meaning one can continue to make use of model atmospheres in cases when a small number of surface elements have parameters outside the model atmosphere grid. As an added value product, we also present tables of limb-darkening coefficients derived from the newly incorporated model atmospheres, such that they can be used as inputs in other binary modelling codes.

Figures

Figures reproduced from arXiv: 2607.07909 by Andrej Prsa, David Jones, Herbert Pablo, James Munday, Joseph Giammarco, Kelly Hambleton, Kyle Conroy, Marcin Wrona, Matthias Fabry, Michael Abdul-Masih, Nicole Reindl, Pier-Emmanuel Tremblay.

Figure 1
Figure 1. Figure 1: The normal intensity in SDSS-g ′ band as a function of surface gravity and effective temperature for the TMAP DA WD models. The white spaces are due to the sparser sampling of the grid for higher temperatures and regions where the models approach or exceed the Eddington limit. as the logarithmic Helium to Hydrogen number fraction (log(He/H)). 2.2. Limb-darkening properties of the TMAP models An example of … view at source ↗
Figure 2
Figure 2. Figure 2: The variation of emergent intensities in the SDSS-g band as a function of angle across the stellar disk for a TMAP sdO model with Teff = 70 kK, log g=6.0 and a log (He/H)=−0.97. The blue points show the TMAP sampling along the stellar disk, while the colored lines represent the fit to these points using different LD parameterisations. tween the sdO and DAO grids. Thus, we explore the key properties of the … view at source ↗
Figure 3
Figure 3. Figure 3: The SDSS g′ band linear limb-darkening coefficient (u, left) and normal intensity (I0, right) of the four TMAP model grids versus the log(He/H) abundance for models with effective temperature of 80kK and surface gravity of log g = 6.5. 1 2 3 4 5 TMAP I0 (1015 W m−2) 1 2 3 4 5 Tremblay I0 (1015 W m − 2) 20000 30000 40000 50000 60000 Teff (K) [PITH_FULL_IMAGE:figures/full_fig_p005_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: The normal intensities of the TMAP and Trem￾blay DA models in the SDSS g′ band, where the point size is proportional to the surface gravity and the color repre￾sents the effective temperature. The dashed line demarcates a perfect agreement between the models. agreement between the Tremblay intensities tabulated by Claret et al. (2020a) and the intensities in PHOEBE are good – again being within one standar… view at source ↗
Figure 6
Figure 6. Figure 6: A comparison of a 125 kK TMAP spectrum with blackbody spectra of different temperatures. Standard SDSS filter bandpasses are underplotted to highlight that the dif￾ferences are appreciable throughout the optical range. ries with lower temperature companions, they are often found to irradiate the face of the companion closest to them leading to a roughly sinusoidal variation as a func￾tion of orbital phase … view at source ↗
Figure 7
Figure 7. Figure 7: A synthetic binary comprising a pre-WD (Teff = 127 kK with TMAP atmospheres) in an 8-hr orbit with a K5V companion (solid black curve; TMAP). For comparison, the same model was run with a blackbody atmosphere for the pre-WD (dashed black line; BB), with a blackbody atmosphere and a reduced temperature (Teff ∼ 94 kK, dashed red line; labelled “BB 74% Teff ”) and with a blackbody atmosphere of reduced temper… view at source ↗
Figure 8
Figure 8. Figure 8: A synthetic binary with a custom user-defined migrating spot. The lower panel shows the synthetic light curve where the vertical dashed lines mark the times of the mesh plots shown in the upper panel. Both meshes are at the same orbital phase but the right-hand panel is one orbit later when the spot is closer to the line of sight, leading to a more pronounced change in flux as shown in the light curve. fro… view at source ↗
Figure 9
Figure 9. Figure 9: An example of sequential dimensionality reduction in 3 dimensions. projections of the point of interest (second panel). These are univariate interpolations. The process yields 4 vertices (depicted in open symbols), thereby reducing the initial dimension d = 3 by 1, to d − 1 = 2. The process is then repeated (third panel), this time along the second axis, a2, yielding 2 vertices, thereby reducing the dimens… 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

45 extracted references · 45 canonical work pages · 26 internal anchors

  1. [1]

    Gravity and limb-darkening coefficients for compact stars: DA, DB, and DBA eclipsing white dwarfs

    Gravity and limb-darkening coefficients for compact stars: DA, DB, and DBA eclipsing white dwarfs. , keywords =. doi:10.1051/0004-6361/201937326 , archivePrefix =. 2001.07129 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201937326 2001

  2. [2]

    and Hart, P

    Cover, T. and Hart, P. , journal=. Nearest neighbor pattern classification , year=

    work page

  3. [3]

    1981 , booktitle=

    A brief description of natural neighbor interpolation , author=. 1981 , booktitle=

    work page 1981

  4. [4]

    The origins of kriging

    Cressie, Noel. The origins of kriging. Mathematical Geology. 1990. doi:10.1007/BF00889887

    work page doi:10.1007/bf00889887 1990

  5. [5]

    , title =

    Hardy, Rolland L. , title =. Journal of Geophysical Research (1896-1977) , volume =. doi:https://doi.org/10.1029/JB076i008p01905 , url =. https://agupubs.onlinelibrary.wiley.com/doi/pdf/10.1029/JB076i008p01905 , abstract =

    work page doi:10.1029/jb076i008p01905 1977

  6. [6]

    Doppler beaming factors for white dwarfs, main sequence stars, and giant stars Limb-darkening coefficients for 3D (DA and DB) white dwarf models

    Doppler beaming factors for white dwarfs, main sequence stars, and giant stars. Limb-darkening coefficients for 3D (DA and DB) white dwarf models. , keywords =. doi:10.1051/0004-6361/202038436 , archivePrefix =. 2007.15715 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202038436 2007

  7. [7]

    Limb-Darkening Coefficients for Eclipsing White Dwarfs

    Limb-darkening Coefficients for Eclipsing White Dwarfs. , keywords =. doi:10.1088/0004-637X/766/1/3 , archivePrefix =. 1301.7091 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/766/1/3

  8. [8]

    Physics of Eclipsing Binaries. V. General Framework for Solving the Inverse Problem. , keywords =. doi:10.3847/1538-4365/abb4e2 , archivePrefix =. 2006.16951 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4365/abb4e2 2006

  9. [9]

    Physics of Eclipsing Binaries. IV. The Impact of Interstellar Extinction on the Light Curves of Eclipsing Binaries. , keywords =. doi:10.3847/1538-4365/ab7927 , archivePrefix =. 1912.09474 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4365/ab7927 1912

  10. [10]

    Physics of Eclipsing Binaries. III. Spin-Orbit Misalignment. , keywords =. doi:10.3847/1538-4365/aacd0f , archivePrefix =. 1806.07680 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4365/aacd0f

  11. [11]

    Physics Of Eclipsing Binaries. II. Toward the Increased Model Fidelity. , keywords =. doi:10.3847/1538-4365/227/2/29 , archivePrefix =. 1609.08135 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4365/227/2/29

  12. [12]

    Uncertainties in (E)UV model atmosphere fluxes

    Uncertainties in (E)UV model atmosphere fluxes. , keywords =. doi:10.1051/0004-6361:200809430 , archivePrefix =. 0802.1773 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:200809430

  13. [13]

    Stellar Atmosphere Modeling , year = 2003, editor =

    Handling of Atomic Data. Stellar Atmosphere Modeling , year = 2003, editor =

    work page 2003

  14. [14]

    Bolometric treatment of irradiation effects: general discussion and application to binary stars

    Bolometric Treatment of Irradiation Effects: General Discussion and Application to Binary Stars. , keywords =. doi:10.3847/1538-4365/aaffd7 , archivePrefix =. 1809.07963 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4365/aaffd7

  15. [15]

    Limb-darkening coefficients of illuminated atmospheres. I. Results for illuminated line-blanketed models with 3 700 K < T\_eff < 7 000 K. , keywords =. doi:10.1051/aas:1999456 , adsurl =

    work page doi:10.1051/aas:1999456

  16. [16]

    New models for the evolution of Post-Asymptotic Giant Branch stars and Central Stars of Planetary Nebulae

    New models for the evolution of post-asymptotic giant branch stars and central stars of planetary nebulae. , keywords =. doi:10.1051/0004-6361/201526577 , archivePrefix =. 1512.04129 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201526577

  17. [17]

    Binary stars as the key to understanding planetary nebulae

    Binary stars as the key to understanding planetary nebulae. Nature Astronomy , keywords =. doi:10.1038/s41550-017-0117 , archivePrefix =. 1705.00283 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1038/s41550-017-0117

  18. [18]

    and Prestwich, A

    The evolution of the theoretical bolometric albedo in close binary systems. , keywords =. doi:10.1046/j.1365-8711.2001.04783.x , adsurl =

    work page doi:10.1046/j.1365-8711.2001.04783.x 2001

  19. [19]

    A grid of synthetic ionizing spectra for very hot compact stars from NLTE model atmospheres

    A grid of synthetic ionizing spectra for very hot compact stars from NLTE model atmospheres. , keywords =. doi:10.1051/0004-6361:20030412 , archivePrefix =. astro-ph/0303464 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:20030412

  20. [20]

    Stellar Atmosphere Modeling , year = 2003, editor =

    Model Photospheres with Accelerated Lambda Iteration. Stellar Atmosphere Modeling , year = 2003, editor =

    work page 2003

  21. [21]

    RV variable, hot post-AGB stars from the MUCHFUSS project - Classification, atmospheric parameters, formation scenarios

    Radial velocity variable, hot post-AGB stars from the MUCHFUSS project. Classification, atmospheric parameters, formation scenarios. , keywords =. doi:10.1051/0004-6361/201527637 , archivePrefix =. 1601.00874 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201527637

  22. [22]

    Astropy: A Community Python Package for Astronomy

    doi:10.1051/0004-6361/201322068 , Eid =. arXiv , Author =:1307.6212 , Journal =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201322068

  23. [23]

    The Astropy Project: Building an inclusive, open-science project and status of the v2.0 core package

    The Astropy Project: Building an Open-science Project and Status of the v2.0 Core Package. , keywords =. doi:10.3847/1538-3881/aabc4f , archivePrefix =. 1801.02634 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-3881/aabc4f

  24. [24]

    Nature Methods , year = "2020", volume=

    SciPy 1.0: Fundamental Algorithms for Scientific Computing in Python. Nature Methods , year = "2020", volume=

    work page 2020

  25. [25]

    2006 , publisher=

    A guide to NumPy , author=. 2006 , publisher=

    work page 2006

  26. [26]

    Computing in Science and Engineering , keywords =

    Matplotlib: A 2D Graphics Environment. Computing in Science and Engineering , keywords =. doi:10.1109/MCSE.2007.55 , adsurl =

    work page doi:10.1109/mcse.2007.55 2007

  27. [27]

    GAIA Spectroscopy: Science and Technology , year = 2003, editor =

    Stellar atmospheres in eclipsing binary models. GAIA Spectroscopy: Science and Technology , year = 2003, editor =

    work page 2003

  28. [28]

    The solar-type eclipsing binary system LL Aquarii

    The solar-type eclipsing binary system LL Aquarii. , keywords =. doi:10.1051/0004-6361/201322195 , archivePrefix =. 1308.1320 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201322195

  29. [29]

    ELLC - a fast, flexible light curve model for detached eclipsing binary stars and transiting exoplanets

    ellc: A fast, flexible light curve model for detached eclipsing binary stars and transiting exoplanets. , keywords =. doi:10.1051/0004-6361/201628579 , archivePrefix =. 1603.08484 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201628579

  30. [30]

    doi:10.1088/978-0-7503-1287-5 , adsurl =

    Modeling and Analysis of Eclipsing Binary Stars; The theory and design principles of PHOEBE. doi:10.1088/978-0-7503-1287-5 , adsurl =

    work page doi:10.1088/978-0-7503-1287-5

  31. [31]

    , year = 1971, month = jun, volume =

    Realization of Accurate Close-Binary Light Curves: Application to MR Cygni. , year = 1971, month = jun, volume =. doi:10.1086/150986 , adsurl =

    work page doi:10.1086/150986 1971

  32. [32]

    A new extensive library of PHOENIX stellar atmospheres and synthetic spectra

    A new extensive library of PHOENIX stellar atmospheres and synthetic spectra. A&A , keywords =. 2013. doi:10.1051/0004-6361/201219058 , archivePrefix =. 1303.5632 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201219058 2013

  33. [33]

    Modelling of Stellar Atmospheres , year = 2003, editor =

    New Grids of ATLAS9 Model Atmospheres. Modelling of Stellar Atmospheres , year = 2003, editor =

    work page 2003

  34. [34]

    , keywords =

    Spectral analysis of the planetary nebula K 1-27 and its very hot hydrogen-deficient central star. , keywords =

    work page

  35. [35]

    Spectroscopic Analysis of DA White Dwarfs: Stark Broadening of Hydrogen Lines Including Non-Ideal Effects

    Spectroscopic Analysis of DA White Dwarfs: Stark Broadening of Hydrogen Lines Including Nonideal Effects. , keywords =. doi:10.1088/0004-637X/696/2/1755 , archivePrefix =. 0902.4182 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/696/2/1755

  36. [36]

    A Comprehensive Spectroscopic Analysis of DB White Dwarfs

    A Comprehensive Spectroscopic Analysis of DB White Dwarfs. , keywords =. doi:10.1088/0004-637X/737/1/28 , archivePrefix =. 1105.5433 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/737/1/28

  37. [37]

    , year = 1970, month = mar, volume =

    Nonlinear Limb Darkening for Early-Type Stars. , year = 1970, month = mar, volume =. doi:10.1086/110960 , adsurl =

    work page doi:10.1086/110960 1970

  38. [38]

    Abundances of Planetary Nebula NGC2392

    Abundances of planetary nebula NGC 2392. , keywords =. doi:10.1051/0004-6361:20079041 , archivePrefix =. 0801.2767 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:20079041

  39. [39]

    Non-LTE Line-blanketed Model Atmospheres of Hot Stars. I. Hybrid Complete Linearization/Accelerated Lambda Iteration Method. , keywords =. doi:10.1086/175226 , adsurl =

    work page doi:10.1086/175226

  40. [40]

    The bright blue side of the night sky: Spectroscopic survey of bright and hot (pre-) white dwarfs

    The bright blue side of the night sky: Spectroscopic survey of bright and hot (pre-) white dwarfs. , keywords =. doi:10.1051/0004-6361/202346865 , archivePrefix =. 2307.03721 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202346865

  41. [41]

    M., Lim , P

    The Astropy Project: Sustaining and Growing a Community-oriented Open-source Project and the Latest Major Release (v5.0) of the Core Package. , keywords =. doi:10.3847/1538-4357/ac7c74 , archivePrefix =. 2206.14220 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/ac7c74

  42. [42]

    An Eclipsing 47 minute Double White Dwarf Binary at 400 pc

    An eclipsing 47 min double white dwarf binary at 400 pc. , keywords =. doi:10.1093/mnras/stad2347 , archivePrefix =. 2308.00036 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stad2347

  43. [43]

    Spectroscopic analysis of DA white dwarfs with 3D model atmospheres

    Spectroscopic analysis of DA white dwarfs with 3D model atmospheres. , keywords =. doi:10.1051/0004-6361/201322318 , archivePrefix =. 1309.0886 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201322318

  44. [44]

    New Grids of Pure-Hydrogen White-Dwarf NLTE Model Atmospheres \newline and the HST/STIS Flux Calibration

    New Grids of Pure-hydrogen White Dwarf NLTE Model Atmospheres and the HST/STIS Flux Calibration. , keywords =. doi:10.3847/1538-3881/ab94b4 , archivePrefix =. 2005.10945 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-3881/ab94b4 2005

  45. [45]

    Lecture Notes in Mathematics, Berlin Springer Verlag , publisher =

    The Levenberg-Marquardt algorithm: Implementation and theory. Lecture Notes in Mathematics, Berlin Springer Verlag , publisher =. doi:10.1007/BFb0067700 , adsurl =

    work page doi:10.1007/bfb0067700