arxiv: 2604.24596 · v1 · submitted 2026-04-27 · 🌌 astro-ph.SR · astro-ph.EP

Recognition: unknown

A Theoretical Study of the Structure and Elemental Abundances of HD 20794

Mrinmay Medhi , Mami Deka , Krishna Saha , Vivek Baruah Thapa , Upakul Mahanta

Authors on Pith no claims yet

Pith reviewed 2026-05-08 01:22 UTC · model grok-4.3

classification 🌌 astro-ph.SR astro-ph.EP

keywords HD 20794MESA stellar modelselemental abundancesmetal-poor G dwarfstellar evolutionplanetary system hostcore-collapse supernovaeGalactic chemical enrichment

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The pith

Models show HD 20794 is a 0.80 solar-mass star about 9 Gyr old that has retained its birth chemical abundances.

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

The paper computes a grid of MESA stellar evolution models for the nearby metal-poor G dwarf HD 20794 to determine its mass, age, and interior structure while testing whether observed surface abundances match the star's original composition. A sympathetic reader would care because this star hosts planets, including one near the habitable zone, and serves as a benchmark for how low-metallicity stars evolve without losing their natal chemistry over long timescales. The authors run 252 models spanning masses from 0.78 to 0.80 solar masses with variations in convective efficiency, resolution, and boundary conditions, then select the best fits through chi-squared comparison to measured temperature, gravity, luminosity, radius, and age. The favored models match all observed properties and recover the full abundance pattern across light elements, alpha-elements, and odd-Z species such as phosphorus and chlorine, which align with core-collapse supernova yields.

Core claim

The best-fit MESA models favor a mass of 0.80 solar masses and an age of about 9 Gyr for HD 20794, reproducing all observed stellar properties within uncertainties. They also successfully recover the observed surface abundance pattern over a wide range of elements, including light elements, alpha-elements, and the odd-Z species phosphorus and chlorine. Comparison with nucleosynthesis yields from massive stars suggests that the measured phosphorus and chlorine abundances are compatible with enrichment from core-collapse supernovae and have remained preserved during stellar evolution.

What carries the argument

A grid of 252 MESA stellar evolution models with initial masses between 0.78 and 0.80 solar masses, varying convective efficiency, numerical resolution, and atmospheric boundary conditions, selected by chi-squared minimization against observed effective temperature, surface gravity, luminosity, radius, and age.

If this is right

The star's surface abundances have remained unchanged since formation and match predictions from core-collapse supernova enrichment.
Low-mass metal-poor G dwarfs retain their natal chemical signatures over Gyr timescales.
Standard stellar evolution theory describes HD 20794 accurately and applies to similar planet-hosting stars.
Such stars can serve as reliable probes of Galactic chemical enrichment without correction for evolutionary surface changes.

Where Pith is reading between the lines

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

The approach could be extended to other nearby planet-hosting dwarfs to test whether abundance preservation holds across different metallicities.
If abundances stay fixed, they could be used directly to reconstruct the chemical conditions at the time of planet formation.
Independent checks via asteroseismology on this star would test whether the model-derived interior structure is correct.

Load-bearing premise

The MESA models with standard physics and adjusted convective efficiency fully capture the star's interior structure without extra mixing or diffusion processes altering surface abundances over time.

What would settle it

Spectroscopic data showing that phosphorus or chlorine abundances in HD 20794 have changed significantly from supernova-yield expectations, or asteroseismic measurements revealing interior density or temperature profiles inconsistent with the best-fit 0.80 solar-mass model.

Figures

Figures reproduced from arXiv: 2604.24596 by Krishna Saha, Mami Deka, Mrinmay Medhi, Upakul Mahanta, Vivek Baruah Thapa.

**Figure 1.** Figure 1: Evolutionary tracks of HD 20794 computed with MESA, showing the time evolution of effective temperature (Teff), surface gravity (log g), luminosity (L/L⊙), and radius (R/R⊙) as a function of stellar age. All models were computed assuming an initial metallicity Z ≃ 0.005 and helium abundances in the range Y = 0.2525–0.2575, corresponding to ΔY/ΔZ = 1.5–2.5 at fixed metallicity. Coloured curves represent mod… view at source ↗

**Figure 2.** Figure 2: Two-dimensional contour maps showing the dependence of Teff, L/L⊙, log g, and R/R⊙ on stellar mass and mixing-length parameter at an age of 9 Gyr for Z = 0.0050 view at source ↗

**Figure 3.** Figure 3: HR diagram showing the location of HD 20794 (filled star) together with MESA evolutionary tracks computed for stellar masses and mixing-length parameters near the best-fit solution. Solid and dashed curves correspond to models spanning the preferred parameter range (M ≃ 0.78–0.80 M⊙, 𝛼MLT = 1.4, Z ≃ 0.0050). For comparison, several nearby solar-type stars with welldetermined parameters (HD 10700, HD 6582,… view at source ↗

**Figure 4.** Figure 4: Time evolution of central and surface mass fractions for selected elements in the best-fit MESA model of HD 20794. Top panels: Central (left) and surface (right) abundances as a function of stellar age. Bottom panels: Central (left) and surface (right) abundances as a function of central temperature. which HD 20794 inherited its chemical composition from gas enriched primarily by earlier generations of ma… view at source ↗

read the original abstract

HD~20794 is a nearby, bright, metal-poor G-type dwarf hosting a compact planetary system, including a super-Earth near the habitable zone. Its low stellar activity and the availability of precise radial-velocity and photometric data make it an excellent benchmark for studying stellar structure and chemical abundances in low-metallicity planet-hosting stars. We present, to our knowledge, the first grid-based stellar evolution analysis of HD~20794 using \texttt{MESA}, focusing on its main-sequence and late main-sequence evolution. A set of 252 stellar models was computed for initial masses between $0.78$ and $0.80\,M_{\odot}$, varying convective efficiency, numerical resolution, and atmospheric boundary conditions. Models were selected through $\chi^2$ minimization using observed constraints on effective temperature, surface gravity, luminosity, radius, and age. The best-fit models favor a mass of $0.80\,M_{\odot}$ and an age of about $9$~Gyr, reproducing all observed stellar properties within uncertainties. They also successfully recover the observed surface abundance pattern over a wide range of elements, including light elements, $\alpha$-elements, and the odd-$Z$ species phosphorus and chlorine. Comparison with nucleosynthesis yields from massive stars suggests that the measured phosphorus and chlorine abundances are compatible with enrichment from core-collapse supernovae and have remained preserved during stellar evolution. Our results support standard stellar evolution theory, indicating that low-mass, metal-poor G dwarfs such as HD~20794 can retain their natal chemical signatures over Gyr timescales. This highlights their importance as probes of stellar evolution, Galactic chemical enrichment, and the chemical environments associated with long-lived planetary systems.

Editorial analysis

A structured set of objections, weighed in public.

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

Desk Editor's Note private letter to a colleague

A careful MESA grid for HD 20794 recovers its mass, age, and full abundance pattern including P and Cl, but stays a narrow case study.

read the letter

HD 20794 gets a careful MESA treatment here. The authors built a 252-model grid around 0.78-0.80 solar masses, tweaked convective efficiency and boundary conditions, and used chi-squared to match the star's temperature, gravity, luminosity, radius, and age. The best fits land at 0.8 solar masses and roughly 9 Gyr, and the models recover the full observed abundance pattern, including the odd-Z elements phosphorus and chlorine. This appears to be the first grid-based MESA run for this particular star. They show that standard stellar evolution can explain the abundances without extra mixing or diffusion, and the P and Cl levels line up with yields from massive star supernovae. That supports the idea that low-mass metal-poor dwarfs keep their birth chemistry over billions of years. The work is solid on its own terms. The narrow mass range makes sense for a well-constrained star, and varying the mixing length addresses one obvious uncertainty. The comparison to nucleosynthesis yields adds an independent check. Still, the scope stays narrow. It's one object, so claims about broader galactic chemistry or planet-hosting stars rest on how representative HD 20794 is. The abstract does not spell out the exact chi-squared values or how many models were close to the minimum, which leaves some room for hidden degeneracies. They also assume the surface abundances reflect the initial composition, which is plausible but could be tested with more detailed diffusion calculations. This paper is mainly for specialists who need a benchmark model for HD 20794 or similar stars in chemical evolution studies. A reader interested in stellar interiors or abundance preservation will find the numbers useful. It is worth sending to peer review because the modeling is reproducible and the target is observationally important, even if the advance is incremental.

Referee Report

2 major / 2 minor

Summary. The manuscript reports the first grid-based MESA stellar evolution study of the metal-poor G dwarf HD 20794. A 252-model grid is computed for initial masses 0.78–0.80 M⊙, varying convective efficiency (mixing-length parameter), numerical resolution, and atmospheric boundary conditions. Best-fit models are identified via χ² minimization against observed Teff, log g, luminosity, radius, and age, yielding a preferred mass of 0.80 M⊙ and age of ~9 Gyr. These models are shown to reproduce the observed surface abundance pattern across light elements, α-elements, and odd-Z species including phosphorus and chlorine. The P and Cl abundances are further compared to core-collapse supernova nucleosynthesis yields, supporting the conclusion that the surface abundances have been preserved since formation and that standard stellar evolution suffices for this star.

Significance. If the central results hold, the work supplies a concrete, reproducible benchmark for a nearby, low-metallicity planet-hosting star whose precise observational constraints make it suitable for testing stellar interiors and chemical evolution. The explicit exploration of convective efficiency and boundary conditions, together with the recovery of a broad abundance pattern without additional mixing or diffusion, strengthens the case that such stars retain natal signatures over Gyr timescales and can serve as anchors for Galactic enrichment studies.

major comments (2)

[Abstract and model-selection section] Abstract and model-selection section: the χ² selection is performed on Teff, log g, luminosity, radius, and age only; the subsequent claim that the models 'successfully recover' the full observed abundance pattern (including P and Cl) is therefore a post-hoc consistency check rather than a prediction from the fit. It is unclear whether the initial abundances in the MESA grid were set to the observed values or to a standard solar-scaled mixture, which directly affects how much weight the 'recovery' carries for the preservation argument.
[Abundance comparison and nucleosynthesis section] Abundance comparison and nucleosynthesis section: the statement that the measured P and Cl abundances 'are compatible with enrichment from core-collapse supernovae' is presented without a quantitative metric (e.g., reduced χ² or yield-matching residuals) or an explicit statement of the assumed supernova progenitor mass range and metallicity. This weakens the link between the stellar models and the independent nucleosynthesis check.

minor comments (2)

[Model grid description] The mass interval 0.78–0.80 M⊙ is narrow; a brief justification citing prior mass estimates for HD 20794 would help readers assess whether the grid boundaries truncate plausible degeneracies with age and mixing length.
[Discussion of abundance preservation] The manuscript states that surface abundances have 'remained preserved'; a short paragraph summarizing the expected magnitude of gravitational settling and radiative levitation for P and Cl at this Teff and metallicity would make the no-mixing assumption more transparent.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive review and recommendation for minor revision. We address each major comment below, agreeing where clarification is needed and outlining the changes we will make to strengthen the manuscript.

read point-by-point responses

Referee: [Abstract and model-selection section] Abstract and model-selection section: the χ² selection is performed on Teff, log g, luminosity, radius, and age only; the subsequent claim that the models 'successfully recover' the full observed abundance pattern (including P and Cl) is therefore a post-hoc consistency check rather than a prediction from the fit. It is unclear whether the initial abundances in the MESA grid were set to the observed values or to a standard solar-scaled mixture, which directly affects how much weight the 'recovery' carries for the preservation argument.

Authors: We agree that the χ² minimization was performed solely on the stellar parameters Teff, log g, luminosity, radius, and age, rendering the abundance comparison a post-hoc consistency check rather than a fitted prediction. This was intentional, as the central aim is to show that standard MESA evolution, calibrated only to global properties, reproduces the full observed abundance pattern (including P and Cl) without extra mixing or diffusion. In the grid, initial abundances were set to a solar-scaled mixture scaled to the star's overall metallicity, not to the individual observed values; the evolved surface abundances at the best-fit age then match the observations. We will revise the abstract and model-selection section to explicitly state the initial abundance setup and to describe the abundance match as a validation of natal abundance preservation. revision: yes
Referee: [Abundance comparison and nucleosynthesis section] Abundance comparison and nucleosynthesis section: the statement that the measured P and Cl abundances 'are compatible with enrichment from core-collapse supernovae' is presented without a quantitative metric (e.g., reduced χ² or yield-matching residuals) or an explicit statement of the assumed supernova progenitor mass range and metallicity. This weakens the link between the stellar models and the independent nucleosynthesis check.

Authors: We acknowledge that adding a quantitative metric and explicit details on the nucleosynthesis comparison would strengthen the section. The observed P and Cl abundances were compared to core-collapse supernova yields for progenitor masses 10–25 M⊙ at metallicities near [Fe/H] ≈ −0.5, appropriate for the star's age and composition; the values lie within the predicted yield ranges. In the revision we will add a quantitative measure (e.g., residuals or reduced χ² for the best-matching yields), state the progenitor mass range and metallicity assumptions explicitly, and clarify how this supports the preservation argument. revision: yes

Circularity Check

0 steps flagged

No significant circularity detected

full rationale

The paper's central derivation consists of computing a finite grid of MESA models (masses 0.78–0.80 M⊙, varying convective efficiency and boundary conditions), applying χ² minimization to the independent observables Teff, log g, luminosity, radius, and age, and then performing a separate consistency check that the evolved surface abundances match the observed pattern (with an external comparison of P and Cl to supernova yields). No equation or selection step reduces by construction to the fitted quantities themselves, no uniqueness theorem is imported via self-citation, and the abundance recovery is not presented as a statistical prediction forced by the same data used in the fit. The procedure is therefore self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

3 free parameters · 2 axioms · 0 invented entities

The analysis rests on fitting a grid of MESA models whose physics inputs and boundary conditions are varied to match observations; the claim that abundances are preserved relies on the assumption that standard stellar evolution does not alter surface composition over 9 Gyr.

free parameters (3)

initial stellar mass = 0.80 M_sun
Varied in narrow range 0.78-0.80 solar masses and selected via chi-squared minimization against observations
convective efficiency (mixing length parameter)
Varied across the 252-model grid to achieve best fit
stellar age = ~9 Gyr
Determined by selecting models that match observed properties

axioms (2)

domain assumption Standard MESA stellar evolution physics (no extra mixing, diffusion, or non-standard processes)
Invoked throughout the grid computation and abundance preservation claim
domain assumption Observed surface abundances reflect natal composition from galactic enrichment
Used to interpret phosphorus and chlorine matches with supernova yields

pith-pipeline@v0.9.0 · 5629 in / 1510 out tokens · 58152 ms · 2026-05-08T01:22:34.827024+00:00 · methodology

discussion (0)

Reference graph

Works this paper leans on

48 extracted references · 45 canonical work pages · 2 internal anchors

[1]

write newline

" write newline "" before.all 'output.state := FUNCTION fin.entry write newline FUNCTION new.block output.state before.all = 'skip after.block 'output.state := if FUNCTION new.sentence output.state after.block = 'skip output.state before.all = 'skip after.sentence 'output.state := if if FUNCTION not #0 #1 if FUNCTION and 'skip pop #0 if FUNCTION or pop #1...
[2]

M., & Grevesse, N

Asplund M., Amarsi A. M., Grevesse N., 2021, @doi [Astronomy & Astrophysics] 10.1051/0004-6361/202140445 , 653, A141

work page doi:10.1051/0004-6361/202140445 2021
[3]

S., 2006, @doi [The Astronomical Journal] 10.1086/508515 , 132, 2326–2332

Balser D. S., 2006, @doi [The Astronomical Journal] 10.1086/508515 , 132, 2326–2332

work page doi:10.1086/508515 2006
[4]

Bensby T., Feltzing S., 2005, @doi [Proceedings of the International Astronomical Union] 10.1017/s1743921305006381 , 1, 531–532

work page doi:10.1017/s1743921305006381 2005
[5]

Bonfanti A., Ortolani S., Nascimbeni V., 2015, @doi [Astronomy & Astrophysics] 10.1051/0004-6361/201527297 , 585, A5

work page doi:10.1051/0004-6361/201527297 2015
[6]

Cambridge University Press, @doi 10.1017/cbo9780511623004

Böhm-Vitense E., 1989, Introduction to Stellar Astrophysics. Cambridge University Press, @doi 10.1017/cbo9780511623004

work page doi:10.1017/cbo9780511623004 1989
[7]

Caffau E., Bonifacio P., Faraggiana R., Steffen M., 2011, @doi [Astronomy & Astrophysics] 10.1051/0004-6361/201117313 , 532, A98

work page doi:10.1051/0004-6361/201117313 2011
[8]

Casagrande L., Schönrich R., Asplund M., Cassisi S., Ramírez I., Meléndez J., Bensby T., Feltzing S., 2011, @doi [Astronomy & Astrophysics] 10.1051/0004-6361/201016276 , 530, A138

work page doi:10.1051/0004-6361/201016276 2011
[9]

C., Pepe F., 2021, @doi [Astronomy & Astrophysics] 10.1051/0004-6361/202140986 , 653, A43

Cretignier M., Dumusque X., Hara N. C., Pepe F., 2021, @doi [Astronomy & Astrophysics] 10.1051/0004-6361/202140986 , 653, A43

work page doi:10.1051/0004-6361/202140986 2021
[10]

Cretignier M., Dumusque X., Aigrain S., Pepe F., 2023, @doi [Astronomy & Astrophysics] 10.1051/0004-6361/202347232 , 678, A2

work page doi:10.1051/0004-6361/202347232 2023
[11]

H., Fields B

Cyburt R. H., Fields B. D., Olive K. A., Yeh T.-H., 2016, @doi [Reviews of Modern Physics] 10.1103/revmodphys.88.015004 , 88

work page doi:10.1103/revmodphys.88.015004 2016
[12]

W., Lee H., Worthey G., Jevremović D., Baron E., 2007, @doi [The Astrophysical Journal] 10.1086/519946 , 666, 403–412

Dotter A., Chaboyer B., Ferguson J. W., Lee H., Worthey G., Jevremović D., Baron E., 2007, @doi [The Astrophysical Journal] 10.1086/519946 , 666, 403–412

work page doi:10.1086/519946 2007
[13]

Feng F., Tuomi M., Jones H. R. A., 2017, @doi [Astronomy & Astrophysics] 10.1051/0004-6361/201730406 , 605, A103

work page doi:10.1051/0004-6361/201730406 2017
[14]

, keywords =

Fischer D. A., Valenti J., 2005, @doi [The Astrophysical Journal] 10.1086/428383 , 622, 1102–1117

work page doi:10.1086/428383 2005
[15]

Gaia DR3 E., 2023, Gaia Data Release 3 (Gaia DR3), Version 1.1 , https://www.cosmos.esa.int/web/gaia/data-release-3, @doi 10.5270/esa-qa4lep3

work page doi:10.5270/esa-qa4lep3 2023
[16]

Holmberg J., Nordström B., Andersen J., 2007, @doi [Astronomy & Astrophysics] 10.1051/0004-6361:20077221 , 475, 519–537

work page doi:10.1051/0004-6361:20077221 2007
[17]

W., 2012, FreeEOS: Equation of State for stellar interiors calculations, Astrophysics Source Code Library

Irwin A. W., 2012, FreeEOS: Equation of State for stellar interiors calculations, Astrophysics Source Code Library

2012
[18]

S., Schwab J., Bauer E., Timmes F

Jermyn A. S., Schwab J., Bauer E., Timmes F. X., Potekhin A. Y., 2021, @doi [The Astrophysical Journal] 10.3847/1538-4357/abf48e , 913, 72

work page doi:10.3847/1538-4357/abf48e 2021
[19]

, keywords =

Johnson J. A., Aller K. M., Howard A. W., Crepp J. R., 2010, @doi [Publications of the Astronomical Society of the Pacific] 10.1086/655775 , 122, 905–915

work page doi:10.1086/655775 2010
[20]

2013, Stellar Structure and Evolution, doi: 10.1007/978-3-642-30304-3

Kippenhahn R., Weigert A., Weiss A., 2012, Stellar Structure and Evolution. Springer Berlin Heidelberg, @doi 10.1007/978-3-642-30304-3

work page doi:10.1007/978-3-642-30304-3 2012
[21]

I., & Lugaro, M

Kobayashi C., Karakas A. I., Lugaro M., 2020, @doi [The Astrophysical Journal] 10.3847/1538-4357/abae65 , 900, 179

work page doi:10.3847/1538-4357/abae65 2020
[22]

W., Granzer T., Görgei A., 2023, @doi [Astronomy & Astrophysics] 10.1051/0004-6361/202245767 , 674, A143

Kriskovics L., Kővári Z., Seli B., Oláh K., Vida K., Henry G. W., Granzer T., Görgei A., 2023, @doi [Astronomy & Astrophysics] 10.1051/0004-6361/202245767 , 674, A143

work page doi:10.1051/0004-6361/202245767 2023
[23]

G., Pilachowski C

Maas Z. G., Pilachowski C. A., Cescutti G., 2017, @doi [The Astrophysical Journal] 10.3847/1538-4357/aa7050 , 841, 108

work page doi:10.3847/1538-4357/aa7050 2017
[24]

G., Hawkins K., Hinkel N

Maas Z. G., Hawkins K., Hinkel N. R., Cargile P., Janowiecki S., Nelson T., 2022, @doi [The Astronomical Journal] 10.3847/1538-3881/ac77f8 , 164, 61

work page doi:10.3847/1538-3881/ac77f8 2022
[25]

Magic Z., Chiavassa A., Collet R., Asplund M., 2014, @doi [Astronomy & Astrophysics] 10.1051/0004-6361/201423804 , 573, A90

work page doi:10.1051/0004-6361/201423804 2014
[26]

Springer Berlin Heidelberg, p

Matteucci F., 2011, Chemical Evolution of Irregular Galaxies. Springer Berlin Heidelberg, p. 171–194, @doi 10.1007/978-3-642-22491-1_7

work page doi:10.1007/978-3-642-22491-1_7 2011
[27]

P., Mahanta U., 2023, @doi [Journal of Astrophysics and Astronomy] 10.1007/s12036-023-09913-3 , 44

Medhi M., Mahanta D. P., Mahanta U., 2023, @doi [Journal of Astrophysics and Astronomy] 10.1007/s12036-023-09913-3 , 44

work page doi:10.1007/s12036-023-09913-3 2023
[28]

C., Sousa S., Israelian G., Mayor M., Udry S., 2013, @doi [Astronomy & Astrophysics] 10.1051/0004-6361/201220707 , 551, A112

Mortier A., Santos N. C., Sousa S., Israelian G., Mayor M., Udry S., 2013, @doi [Astronomy & Astrophysics] 10.1051/0004-6361/201220707 , 551, A112

work page doi:10.1051/0004-6361/201220707 2013
[29]

Nari N., et al., 2025, @doi [Astronomy & Astrophysics] 10.1051/0004-6361/202451769 , 693, A297

work page doi:10.1051/0004-6361/202451769 2025
[30]

Paxton B., Bildsten L., Dotter A., Herwig F., Lesaffre P., Timmes F., 2010, @doi [The Astrophysical Journal Supplement Series] 10.1088/0067-0049/192/1/3 , 192, 3

work page doi:10.1088/0067-0049/192/1/3 2010
[31]

Paxton B., et al., 2013, @doi [The Astrophysical Journal Supplement Series] 10.1088/0067-0049/208/1/4 , 208, 4

work page internal anchor Pith review doi:10.1088/0067-0049/208/1/4 2013
[32]

Paxton B., et al., 2015, @doi [The Astrophysical Journal Supplement Series] 10.1088/0067-0049/220/1/15 , 220, 15

work page internal anchor Pith review doi:10.1088/0067-0049/220/1/15 2015
[33]

Paxton B., et al., 2018, @doi [The Astrophysical Journal Supplement Series] 10.3847/1538-4365/aaa5a8 , 234, 34

work page doi:10.3847/1538-4365/aaa5a8 2018
[34]

Paxton B., et al., 2019, @doi [The Astrophysical Journal Supplement Series] 10.3847/1538-4365/ab2241 , 243, 10

work page doi:10.3847/1538-4365/ab2241 2019
[35]

Peimbert M., Torres-Peimbert S., 1974, @doi [The Astrophysical Journal] 10.1086/153166 , 193, 327

work page doi:10.1086/153166 1974
[36]

Pepe F., et al., 2011, @doi [Astronomy & Astrophysics] 10.1051/0004-6361/201117055 , 534, A58

work page doi:10.1051/0004-6361/201117055 2011
[37]

Y., & Chabrier, G

Potekhin A. Y., Chabrier G., 2010, @doi [Contributions to Plasma Physics] 10.1002/ctpp.201010017 , 50, 82–87

work page doi:10.1002/ctpp.201010017 2010
[38]

2003, MNRAS, 339, 937, doi: 10.1046/j.1365-8711.2003.06241.x G¨ otberg, Y., de Mink, S

Reddy B. E., Tomkin J., Lambert D. L., Prieto C. A., 2003, @doi [Monthly Notices of the Royal Astronomical Society] 10.1046/j.1365-8711.2003.06305.x , 340, 304–340

work page doi:10.1046/j.1365-8711.2003.06305.x 2003
[39]

Ritter C., Herwig F., Jones S., Pignatari M., Fryer C., Hirschi R., 2018, @doi [Monthly Notices of the Royal Astronomical Society] 10.1093/mnras/sty1729 , 480, 538–571

work page doi:10.1093/mnras/sty1729 2018
[40]

J., & Nayfonov, A

Rogers F. J., Nayfonov A., 2002, @doi [The Astrophysical Journal] 10.1086/341894 , 576, 1064–1074

work page doi:10.1086/341894 2002
[41]

Wiley, @doi 10.1002/0470033452 , http://dx.doi.org/10.1002/0470033452

Salaris M., Cassisi S., 2005, Evolution of Stars and Stellar Populations. Wiley, @doi 10.1002/0470033452 , http://dx.doi.org/10.1002/0470033452

work page doi:10.1002/0470033452 2005
[42]

M., 1995, @doi [The Astrophysical Journal Supplement Series] 10.1086/192204 , 99, 713

Saumon D., Chabrier G., van Horn H. M., 1995, @doi [The Astrophysical Journal Supplement Series] 10.1086/192204 , 99, 713

work page doi:10.1086/192204 1995
[43]

G., et al., 2015, @doi [Astronomy & Astrophysics] 10.1051/0004-6361/201425227 , 576, A94

Sousa S. G., et al., 2015, @doi [Astronomy & Astrophysics] 10.1051/0004-6361/201425227 , 576, A94

work page doi:10.1051/0004-6361/201425227 2015
[44]

X., & Swesty, F

Timmes F. X., Swesty F. D., 2000, @doi [The Astrophysical Journal Supplement Series] 10.1086/313304 , 126, 501–516

work page doi:10.1086/313304 2000
[45]

F., 2013, @doi [The Astrophysical Journal] 10.1088/0004-637x/769/1/18 , 769, 18

Trampedach R., Asplund M., Collet R., Nordlund A., Stein R. F., 2013, @doi [The Astrophysical Journal] 10.1088/0004-637x/769/1/18 , 769, 18

work page doi:10.1088/0004-637x/769/1/18 2013
[46]

A., Arnett D., 2005, @doi [The Astrophysical Journal] 10.1086/426131 , 618, 908–918

Young P. A., Arnett D., 2005, @doi [The Astrophysical Journal] 10.1086/426131 , 618, 908–918

work page doi:10.1086/426131 2005
[47]

A., Mamajek E

Young P. A., Mamajek E. E., Arnett D., Liebert J., 2001, @doi [The Astrophysical Journal] 10.1086/321559 , 556, 230–244

work page doi:10.1086/321559 2001
[48]

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