Modules for Experiments in Stellar Astrophysics (Mesa): Planets, Oscillations, Rotation, and Massive Stars

Paxton, Bill; Cantiello, Matteo; Arras, Phil; Bildsten, Lars; Brown, Edward F.; Dotter, Aaron; Mankovich, Christopher; Montgomery, M. H.; Stello, Dennis; Timmes, F. X.; Townsend, R. H. D.

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

Cited by 3,250 publications

(3,256 citation statements)

References 210 publications

(261 reference statements)

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“…3.1 because it leads to a convective core decrease that is much too fast as a result of the strong stabilizing influence of the µ-gradient term during core hydrogen burning. One can expect an even faster shrinking than that found in Paxton et al (2013) in their Fig. 13 and a Hertzsprung-Russell track still less compatible with observations than what they found in their Fig.…”

Section: The Chemical Composition and Its Gradient Are Discontinuouscontrasting

confidence: 45%

“…The numerous methods tested recently by Paxton et al (2013) clearly show that stellar evolution results are very sensitive to the choice that is made. The answer to these questions cannot be found from comparing numerical results obtained with different assumptions in stellar evolution codes since other uncertainties affect stellar modeling.…”

Section: Introductionmentioning

confidence: 99%

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Proper use of Schwarzschild Ledoux criteria in stellar evolution computations

Gabriel

Noels

Montalbán

et al. 2014

A&A

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The era of detailed asteroseismic analyses opened by space missions such as CoRoT and Kepler has highlighted the need for stellar models devoid of numerical inaccuracies, in order to be able to diagnose which physical aspects are being ignored or poorly treated in standard stellar modeling. We tackle here the important problem of fixing convective zone boundaries in the frame of the local mixing length theory. First we show that the only correct way to locate a convective zone boundary is to find, at each iteration step, through interpolations or extrapolations from points within the convective zone, the mass where the radiative luminosity is equal to the total luminosity. We then discuss two misuses of the boundary condition and the ways they affect stellar modeling and stellar evolution. The first consists in applying the neutrality condition for convective instability on the radiative side of the convective boundary. The second way of misusing the boundary condition comes from the process of fixing the convective boundary through the search for a change of sign of a possibly discontinuous function. We show that these misuses can lead to completely wrong estimates of convective core sizes with important consequences for the following evolutionary phases. We point out the advantages of using a double mesh point at each convective zone boundary. The specific problem of a convective shell is discussed and some remarks concerning overshooting are given.

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Section: The Chemical Composition and Its Gradient Are Discontinuouscontrasting

confidence: 45%

Section: Introductionmentioning

confidence: 99%

Proper use of Schwarzschild Ledoux criteria in stellar evolution computations

Gabriel

Noels

Montalbán

et al. 2014

A&A

View full text Add to dashboard Cite

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“…The grid of models was computed using the MESA code (Paxton et al 2011(Paxton et al , 2013. We computed 21 masses in a range between M = 0.6 − 2.5M⊙, in combination with 7 dif- • The tracks were computed starting from the pre-main sequence (PMS) up to the first thermal pulse of the asymptotic giant branch (TP-AGB).…”

Section: Physical Inputsmentioning

confidence: 99%

Determining stellar parameters of asteroseismic targets: going beyond the use of scaling relations

Rodrigues

Bossini

Miglio

et al. 2017

Mon. Not. R. Astron. Soc.

104

119

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Asteroseismic parameters allow us to measure the basic stellar properties of field giants observed far across the Galaxy. Most of such determinations are, up to now, based on simple scaling relations involving the large frequency separation, ∆ν, and the frequency of maximum power, ν max . In this work, we implement ∆ν and the period spacing, ∆P , computed along detailed grids of stellar evolutionary tracks, into stellar isochrones and hence in a Bayesian method of parameter estimation. Tests with synthetic data reveal that masses and ages can be determined with typical precision of 5 and 19 per cent, respectively, provided precise seismic parameters are available. Adding independent information on the stellar luminosity, these values can decrease down to 3 and 10 per cent respectively. The application of these methods to NGC 6819 giants produces a mean age in agreement with those derived from isochrone fitting, and no evidence of systematic differences between RGB and RC stars. The age dispersion of NGC 6819 stars, however, is larger than expected, with at least part of the spread ascribable to stars that underwent mass-transfer events.

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“…Grid model parameters (Paxton et al 2011(Paxton et al , 2013. 6) Nuclear Astrophysics Compilation of REaction rates (Angulo et al 1999).…”

Section: Stellar Model Comparisonsmentioning

confidence: 99%

A seismic and gravitationally bound double star observed byKepler

Appourchaux

Antia

Ball

et al. 2015

A&A

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Context. Solar-like oscillations have been observed by Kepler and CoRoT in many solar-type stars, thereby providing a way to probe stars using asteroseismology. Aims. The derivation of stellar parameters has usually been done with single stars. The aim of the paper is to derive the stellar parameters of a double-star system (HIP 93511), for which an interferometric orbit has been observed along with asteroseismic measurements. Methods. We used a time series of nearly two years of data for the double star to detect the two oscillation-mode envelopes that appear in the power spectrum. Using a new scaling relation based on luminosity, we derived the radius and mass of each star. We derived the age of each star using two proxies: one based upon the large frequency separation and a new one based upon the small frequency separation. Using stellar modelling, the mode frequencies allowed us to derive the radius, the mass, and the age of each component. In addition, speckle interferometry performed since 2006 has enabled us to recover the orbit of the system and the total mass of the system. Results. From the determination of the orbit, the total mass of the system is 2.34 +0.45 −0.33 M . The total seismic mass using scaling relations is 2.47 ± 0.07 M . The seismic age derived using the new proxy based upon the small frequency separation is 3.5 ± 0.3 Gyr. Based on stellar modelling, the mean common age of the system is 2.7-3.9 Gyr. The mean total seismic mass of the system is 2.34-2.53 M consistent with what we determined independently with the orbit. The stellar models provide the mean radius, mass, and age of the stars as R A = 1.82−1.87 R , M A = 1.25−1.39 M , Age A = 2.6-3.5 Gyr; R B = 1.22−1.25 R , M B = 1.08−1.14 M , Age B = 3.35-4.21 Gyr. The models provide two sets of values for Star A: [1.25-1.27] M and [1.34-1.39] M . We detect a convective core in Star A, while Star B does not have any. For the metallicity of the binary system of Z ≈ 0.02, we set the limit between stars having a convective core in the range [1.14-1.25] M .

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Modules for Experiments in Stellar Astrophysics (Mesa): Planets, Oscillations, Rotation, and Massive Stars

Cited by 3,250 publications

References 210 publications

Proper use of Schwarzschild Ledoux criteria in stellar evolution computations

Proper use of Schwarzschild Ledoux criteria in stellar evolution computations

Determining stellar parameters of asteroseismic targets: going beyond the use of scaling relations

A seismic and gravitationally bound double star observed byKepler

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