Modules for Experiments in Stellar Astrophysics (Mesa)

Paxton, Bill; Bildsten, Lars; Dotter, Aaron; Herwig, Falk; Lesaffre, Pierre; Timmes, F. X.

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

Cited by 4,124 publications

(4,075 citation statements)

References 155 publications

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“…The structure of the giant stars were calculated using the stellar evolution code Modules for Experiments in Stellar Astrophysics (mesa ; Paxton et al 2011Paxton et al , 2013. We used two stellar structures, evolved from the same 3.5-M⊙, zeroage main sequence, solar metallicity model.…”

Section: Methodsmentioning

confidence: 99%

Hydrodynamic simulations of the interaction between giant stars and planets

Staff

Marco

Wood

et al. 2016

Mon. Not. R. Astron. Soc.

127

100

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We present the results of hydrodynamic simulations of the interaction between a 10 Jupiter mass planet and a red or asymptotic giant branch stars, both with a zeroage main sequence mass of 3.5 M ⊙ . Dynamic in-spiral timescales are of the order of few years and a few decades for the red and asymptotic giant branch stars, respectively. The planets will eventually be destroyed at a separation from the core of the giants smaller than the resolution of our simulations, either through evaporation or tidal disruption. As the planets in-spiral, the giant stars' envelopes are somewhat puffed up. Based on relatively long timescales and even considering the fact that further inspiral should take place before the planets are destroyed, we predict that the merger would be difficult to observe, with only a relatively small, slow brightening. Very little mass is unbound in the process. These conclusions may change if the planet's orbit enhances the star's main pulsation modes. Based on the angular momentum transfer, we also suspect that this star-planet interaction may be unable to lead to large scale outflows via the rotation-mediated dynamo effect of Nordhaus and Blackman. Detectable pollution from the destroyed planets would only result for the lightest, lowest metallicity stars. We furthermore find that in both simulations the planets move through the outer stellar envelopes at Mach-3 to Mach-5, reaching Mach-1 towards the end of the simulations. The gravitational drag force decreases and the in-spiral slows down at the sonic transition, as predicted analytically.

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Section: Methodsmentioning

confidence: 99%

Hydrodynamic simulations of the interaction between giant stars and planets

Staff

Marco

Wood

et al. 2016

Mon. Not. R. Astron. Soc.

127

100

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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%

“…First, MESA, used by Verma and Ball, is a recent evolution code. Some results of the MESA code have been compared with those of another code in Paxton et al (2011). However the comparisons of the MESA interior structures have not been shown with many details.…”

Section: Analysis Of Model Differencesmentioning

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)

Cited by 4,124 publications

References 155 publications

Hydrodynamic simulations of the interaction between giant stars and planets

Hydrodynamic simulations of the interaction between giant stars and planets

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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