The ACS Survey of Galactic Globular Clusters. II. Stellar Evolution Tracks, Isochrones, Luminosity Functions, and Synthetic Horizontal-Branch Models

Dotter, Aaron; Chaboyer, Brian; Jevremović, D.; Baron, E.; Ferguson, Jason W.; Sarajedini, Ata; Anderson, Jay

doi:10.1086/517915

Cited by 281 publications

(385 citation statements)

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“…The surface temperature and pressure of the star are usually set close to the photosphere, either through the use of a T − τ relation, or via the use of pre-computed model atmospheres. Dotter et al (2007) show the effects of the choice of T − τ relation on a 1 M model, together with models computed using PHOENIX model atmospheres. They find that while the location of the red giant branch can be substantially affected by the choice of the relation, the main sequence is not strongly influenced.…”

Section: Discussionmentioning

confidence: 99%

“…The version employed here is that of Stancliffe & Eldridge (2009) which was developed for doing binary stellar evolution. The code treats all forms of mixing by means of a diffusive formalism (Eggleton 1972 Bjork & Chaboyer (2006) and Dotter et al (2007). The models used here come from the work of Dotter et al (2008) and are available online 6 .…”

Section: Introductionmentioning

confidence: 99%

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Confronting uncertainties in stellar physics

Stancliffe

Fossati

Passy

et al. 2016

A&A

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We assess the systematic uncertainties in stellar evolutionary calculations for low-to intermediate-mass, main-sequence stars. We compare published stellar tracks from several different evolution codes with our own tracks computed using the stellar codes stars and mesa. In particular, we focus on tracks of 1 and 3 M at solar metallicity. We find that the spread in the available 1 M tracks (computed before the recent solar composition revision) can be covered by tracks between 0.97−1.01 M computed with the stars code. We assess some possible causes of the origin of this uncertainty, including how the choice of input physics and the solar constraints used to perform the solar calibration affect the tracks. We find that for a 1 M track, uncertainties of around 10% in the initial hydrogen abundance and initial metallicity produce around a 2% error in mass. For the 3 M tracks, there is very little difference between the tracks from the various different stellar codes. The main difference comes in the extent of the main sequence, which we believe results from the different choices of the implementation of convective overshooting in the core. Uncertainties in the initial abundances lead to a 1−2% error in the mass determination. These uncertainties cover only part of the total error budget, which should also include uncertainties in the input physics (e.g., reaction rates, opacities, convective models) and any missing physics (e.g., radiative levitation, rotation, magnetic fields). Uncertainties in stellar surface properties such as luminosity and effective temperature will further reduce the accuracy of any potential mass determinations.

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Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Confronting uncertainties in stellar physics

Stancliffe

Fossati

Passy

et al. 2016

A&A

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“…Salaris & Weiss 1998;Buzzoni et al 1983), which also affects RGB and HB lifetimes. We selected works that provide an extended database of tracks and isochrones with solar-scaled and α-enhanced chemical compositions for the required age range: BaSTI database (Pietrinferni et al 2004(Pietrinferni et al , 2006, Dartmouth (Dotter et al 2007(Dotter et al , 2008, and Padova STEV (Bertelli et al 2008(Bertelli et al , 2009. Obviously, the quoted models do not exhaust the rich and composite scenario of stellar evolutionary calculations.…”

Section: Comparison With Recent Stellar Model Databasesmentioning

confidence: 99%

The Pisa Stellar Evolution Data Base for low-mass stars

Dell’Omodarme

Valle

Degl’Innocenti

et al. 2012

A&A

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Context. The last decade showed an impressive observational effort from the photometric and spectroscopic point of view for ancient stellar clusters in our Galaxy and beyond, leading to important and sometimes surprising results. Aims. The theoretical interpretation of these new observational results requires updated evolutionary models and isochrones spanning a wide range of chemical composition so that the possibility of multipopulations inside a stellar cluster is also taken also into account. Methods. With this aim we built the new "Pisa Stellar Evolution Database" of stellar models and isochrones by adopting a welltested evolutionary code (FRANEC) implemented with updated physical and chemical inputs. In particular, our code adopts realistic atmosphere models and an updated equation of state, nuclear reaction rates and opacities calculated with recent solar elements mixture. Results. A total of 32 646 models have been computed in the range of initial masses 0.30 ÷ 1.10 M for a grid of 216 chemical compositions with the fractional metal abundance in mass, Z, ranging from 0.0001 to 0.01, and the original helium content, Y, from 0.25 to 0.42. Models were computed for both solar-scaled and α-enhanced abundances with different external convection efficiencies. Correspondingly, 9720 isochrones were computed in the age range 8÷15 Gyr, in time steps of 0.5 Gyr. The whole database is available to the scientific community on the web. Models and isochrones were compared with recent calculations available in the literature and with the color-magnitude diagram of selected Galactic globular clusters. The dependence of relevant evolutionary quantities, namely turn-off and horizontal branch luminosities, on the chemical composition and convection efficiency were analyzed in a quantitative statistical way and analytical formulations were made available for reader's convenience. These relations can be useful in several fields of stellar evolution, e.g. evolutionary properties of binary systems, synthetic models for simple stellar populations and for star counts in galaxies, and chemical evolution models of galaxies.

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“…Stellar evolution calculations were carried out using two codes: DSEP (Dotter et al 2007) and MESA (an open source stellar evolution code developed by B. Paxton and collaborators; http://mesa.sourceforge.net/). The input physics employed by DSEP and MESA are similar for the models presented here.…”

Section: Stellar Evolution Model Comparisonmentioning

confidence: 99%

Evolutionary implications of the new triple-α nuclear reaction rate for low mass stars

Dotter

Paxton

2009

A&A

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Context. Ogata et al. (2009, Progr. Theor. Phys., 122, 1055 presented a theoretical determination of the 4 He(αα, γ) 12 C, or triple-α, nuclear reaction rate. Their rate differs from the NACRE rate by many orders of magnitude at temperatures relevant for low mass stars. Aims. We explore the evolutionary implications of adopting the OKK triple-α reaction rate in low mass stars and compare the results with those obtained using the NACRE rate. Methods. The triple-α reaction rates are compared by following the evolution of stellar models at 1 and 1.5 M with Z = 0.0002 and Z = 0.02. Results. Results show that the OKK rate has severe consequences for the late stages of stellar evolution in low mass stars. Most notable is the shortening-or disappearance-of the red giant phase. Conclusions. The OKK triple-α reaction rate is incompatible with observations of extended red giant branches and He burning stars in old stellar systems.

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The ACS Survey of Galactic Globular Clusters. II. Stellar Evolution Tracks, Isochrones, Luminosity Functions, and Synthetic Horizontal-Branch Models

Cited by 281 publications

References 47 publications

Confronting uncertainties in stellar physics

Confronting uncertainties in stellar physics

The Pisa Stellar Evolution Data Base for low-mass stars

Evolutionary implications of the new triple-α nuclear reaction rate for low mass stars

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