The Dartmouth Stellar Evolution Database

By Aaron Dotter, B. Chaboyer, Darko Jevremovic, V. Kostov, Eddie Baron, J. Ferguson. 2008

1,408 citations recorded by the source corpus.

The ever-expanding depth and quality of photometric and spectroscopic observations of stellar populations increase the need for theoretical models in regions of age-composition parameter space that are largely unexplored at present. Stellar evolution models that employ the most advanced physics and cover a wide range of compositions are needed to extract the most information from current observations of both resolved and unresolved stellar populations. The Dartmouth Stellar Evolution Database is a collection of stellar evolution tracks and isochrones that spans a range of [Fe/H] from –2.5 to +0.5, [α/Fe] from –0.2 to +0.8 (for [Fe/H] ⩽ 0) or +0.2 (for [Fe/H] > 0), and initial He mass fractions from Y = 0.245 to 0.40. Stellar evolution tracks were computed for masses between 0.1 and 4 M☉, allowing isochrones to be generated for ages as young as 250 Myr. For the range in masses where the core He flash occurs, separate He-burning tracks were computed starting from the zero age horizontal branch. The tracks and isochrones have been transformed to the observational plane in a variety of photometric systems including standard UBV(RI)C, Stromgren uvby, SDSS ugriz, 2MASS JHKs, and HST ACS/WFC and WFPC2. The Dartmouth Stellar Evolution Database is accessible through a Web site at http://stellar.dartmouth.edu/~models/ where all tracks, isochrones, and additional files can be downloaded.

Subfields: Astronomy and Astrophysics, Instrumentation, Statistical and Nonlinear Physics

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Citations in the corpus

STELLAR AND PLANETARY PROPERTIES OF K2 CAMPAIGN 1 CANDIDATES AND VALIDATION OF 17 PLANETS, INCLUDING A PLANET RECEIVING EARTH-LIKE INSOLATION (2015, methodology): “In this work, we use grids from the Dartmouth Stellar Evolution Database (Dotter et al. 2008) at Solar values of [α/ Fe] = 0.0 and helium abundance Y = 0.2741, which come packaged with the isochrones module.”
PLANET HUNTERS: A TRANSITING CIRCUMBINARY PLANET IN A QUADRUPLE STAR SYSTEM (2012, methodology): “In Figure 14 we present another comparison using models from the Dartmouth series (Dotter et al. 2008), in which the physical ingredients (including the equation of state and the non-gray boundary conditions between the interior and the atmosphere) are more realistic for stars significantly below…”
EIGHT ULTRA-FAINT GALAXY CANDIDATES DISCOVERED IN YEAR TWO OF THE DARK ENERGY SURVEY (2015, methodology): “To assess the error contribution from intrinsic uncertainty in the isochrone, we resample the posterior distribution using the Dartmouth isochrone family (Dotter et al. 2008).”
COUNTING LOW-MASS STARS IN INTEGRATED LIGHT (2011, methodology): “Such a shift can be caused for example by a change in [α/Fe] by±0.2 or [Fe/H] by±0.1 dex (e.g., Dotter et al. 2007, 2008).”
ZODIACAL EXOPLANETS IN TIME (ZEIT). III. A SHORT-PERIOD PLANET ORBITING A PRE-MAIN-SEQUENCE STAR IN THE UPPER SCORPIUS OB ASSOCIATION (2016, methodology): “We comparing our observables to two grids of PMS models computed with an updated version of the Dartmouth stellar evolution code (Dotter et al. 2008; Feiden & Chaboyer 2012).”
SOAR TESS Survey. I. Sculpting of TESS Planetary Systems by Stellar Companions (2019, methodology): “…companions in the scenario where they are bound to the target star were estimated using the observed contrast ratio in the TESS band (approximated using the I bandpass of SOAR) and finding the radius of an appropriately fainter star within the Dartmouth stellar models (Dotter et al. 2008).”
THE INNER EDGE OF THE HABITABLE ZONE FOR SYNCHRONOUSLY ROTATING PLANETS AROUND LOW-MASS STARS USING GENERAL CIRCULATION MODELS (2016, methodology): “In this srudy, we used the Dartmouth stellar evolution database (Dotter et al. 2008)2 to obtain L? and M? for both low ([Fe/H] = −0.5) and high ([Fe/H] = 0.3) metallicities, as a function of Teff .”
THE CHEMICAL EVOLUTION OF THE DRACO DWARF SPHEROIDAL GALAXY (2009, methodology): “Superposed in this figure are isochrones from the Dartmouth Stellar Evolution Database (Dotter et al. 2008) for [Fe/H] −2.5 dex with [α/Fe] = +0.2 dex (solid lines) and for [Fe/H] −1.5 dex with [α/Fe] Solar (dashed lines) for ages 9 and 12.5 Gyr.”
MESA ISOCHRONES AND STELLAR TRACKS (MIST) 0: METHODS FOR THE CONSTRUCTION OF STELLAR ISOCHRONES (2016, background): “Many of the isochrone libraries in use today, such as BaSTI (Pietrinferni et al. 2004), Dartmouth (Dotter et al. 2008), PARSEC (Bressan et al. 2012), Pisa (Tognelli et al. 2011), Victoria-Regina (VandenBerg et al. 2006), and YaleYonsei (Yi et al. 2001), are based on the more-sophisticated approach,…”
Evolutionary stellar population synthesis with MILES – II. Scaled-solar and α-enhanced models (2015, background): “…spectra (e.g. Coelho et al. 2005; Munari et al. 2005), and isochrones with varying [α/Fe] abundance (e.g. Salaris & Weiss 1998; Salasnich et al. 2000; VandenBerg et al. 2000; Pietrinferni et al. 2006; Coelho et al. 2007; Dotter et al. 2008; VandenBerg et al. 2014; Kim et al. in preparation).”
THE GHOSTS SURVEY. I. HUBBLE SPACE TELESCOPE ADVANCED CAMERA FOR SURVEYS DATA (2011, methodology): “Using isochrones from the Dartmouth Stellar Evolution Database (Dotter et al. 2008), decreasing the age of a [Fe/H] = −1.0 RGB population from 10 to 3.33 Gyr shifts the color at half a magnitude below the TRGB by −0.11 mag.”
A self-consistent, absolute isochronal age scale for young moving groups in the solar neighbourhood (2015, methodology): “In this study we adopt four sets of semi-empirical model isochrones based on different interior models, namely the Dotter et al. (2008), Tognelli et al. (2011), Bressan et al. (2012) and Baraffe et al. (2015) models (hereafter referred to as Dartmouth, Pisa, PARSEC and BHAC15 respectively)1.”
WASP-121 b: a hot Jupiter close to tidal disruption transiting an active F star (2015, methodology): “To model the stars, we used the Dartmouth stellar evolution tracks of Dotter et al. (2008) and the BT-SETTL stellar atmosphere models of Allard et al. (2012) that we integrated in each individual bandpass.”
Homogeneous studies of transiting extrasolar planets – IV. Thirty systems with space-based light curves (2011, background): “As in Paper III Iuse five sets of model predictions:Claret (Claret 2004, 2005, 2006, 2007), Y2 (Demarque et al. 2004),Teramo(Pietrinferni et al. 2004),VRSS (VandenBerg et al. 2006) andDSEP(Dotter et al. 2008).”
TERRESTRIAL PLANET OCCURRENCE RATES FOR THE KEPLER GK DWARF SAMPLE (2015, methodology): “With an improved observational database, Huber et al. (2014) derive stellar parameters by fitting the observations to isochrones from the Dartmouth Stellar Evolution Database (Dotter et al. 2008) using a χ2 minimization.”
A catalogue of masses, structural parameters, and velocity dispersion profiles of 112 Milky Way globular clusters (2018, methodology): “We determined the stellar mass functions from the luminosity functions by fitting either Dartmouth (Dotter et al. 2008) or PARSEC isochrones (Bressan et al. 2012) to the HST color-magnitude diagrams.”
LOW FALSE POSITIVE RATE OF KEPLER CANDIDATES ESTIMATED FROM A COMBINATION OF SPITZER AND FOLLOW-UP OBSERVATIONS (2015, methodology): “However, Huber et al. (2013) recently updated the stellar properties using data from Quarter 1-16 and different observational techniques, but homogeneously extract the parameters from the Dartmouth stellar isochrones (Dotter et al. 2008).”
SPECTRO-THERMOMETRY OF M DWARFS AND THEIR CANDIDATE PLANETS: TOO HOT, TOO COOL, OR JUST RIGHT? (2013, methodology): “Metallicity B12 finds that radius is insensitive to metallicity, in contrast to model predictions (Baraffe et al. 1998; Dotter et al. 2008).”