The Stellar Evolution CodeThe Dartmouth Stellar Evolution Program (DSEP) is a state of the art stellar evolution code and has been featured in several publications. Some of the sources of the input physics used by DSEP are listed on the Related Links page.
A selection of published papers relating to DSEP (most recent first):
- Accurate Low-mass Stellar Models of KOI-126
G. Feiden, B. Chaboyer, & A. Dotter (ADS)
- The Dartmouth Stellar Evolution Database
A. Dotter, B. Chaboyer, D. Jevremovic, V. Kostov, E. Baron, & J. W. Ferguson (ADS)
- Stellar Population Models and Individual Element Abundances I: Sensitivity of Stellar Evolution Models
A. Dotter, B. Chaboyer, J. W. Ferguson, H-c. Lee, G. Worthey, D. Jevremovic, & E. Baron (ADS)
- The ACS Galactic Globular Cluster Survey. II. Stellar Evolution Tracks, Isochrones, Luminosity Functions, and Synthetic Horizontal Branch Models
A. Dotter, B. Chaboyer, D. Jevremovic, E. Baron, J. W. Ferguson, A. Sarajedini, & J. Anderson (ADS)
- Theoretical Uncertainties in Red Giant Branch Evolution: The Red Giant Branch Bump
S. R. Bjork, & B. Chaboyer (ADS)
- Stellar Pollution and [Fe/H] in the Hyades
A. Dotter & B. Chaboyer (ADS)
- The Impact of Pollution on Stellar Evolution Models
A. Dotter & B. Chaboyer (ADS)
- Theoretical Uncertainties in the Subgiant Mass-Age Relation and the Absolute Age of omega Centauri
B. Chaboyer & L. M. Krauss (ADS)
- Heavy-Element Diffusion in Metal-poor Stars
B. Chaboyer, W. H. Fenton, J. E. Nelan, D. J. Patnaude, & F. E. Simon (ADS)
Isochrones and Stellar Evolution TracksThe isochrones and stellar evolution tracks are tabulated in several photometric systems (see next section for more details).
Isochrones are tabulated on the following age grid:
- 0.25 - 1 Gyr in 50 Myr intervals
- 1 - 5 Gyr in 250 Myr intervals
- 5 - 15 Gyr in 500 Myr intervals
Stellar evolution tracks are provided for masses ranging from 0.1 - 4 Msun in most cases with the following mass intervals:
- 0.1 - 1.8 Msun in steps of 0.05 Msun
- 1.8 - 3 Msun in steps of 0.1 Msun
- 3 - 4 Msun in steps of 0.2 Msun
Color-Teff TransformationsThis page lists each of the photometric systems the isochrones have been transformed to. The names in each list refer to the suffix found on the corresponding isochrone file.
ACS Galactic Globular Cluster SurveyIsochrones intended for use with the ACS GGC Survey (see Related Links) are available in both synthetic and empirical colors. Both sets include groundbased B, V, and I magnitudes as well F606W and F814W for both ACS-WFC and WFPC2 systems. All HST magnitudes are on the VegaMAG system.
- phx - Synthetic magnitudes using Bessell and Sirianni filter curves
- cmd - Semi-empirical magnitudes using Vandenberg & Clem BVI with Sirianni transformations
Synthetic ColorsPHOENIX synthetic fluxes (see Related Links for the PHOENIX website) are used below 10,000 K. Castelli & Kurucz synthetic fluxes are used above 10,000 K.
The following are the sources for the filter transmission curves. The table at the bottom of the page lists the filters included in each system.
- jc2mass - UBV(RI)c from Bessell (1990) (ADS) and JHKs from 2MASS
- hst_acs - HST/ACS-WFC from Sirianni et al. (2005) (ADS; ACS website)
- hst_wfpc2 - HST/WFPC2 from Sirianni et al. (2005)
- ugriz - SDSS DR 6 flux calibration page
- irac - Spitzer IRAC spectral response
- hst_wfc3 - HST/WFC3 UVIS and IR channels from J. Kalirai (2009, private communication)
Semi-Empirical ColorsSemi-empirically colors and bolometric corrections from the following sources are also used:
|Photometric System||Filters (and Combinations)|
|Bessell + 2MASS||U||B||V||Rc||Ic||J||H||Ks|
|ACS GGC Survey||B||V||Ic||F606W||F814W||F606W||F814W|
NOTE: WFC3 has too many filters to fit into the table above. Click here for a legend that links column number to filter.