A Bag of Stellar Tracks and Isochrones...
last modification: 26 Feb 2009
The models do not include gravitational settling, radiative acceleration, convective overshooting, rotational mixing, but otherwise they are based on up-to-date physics, as described in: Pietrinferni, Cassisi, Salaris & Castelli (2006, ApJ, 642, 797) - Pietrinferni, Cassisi, Salaris & Castelli (2004, ApJ, 612, 168) - Cassisi, Salaris, Castelli & Pietrinferni (2004, ApJ, 616, 498) - Cassisi, Pietrinferni, Salaris, Castelli, Cordier & Castellani (2006, MemSaIt, 77, 71).
We strongly encourage people interested in a specific set of evolutionary tracks (not yet available in this database) to contact us, either by e_mail or by filling in the request form (present in this web site). We'll try to perform these computations within a week upon receiving the request.
All models have been computed by using the following alpha-enhanced heavy elements distribution:
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All models include mass loss according to the Reimers (1975) law (eta=0.2) and the mass range goes from 0.4Mo to 1.5Mo.
Each file contains:
in the fifth line - 1) the number of evolutionary points, 2) the global metallicity [M/H], 3) the abundance by mass of metals (Z), 4) the initial He abundance (Y), 5) the inital mass (in solar units); starting from the ninth line the following quantities are listed:
1 column) the logarithm of the age in years; 2 column) the actual mass in solar units; 3 column) the logarithm of the surface luminosity in solar units; 4 column) the logarithm of the effective temperature (K); 5 column) the visual absolute magnitude; 6 column) the (V-I) color; 7 column) the (V-R) color; 8 column) the (V-J) color; 9 column) the (V-K) color; 10 column) the (V-L) color; 11 column) the (H-K) color;from the Zero Age main Sequence to the Tip of Red Giant Branch (TRGB) (for masses larger than 0.6Mo).More details about the adopted color-Teff transformations and bolometric correction can be found in the quoted reference.
The coding of the file names is as follows:
bcdfZlmnYghiaes.nor
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| evolutionary track for a model with --> initial mass = bc.df Mo
--> metallicity Z= l.m • 10(-n)
--> initial He abundance Y = 0.ghi
--> mixture = alpha-enhanced (ae)
The suffix "nor" indicates that the evolutionary sequence has been "reduced" to a suitable number of points. This has been accomplished by fixing some key stage along the evolutionary path, and distributing for each track the same number of points between two consecutive stages. This allows a straightforward interpolation for producing isochrones of a given age, and for determining tracks and isochrones for other metallicities within the range spanned by the computed grid of models.
Example: 0130z402y303aes.nor_c04ae ---> 1.30 Mo canonical model with Z=4.0 • 10-2 and Y=0.303 |
The whole set of evolutionary models has been also transferred from the theoretical plane to the Advanced Camera for Survey (ACS) - on board of HST - Vega-mag. Each set of models can be downloaded as a single compressed tar archive. Each file contains:
on the fifth line - 1) the number of evolutionary points, 2) the global metallicity [M/H], 3) the abundance by mass of metals (Z), 4) the initial He abundance (Y), 5) the inital mass (in solar units); starting from the ninth line the following quantities are listed, from the Zero Age Main Sequence to the TRGB (for masses larger than 0.7Mo):
1 column) the logarithm of the age in years; 2 column) the actual mass in solar units; 3 column) the logarithm of the surface luminosity in solar units; 4 column) the logarithm of the effective temperature (K); 5 column) the F555W magnitude; 6 column) the F606W magnitude; 7 column) the F625W magnitude; 8 column) the F775W magnitude; 9 column) the F814W magnitude;
As for the choice of the key stages, in order to accurately sampling the morphology of the evolutionary tracks we have adopted 8 key stages along the evolutionary track, more in detail:
In this case low-mass stars denotes all objects which do not develop a convective core during the whole central H-burning phase; the high-mass structures are all the others.
For those structures which do not present the Bump along the RGB, we have - arbitrarily - chosen as representative of the key points 6 and 7, two points whose brightness was intermediate between the luminosities corresponding to the key points 5 and 8.
The correspondence between key stages and rows is the following:
For more details about the adopted key stages, please contact one of the authors.
For each chemical composition, we also provide a large set of horizontal branch (HB) models corresponding to the same RGB star progenitor - whose age at the RGB tip is of the order of 12/13Gyrs - but different assumptions about the total stellar mass of the HB structure.
The coding of the file names is as follows:
bcdfMpqZghiYlmncno.nor_c04aes
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| evolutionary track for a model with --> initial mass = b.cdf Mo
--> initial mass of the RGB progenitor
M = p.q Mo
--> metallicity Z= g.h • 10(-i)
--> initial He abundance of the
RGB progenitor Y = 0.lmn
--> misture = alpha-enhanced (ae)
The suffix "nor" indicates that the evolutionary sequence has been
"reduced" to a suitable number of points by fixing some key points
- suitable chosen - along the evolutionary track.
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Example:
0513m08z104y245cno.nor_c04ae ---> 0.513 Mo HB model with a canonical RGB progenitor with
mass equal to 0.8Mo, metallicity Z=1.0• 10-4 and initial
He content equal to Y=0.245.
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Each file contains:
on the fifth line - 1) the number of evolutionary points, 2) the global metallicity [M/H], 3) the abundance by mass of metals (Z), 4) the initial He abundance (Y), 5) the inital mass (in solar units); starting from the ninth line the following quantities are listed (from the ZAHB to the double shell burning or the beginning of the White dwarf cooling sequence):
1 column) the logarithm of the age in years (the age of 1Myr corresponds to the ZAHB); 2 column) the logarithm of the surface luminosity in solar units; 3 column) the logarithm of the effective temperature (K); 4 column) the visual absolute magnitude; 5 column) the (V-I) color; 6 column) the (V-R) color; 7 column) the (V-J) color; 8 column) the (V-K) color; 9 column) the (V-L) color; 10 column) the (H-K) color;
The full set of HB tracks can be downloaded as a single compressed tar archive.
The whole set of HB tracks has been also transferred (as for the evolutionary models from the Main Sequence to the TRGB) to the ACS. Also these sets of models can be downloaded as a single compressed tar archive. Each file contains:
on the fifth line - 1) the number of evolutionary points, 2) the global metallicity [M/H], 3) the abundance by mass of metals (Z), 4) the initial He abundance (Y), 5) the inital mass (in solar units); starting from the ninth line the following quantities are listed (from the ZAHB to the double shell burning or the beginning of the White dwarf cooling sequence):
1 column) the logarithm of the age in years (the age of 1Myr corresponds to the ZAHB); 2 column) the logarithm of the surface luminosity in solar units; 3 column) the logarithm of the effective temperature (K); 4 column) the F555W magnitude; 5 column) the F606W magnitude; 6 column) the F625W magnitude; 7 column) the F775W magnitude; 8 column) the F814W magnitude;
As for the choice of the key stages, in order to accurately sampling the morphology of the HB tracks we have adopted 9 key stages along the evolutionary track, more in detail:
The correspondence between key stages and rows is the following:
For more details about the adopted key stages, please contact one of the authors.
In case one is interested in the complete evolutionary track (i.e, a non normalized track) as well as for more information about the models (such as burnings, internal structure and so on) we will be pleased to provide them upon request. All comments/suggestions/requests are welcome. We hope that this database will be useful to your work!
Our best regards!!!
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