J/A+A/533/A109 Pisa pre-main sequence tracks and isochrones (Tognelli+, 2011)
The Pisa pre-main sequence tracks and isochrones.
A database covering a wide range of Z, Y, mass, and age values.
Tognelli E., Prada Moroni P. G., Degl'Innocenti S.
<Astron. Astrophys. 533, A109 (2011)>
=2011A&A...533A.109T 2011A&A...533A.109T
ADC_Keywords: Stars, pre-main sequence ; Models, evolutionary ; Isochrones ;
Abundances ; Stars, ages ; Stars, masses
Keywords: stars: pre-main sequence - stars: evolution - stars: formation -
stars: interiors - stars: low-mass -
Hertzsprung-Russel and C-M diagrams
Abstract:
In recent years new observations of pre-main sequence stars (pre-MS)
with Z<Z☉ have been made available. To take full advantage of
the continuously growing amount of data of pre-MS stars in different
environments, we need to develop updated pre-MS models for a wide
range of metallicity to assign reliable ages and masses to the
observed stars. We present updated evolutionary pre-MS models and
isochrones for a fine grid of mass, age, metallicity, and helium
values. We use a standard and well-tested stellar evolutionary code
(i.e. FRANEC), that adopts outer boundary conditions from detailed and
realistic atmosphere models. In this code, we incorporate additional
improvements to the physical inputs related to the equation of state
and the low temperature radiative opacities essential to computing
low-mass stellar models.
We make available via internet a large database of pre-MS tracks and
isochrones for a wide range of chemical compositions (Z=0.0002-0.03),
masses (M=0.2-7.0M☉), and ages (1-100Myr) for a solar-calibrated
mixing length parameter alpha (i.e. 1.68). For each chemical
composition, additional models were computed with two different mixing
length values, namely alpha=1.2 and 1.9.
Moreover, for Z≥0.008, we also provided models with two different
initial deuterium abundances. The characteristics of the models have
been discussed in detail and compared with other work in the
literature. The main uncertainties affecting theoretical predictions
have been critically discussed.
Comparisons with selected data indicate that there is close agreement
between theory and observation.
Description:
Evolutionary tracks and Isochrones in the log L vs log Te plane,
for the following chemical compositions:
Z Y Y Y
2.00E-04 0.230 0.249 0.250
1.00E-03 0.232 0.251 0.254
2.00E-03 0.234 0.253 0.259
3.00E-03 0.236 0.254 0.263
4.00E-03 0.238 0.256 0.269
5.00E-03 0.240 0.258 0.273
6.00E-03 0.242 0.260 0.279
7.00E-03 0.244 0.262 0.283
8.00E-03 0.246 0.265 0.289
9.00E-03 0.248 0.267 0.294
1.00E-02 0.250 0.268 0.299
1.25E-02 0.255 0.274 0.311
1.50E-02 0.260 0.278 0.323
1.75E-02 0.265 0.284 0.336
2.00E-02 0.270 0.288 0.349
2.25E-02 0.275 0.294 0.361
2.50E-02 0.280 0.299 0.374
2.75E-02 0.285 0.304 0.386
3.00E-02 0.290 0.308 0.398
Each model is calculated with an initial Deuterium abundance
XD=4.0E-05. For Z≥0.008, models with XD=2.0E-05 are available,
too.
Each model is calculated with three different values of the mixing
length parameter alpha = 1.20, 1.68 (solar calibrated), 1.90.
There is also a dataset for our Standard Solar Model parameters
(Z=0.01377, Y=0.2533, alpha=1.68, XD=2.0E-05).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
datasets.dat 74 272 Table of different choices of physical parameters
trk.dat 148 11696 Table of stellar tracks parameters
iso.dat 149 9792 Table of isochrones parameters
trk/*/* . 272 Stellar tracks for pre-main sequence, M=0.2 to 7
iso/*/* . 272 Isochrone tables, age=1 to 100Myr
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See also:
http://astro.df.unipi.it/stellar-models/ : Stellar models Home Page
Description of file: trk/*/*
Stellar tracks of different initial masses and same physical
parameters (i.e. a "dataset") are grouped in subdirectories under trk/
The subdirectory names of the datasets are in the form:
Zz.zzzzzYy.yyyyXDdEdMLa.aaAS05
where:
Zz.zzzzz is the metallicity, 19 values from 0.00020 to 0.03000
Yy.yyy is the Helium abundance, three different values for each Z
XDdEd is the Deuterium abundance, two values: "XD2E5" for 2E-2,
and "XD4E5" for 4E-5.
MLa.aa is the mixing length parameter, three values: 1.2, 1.68, 1.9
AS05 indicates the Asplund et al. 2005 Solar mixture
Inside each dataset, names of the stellar tracks are in the form:
TRKMm.mmZz.zzzzzYy.yyyyXDdEdMLa.aaAS05.DAT
where:
M.m.mm is the initial mass in solar units, from 0.20 to 7.00.
Description of file: iso/*/*
Isochrone tables of different ages and same physical
parameters (i.e. a "dataset") are grouped in subdirectories under iso/
The subdirectory names of the datasets are in the form:
Zz.zzzzzYy.yyyyXDdEdMLa.aaAS05
where:
Zz.zzzzz is the metallicity, 19 values from 0.00020 to 0.03000
Yy.yyy is the Helium abundance, three different values for each Z
XDdEd is the Deuterium abundance, two values: "XD2E5" for 2E-2,
and "XD4E5" for 4E-5.
MLa.aa is the mixing length parameter, three values: 1.2, 1.68, 1.9
AS05 indicates the Asplund et al. 2005 Solar mixture
Inside each dataset, names of the isochrone tables are in the form:
ISOAaaaaaZz.zzzzzYy.yyyyXDdEdMLa.aaAS05.DAT
where:
Aaaaaa is the isochrone age in Myr, from 1 to 100.
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Byte-by-byte Description of file (#): datasets.dat
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Bytes Format Units Label Explanations
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1- 35 A35 --- dataset Dataset name
40- 46 F7.5 --- Z Metallicity
51- 55 F5.3 --- Y Helium abundance
60- 66 E7.1 --- XD Deuterium abundance
71- 74 F4.2 --- ML Mixing length parameter
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Byte-by-byte Description of file (#): trk.dat
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Bytes Format Units Label Explanations
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1- 4 F4.2 Msun M Stellar initial mass, in solar units
9- 15 F7.5 --- Z Metallicity
20- 24 F5.3 --- Y Helium abundance
29- 35 E7.1 --- XD Deuterium abundance
40- 43 F4.2 --- ML Mixing length parameter
60- 97 A38 --- dir Directory
101-150 A50 --- file Filename
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Byte-by-byte Description of file (#): iso.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 I4 Myr Age Isochrone age
9- 15 F7.5 --- Z Metallicity
20- 24 F5.3 --- Y Helium abundance
29- 35 E7.1 --- XD Deuterium abundance
40- 43 F4.2 --- ML Mixing length parameter
60- 97 A38 --- dir Directory
101-150 A50 --- file Filename
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Byte-by-byte Description of file (#): trk/*/*
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
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1- 4 I4 --- NMD Model number
5- 16 F12.8 [yr] logAge Age of the model: log(AGE/yr)
19- 24 F6.3 --- Xc Central Hydrogen abundance
26- 34 F9.5 [Lsun] logL Total luminosity: log(L/Lsun)
36- 44 F9.5 [K] logTe Effective temperature: log(Te/K)
46- 54 F9.5 [K] logTc Central Temperature: log(Tc/K)
56- 64 F9.5 [g/cm3] logrhoC Central Density: log(rhoC/(g/cm^3))
66- 74 F9.5 Msun Mcc Mass of convective core
77- 86 E10.3 --- Lpp Luminosity of PP chain
(in units of the total luminosity L)
89- 98 E10.3 --- Lcno Luminosity of CNO cycle
(in units of the total luminosity L)
101-110 E10.3 --- Lgra Gravitational luminosity
(in units of the total luminosity L)
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Byte-by-byte Description of file (#): iso/*/*
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Bytes Format Units Label Explanations
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3- 13 F11.8 [Lsun] logL Total luminosity: log(L/Lsun)
16- 26 F11.8 [K] logTe Effective temperature: log(Te/K)
29- 39 F11.8 Msun M Stellar mass: M/Msun
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History:
Pier Giorgio Prada Moroni, prada(at)df.unipi.it
(End) Patricia Vannier [CDS] 20-Jul-2011