J/A+A/540/A26 Pisa Evolution Models for low-mass stars (Dell'Omodarme+, 2012)
The Pisa Stellar Evolution Data Base for low-mass stars.
Dell'Omodarme M., Valle G., Degl'Innocenti S., Prada Moroni P.G.
<Astron. Astrophys. 540, A26 (2012)>
=2012A&A...540A..26D 2012A&A...540A..26D (SIMBAD/NED BibCode)
ADC_Keywords: Stars, horizontal branch ; Models, evolutionary ; Isochrones ;
Abundances ; Stars, ages ; Stars, masses
Keywords: stars: horizontal-branch - stars: evolution -
Hertzsprung-Russell and C-M diagrams - stars: low-mass -
stars: interiors - globular clusters: general
Abstract:
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.
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. With this aim we built the new "Pisa Stellar Evolution
Database" of stellar models and isochrones by adopting a well-tested
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.
A total of 32646 models have been computed in the range of initial
masses 0.30-1.10M☉ 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 alpha-enhanced abundances with
different external convection efficiencies. Correspondingly, 9720
isochrones were computed in the age range 8-15Gyr, in time steps of
0.5Gyr. 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.
Description:
Evolutionary tracks and Isochrones in the log L vs log Te plane,
for the following chemical compositions:
Z Y Y Y Y Y Y
0.0001 0.249 0.250 0.270 0.330 0.380 0.420
0.0002 0.249 0.250 0.270 0.330 0.380 0.420
0.0003 0.249 0.250 0.270 0.330 0.380 0.420
0.0004 0.249 0.250 0.270 0.330 0.380 0.420
0.0005 0.250 0.250 0.270 0.330 0.380 0.420
0.0006 0.250 0.250 0.270 0.330 0.380 0.420
0.0007 0.250 0.250 0.270 0.330 0.380 0.420
0.0008 0.250 0.250 0.270 0.330 0.380 0.420
0.0009 0.250 0.250 0.270 0.330 0.380 0.420
0.0010 0.250 0.250 0.270 0.330 0.380 0.420
0.0020 0.252 0.250 0.270 0.330 0.380 0.420
0.0030 0.254 0.250 0.270 0.330 0.380 0.420
0.0040 0.256 0.250 0.270 0.330 0.380 0.420
0.0050 0.258 0.250 0.270 0.330 0.380 0.420
0.0060 0.260 0.250 0.270 0.330 0.380 0.420
0.0070 0.262 0.250 0.270 0.330 0.380 0.420
0.0080 0.264 0.250 0.270 0.330 0.380 0.420
0.0090 0.266 0.250 0.270 0.330 0.380 0.420
0.0100 0.268 0.250 0.270 0.330 0.380 0.420
Each model is calculated with three different values of the mixing
length parameter alpha=1.70, 1.80, 1.90 and two different
alpha-enhancement [alpha/Fe]=0.0, 0.3.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
datasets.dat 54 648 Table of different choices of physical parameters
for trk, hb and iso
hb.dat 132 5554 Table of stellar tracks parameters from ZAHB to
thermal pulses (M=0.55 to 1.1)
hbgrid.dat 131 16729 Table of stellar tracks parameters from ZAHB to
thermal pulses/grid (different ZAHB initial masses
for one Mini) (M=0.55 to 1.1)
trk.dat 120 11016 Table of stellar tracks parameters from
pre-main sequence (M=0.3 to 1.1)
zahb.dat 68 648 Table of ZAHB models parameters
iso.dat 113 9720 Table of isochrones parameters
trk/*/* . 648 Stellar tracks from pre-main sequence, M=0.3 to 1.1
hb/*/* . 648 Stellar tracks from ZAHB to thermal pulses,
M=0.55 to 1.1
hb/*/grid/* . 648 Stellar tracks from ZAHB to thermal pulses/grid,
M=0.55 to 1.1
iso/*/* . 648 Isochrone tables, age=8.0 to 15.0Gyr
zahb/* . 648 ZAHB models
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See also:
J/A+A/533/A109 : Pisa pre-main sequence tracks and isochrones (Tognelli+, 2011)
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:
TRKZz.zzzzzHey.yyyyMLa.aaAS09mm
where:
Zz.zzzzz is the metallicity, 19 values from 0.0001 to 0.01000
Hey.yyyy is the Helium abundance, six different values for each Z
MLa.aa is the mixing length parameter, three values: 1.7, 1.8, 1.9
AS09mm indicates the Solar mixture from Asplund et al. (2009) and the
alfa-enhancement a0=[alpha/Fe]=0.0, a3=[alpha/Fe]=0.3
Inside each dataset, names of the stellar tracks are in the form:
OUTMm.mmZz.zzzzzHey.yyyyMLa.aaAS09mm.DAT
where:
Mm.mm is the initial mass in solar units, from 0.30 to 1.10.
Description of file: hb/*/* hb/*/grid/*
Stellar tracks from ZAHB of different initial masses and same physical
parameters (i.e. a "dataset") are grouped in subdirectories under hb/
The subdirectory names of the datasets are in the form:
TRKZz.zzzzzHey.yyyyMLa.aaAS09mm_HB
where:
Zz.zzzzz is the metallicity, 19 values from 0.0001 to 0.01000
Hey.yyyy is the Helium abundance, six different values for each Z
MLa.aa is the mixing length parameter, three values: 1.7, 1.8, 1.9
AS09mm indicates the Solar mixture from Asplund et al. (2009) and the
alfa-enhancement a0=[alpha/Fe]=0.0, a3=[alpha/Fe]=0.3
Inside each dataset, names of the stellar tracks are in the form:
OUTMm.mmZz.zzzzzHey.yyyyMLa.aaAS09mm_ZAHBv.vvvv.DAT
where:
Mm.mm is the initial mass in solar units, from 0.30 to 1.10
ZAHBv.vvvv is the ZAHB mass of the star
Description of file: zahb/*
Stellar ZAHB for different initial masses
The file names are in the form:
ZAHBZz.zzzzzHey.yyyyMLa.aaAS09mm.DAT
where:
Zz.zzzzz is the metallicity, 19 values from 0.0001 to 0.01000
Hey.yyyy is the Helium abundance, six different values for each Z
MLa.aa is the mixing length parameter, three values: 1.7, 1.8, 1.9
AS09mm indicates the Solar mixture from Asplund et al. (2009) and the
alfa-enhancement a0=[alpha/Fe]=0.0, a3=[alpha/Fe]=0.3
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:
ISOZz.zzzzzHey.yyyyMLa.aaAS09mm
where:
Zz.zzzzz is the metallicity, 19 values from 0.00010 to 0.01000
Yy.yyy is the Helium abundance, six different values for each Z
MLa.aa is the mixing length parameter, three values: 1.7, 1.8, 1.9
AS09mm indicates the Asplund et al. 2009 Solar mixture and the
alfa-enhancement a0=[alpha/Fe]=0.0, a3=[alpha/Fe]=0.3
Inside each dataset, names of the isochrone tables are in the form:
AGEaaaaaZz.zzzzzHey.yyyyMLa.aaAS09mm.DAT
where:
AGEaaaaa is the isochrone age in Myr, from 8000 to 15000.
--------------------------------------------------------------------------------
Byte-by-byte Description of file (#): datasets.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 31 A31 --- dataset Dataset name
33- 39 F7.5 --- Z Metallicity
41- 46 F6.4 --- Y Helium abundance
48- 51 F4.2 --- ML Mixing length parameter
53- 54 A2 --- AS09 [a0,a3] Solar mixture from Asplund et al.
(2009) and the alfa-enhancement
a0=[alpha/Fe]=0.0, a3=[alpha/Fe]=0.3
--------------------------------------------------------------------------------
Byte-by-byte Description of file (#): hbgrid.dat hb.dat trk.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 F4.2 Msun M Stellar initial mass, in solar units
6- 12 F7.5 --- Z Metallicity
14- 19 F6.4 --- Y Helium abundance
21- 24 F4.2 --- ML Mixing length parameter
26- 27 A2 --- AS09 [a0,a3] Solar mixture from Asplund et al.
(2009) and the alfa-enhancement
a0=[alpha/Fe]=0.0, a3=[alpha/Fe]=0.3
29- 74 A46 --- dir Directory
76-132 A57 --- file Filename
--------------------------------------------------------------------------------
Byte-by-byte Description of file (#): zahb.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 F7.5 --- Z Metallicity
9- 14 F6.4 --- Y Helium abundance
16- 19 F4.2 --- ML Mixing length parameter
21- 22 A2 --- AS09 [a0,a3] Solar mixture from Asplund et al.
(2009) and the alfa-enhancement
a0=[alpha/Fe]=0.0, a3=[alpha/Fe]=0.3
24- 27 A4 --- dir Directory
29- 85 A57 --- file Filename
--------------------------------------------------------------------------------
Byte-by-byte Description of file (#): iso.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 I5 Myr Age Isochrone age
7- 13 F7.5 --- Z Metallicity
15- 20 F6.4 --- Y Helium abundance
22- 25 F4.2 --- ML Mixing length parameter
27- 28 A2 --- AS09 [a0,a3] Solar mixture from Asplund et al.
(2009) and the alfa-enhancement
a0=[alpha/Fe]=0.0, a3=[alpha/Fe]=0.3
30- 68 A39 --- dir Directory
70-113 A44 --- file Filename
--------------------------------------------------------------------------------
Byte-by-byte Description of file (#): trk/*/* hb/*/* hb/*/grid/*
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 3 I3 --- MOD Model number
6- 18 F13.10 [yr] logAge Age of the model: log(Age/yr)
20- 28 F9.6 [Lsun] logL Total luminosity: log(L/Lsun)
30- 38 F9.6 [K] logTe Effective temperature: log(Te/K)
41- 50 E10.4 Msun M Mass of the star
53- 62 E10.4 --- Hc Central Hydrogen (Helium) abundance
65- 74 E10.4 [K] logTc Central Temperature: log(Tc/K)
77- 86 E10.4 [g/cm3] logrhoC Central Density: log(rhoC/(g/cm^3))
89- 98 E10.4 Msun MHeC He core mass
101-110 E10.4 --- LPP Luminosity of PP chain
(in units of the total luminosity L)
113-122 E10.4 --- LCNO Luminosity of CNO cycle
(in units of the total luminosity L)
125-134 E10.4 --- L3a Luminosity of triple alpha
(in units of the total luminosity L)
137-146 E10.4 --- Lg Gravitational luminosity
(in units of the total luminosity L)
149-158 E10.4 Rsun R Radius of the star
161-170 E10.4 [cm/s2] logG Logarithm of surface gravity
--------------------------------------------------------------------------------
Byte-by-byte Description of file (#): iso/*/*
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
2- 12 F11.8 [Lsun] logL Total luminosity: log(L/Lsun)
16- 25 F10.8 [K] logTe Effective temperature: log(Te/K)
28- 38 F11.8 Msun M Stellar mass: M/Msun
41- 52 E12.6 Rsun R Radius of the star: R/Rsun
55- 65 F11.8 [cm/s2] logg Logarithm of surface gravity
--------------------------------------------------------------------------------
Byte-by-byte Description of file (#): zahb/*
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 6 F6.4 Msun M Stellar mass: M/Msun
8- 15 F8.6 [K] logT Temperature: log(T/K)
17- 23 F7.5 [Lsun] logL Luminosity: log(L/Lsun)
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Acknowledgements:
Giada Valle, valle(at)df.unipi.it
(End) Giada Valle [Pisa], Patricia Vannier [CDS] 10-Mar-2012