In this database can be found stellar evolutionary tracks, their ejecta and the production rates of ionizing photons. All details on the physical assumptions, and on the evolutionary properties of the tracks can be find in Costa, Shepherd et al. 2025.
The files are divided in three data groups which contains:
In the following, we describe the content of each file type.
The grids of stellar tracks contains models computed with a mass that ranges from 2 M to 2000 M, in the metallicity range between Z=1E-11 and Z=0.0001, and from 2 M to 600 M, in the metallicity range between Z=0.001 and Z=0.03. The total dataset contains more than ~1100 tracks. All stellar tracks have been computed with PARSEC v2.0, details can be find in the paper cited above.
The tables for each stellar track contains the quantities listed in the following table
Column number | Quantity | Description |
---|---|---|
1 | MASS | Current total mass [M] |
2 | AGE | Age [yr] |
3 | Dtime | Time-step of the previous model [yr] |
4 | LOG_L | log10 total luminosity [log10 L] |
5 | LOG_TE | Effective temperature [log10 K] |
6 | RSTAR | Star radius [cm] |
7 | CONV | Mass of the convective core (incl. overshooting) [M/Mtot] |
8 | QSCHW | Mass of the unstable core (Schwartzschild criterion, w/o overshooting) [M/Mtot] |
9 | QHEL | Mass of the He-core, i.e. where X < 10-3 [M/Mtot] |
10 | QCAROX | Mass of the Carbon Oxygen (CO) core, i.e. where Y = 10-3 [M/Mtot] |
11 | LOG_Tc | log10 central temperature [log10 K] |
12 | LOG_RHc | log10 central density [log10 g cm-3] |
13 | LOG_Pc | log10 central pressure [log10 10-1 Pa] |
14 | PSI_C | Degeneracy parameter in the center |
15 | G1_AVG | Averaged 1 adiabatic index (through the whole star) |
16 | XCEN | Central H1 mass fraction |
17 | XHE3C | Central He3 mass fraction |
18 | YCEN | Central He4 mass fraction |
19 | XC_CEN | Central C12 mass fraction |
20 | XN_CEN | Central N14 mass fraction |
21 | XO_CEN | Central O16 mass fraction |
22 | XNE_CEN | Central Ne20+Ne22 mass fraction |
23 | XMG_CEN | Central Mg24+Mg25+Mg26 mass fraction |
24 | XSI28_CEN | Central Si28 mass fraction |
25 | XS32_CEN | Central S32 mass fraction |
26 | XAR36_CEN | Central Ar36 mass fraction |
27 | XCA40_CEN | Central Ca40 mass fraction |
28 | XTI44_CEN | Central Ti44 mass fraction |
29 | RATE | Mass loss or accretion rate [M yr-1] |
30 | Xsup | Surface H1 mass fraction |
31 | Ysup | Surface He4 mass fraction |
32 | XCsup | Surface C12 mass fraction |
33 | XC13sup | Surface C13 mass fraction |
34 | XNsup | Surface N14 mass fraction |
35 | XOsup | Surface O16 mass fraction |
36 | XO18sup | Surface O18 mass fraction |
37 | XNEsup | Surface Ne20 + Ne22 mass fraction |
38 | XMGsup | Surface Mg24 + Mg25 + Mg26 mass fraction |
39 | POLRAD_ENV | Star polar radius [cm] |
40 | EQRAD_ENV | Star equatorial radius [cm] |
41 | OMG_ENV | Angular rotation rate = angular velocity / angular critical velocity |
42 | ANG_VEL_ENV | envelope angular velocity [cm s-1] |
43 | TANVEL_ENV | tangential linear velocity at the equator[cm s-1] |
44 | TOT_INERTIA | Total moment of inertia of the star [g cm2] |
45 | TOT_ANGMOM | Total angular momentum [g cm2 s-1] |
46 | TOT_MOM_LOST | Total angular momentum lost due to stellar wind [g cm2 s-1] |
47 | R_CONV | Radius at CONV [log10 cm] |
48 | RHEL | Radius at QHEL [log10 cm] |
49 | R_CAROX | Radius at QCAROX [log10 cm] |
50 | INERTIA_HEL | He-core inertia [g cm2] |
51 | ANGMOM_HEL | He-core angular momentum [g cm2 s-1] |
52 | INERTIA_CAROX | CO-core inertia [g cm2] |
53 | ANGMOM_CAROX | CO-core angular momentum [g cm2 s-1] |
54 | TMAX | Maximum temperature [log10 K] |
55 | RHTMAX | Density where T = TMAX [log10 g cm-3] |
56 | QTMAX | Mass coordinate where T = TMAX [M/Mtot] |
57 | LNUC | Luminosity produced by nuclear burning [L/Ltot] |
58 | LX | Luminosity by hydrogen burning [L/Ltot] |
59 | LY | Luminosity by helium burning [L/Ltot] |
60 | LC | Luminosity by carbon burning [L/Ltot] |
61 | LNEUTR | Neutrinos luminosity [L/Ltot] |
62 | L_GRAV | Gravitational luminosity [L/Ltot] |
63 | L_ACC | Accretion luminosity [L/Ltot] |
64 | Q_CNV | Mass coordinate depth of convective envelope [M/Mtot] |
65 | DPTH_CNV | Radial depth of convective envelope [log10 cm] |
66 | INERTIA_CNV | Inertia of the convective envelope [g cm2] |
67 | ANGMOM_CNV | Angular momentum of the convective envelope [g cm2 s-1] |
68 | TCNV_YR | Turnover timescale of convective bubble [yr] |
69 | T20L10 | Atmosphere temperature of the gas at = 20 [log10 K] |
70 | RH20L10 | Atmosphere density of the gas at = 20 [log10 g cm-3] |
71 | P20L10 | Atmosphere pressure of the gas at = 20 [log10 10-1 Pa] |
72 | TE20L10 | Effective temperature at = 20 [log10 K] |
73 | R20L10 | Atmosphere radius at = 20 [log10 cm] |
74 | MU20 | Atmosphere molecular weight at = 20 [log10 cm] |
75 | T2_3L10 | Atmosphere temperature of the gas at = 2/3 [log10 K] |
76 | RH2_3L10 | Atmosphere density of the gas at = 2/3 [log10 g cm-3] |
77 | P2_3L10 | Atmosphere pressure of the gas at = 2/3 [log10 10-1 Pa] |
78 | TE2_3L10 | temperature from Stefan-Boltzmann law at = 2/3 [log10 K] |
79 | R2_3L10 | Atmosphere radius at = 2/3 [log10 cm] |
80 | MU2_3 | Atmosphere molecular weight at = 2/3 [log10 cm] |
Chemical ejecta are computed for all track from 14 M and above, by integrating throughout the whole evolution of the star, and taking into account for the different final fates. Stellar ejecta are given in two tables:
*_winds_ejecta.dat
), which contains the sum of each ejected elements in solar masses along the evolution, without the explosions.*_total_ejecta.dat
), which include winds and the elements ejected in the final explosion (if any).In the header of each file it is indicated the initial composition. The quantities contained in each total ejecta file are listed below:
Column number | Quantity | Description |
---|---|---|
1 | Min | Initial mass at the Zero-Age Main-Sequence [M] |
2 | Mfin | Final mass at the pre-SN stage (end of PARSEC computation) [M] |
3 | M_HE | Final He-core mass at the pre-SN stage [M] |
4 | M_CO | Final CO-core mass at the pre-SN stage [M] |
5 | Mrem | Remnant mass [M] |
6 | Mbar | Barionic mass content before neutrinos escape [M] |
7 | NI56 | Nickel ejected [M] |
8 | SNT | Supernova type. Core Collapse SuperNova (CCSN), Failed SN (FSN), Pulsational Pair-Instability SN (PPISN), Pair-Instability SN (PISN), Direct Black Hole collapse (DBH) |
9 | H | Hydrogen mass ejected [M] |
10 | HE3 | Helium-3 mass ejected [M] |
11 | HE4 | Helium mass ejected [M] |
12 | LI7 | Lithium mass ejected [M] |
13 | BE7 | Berylium mass ejected [M] |
14 | C12 | Carbon mass ejected [M] |
15 | C13 | Carbon-13 mass ejected [M] |
16 | N14 | Nitrogen mass ejected [M] |
17 | N15 | Nitrogen-15 mass ejected [M] |
18 | O16 | Oxygen mass ejected [M] |
19 | O17 | Oxygen-17 mass ejected [M] |
20 | O18 | Oxygen-18 mass ejected [M] |
21 | F19 | Fluorine mass ejected [M] |
22 | NE20 | Neon mass ejected [M] |
23 | NE21 | Neon-21 mass ejected [M] |
24 | NE22 | Neon-22 mass ejected [M] |
25 | NA23 | Sodium mass ejected [M] |
26 | MG24 | Magnesium mass ejected [M] |
27 | MG25 | Magnesium-25 mass ejected [M] |
28 | MG26 | Magnesium-26 mass ejected [M] |
29 | AL26 | Aluminium-26 mass ejected [M] |
30 | AL27 | Aluminium mass ejected [M] |
31 | SI28 | Silicon mass ejected [M] |
32 | SI29 | Silicon-29 mass ejected [M] |
33 | P | Phosphorus mass ejected [M] |
34 | S | Sulfur mass ejected [M] |
35 | CL | Chlorine mass ejected [M] |
36 | AR | Argon mass ejected [M] |
37 | K | Potassium mass ejected [M] |
38 | CA | Calcium mass ejected [M] |
39 | SC | Scandium mass ejected [M] |
40 | TI | Titanium mass ejected [M] |
41 | V | Vanadium mass ejected [M] |
42 | CR | Chromium mass ejected [M] |
43 | MN | Manganese mass ejected [M] |
44 | FE | Iron mass ejected [M] |
45 | CO | Cobalt mass ejected [M] |
46 | NI | Nickel mass ejected [M] |
47 | CU | Copper mass ejected [M] |
48 | ZN | Zinc mass ejected [M] |
The quantities in the winds ejecta files are a subset of those presented above.
The ionizing photons tables contains the number of photons per second emitted from the stars' surface during the evolution. The production rate is computed for photons with energies high enough to ionize H, He, He+, O+, and the UV Lyman-Werner band (able to dissociate the H2 molecule). Each table include the following quantities:
Column number | Quantity | Description |
---|---|---|
1 | Myr | Age [Myr] |
2 | MASS | Current mass of the star [M] |
3 | LG_L | log10 total luminosity [log10 L] |
4 | LG_TE | Effective temperature [log10 K] |
5 | LG_R_cm | Star radius [log10 cm] |
6 | LG_Q_H_sec | HI ionizing photons rate [log10 #phot s-1] |
7 | LG_Q_HEI_sec | HEI ionizing photons rate [log10 #phot s-1] |
8 | LG_Q_HEII_sec | HEII ionizing photons rate [log10 #phot s-1] |
9 | LG_Q_OII_sec | OII ionizing photons rate [log10 #phot s-1] |
10 | LG_QWERNER_sec | Lyman-Werner ionizing photons rate [log10 #phot s-1] |