PARSEC V2.0 - Intermediate to Very massive stellar tracks

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:

Stellar tracks;
Ejecta;
Ionizing photons emission rates.

In the following, we describe the content of each file type.

Stellar evolutionary tracks

The grids of stellar tracks contains models computed with a mass that ranges from 2 M_$\odot$ to 2000 M_$\odot$, in the metallicity range between Z=1E-11 and Z=0.0001, and from 2 M_$\odot$ to 600 M_$\odot$, 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_$\odot$]
2	AGE	Age [yr]
3	Dtime	Time-step of the previous model [yr]
4	LOG_L	log₁₀ total luminosity [log₁₀ L_$\odot$]
5	LOG_TE	Effective temperature [log₁₀ K]
6	RSTAR	Star radius [cm]
7	CONV	Mass of the convective core (incl. overshooting) [M/M_tot]
8	QSCHW	Mass of the unstable core (Schwartzschild criterion, w/o overshooting) [M/M_tot]
9	QHEL	Mass of the He-core, i.e. where X < 10^-3 [M/M_tot]
10	QCAROX	Mass of the Carbon Oxygen (CO) core, i.e. where Y = 10^-3 [M/M_tot]
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 $\Gamma$ 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_$\odot$ 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/M_tot]
57	LNUC	Luminosity produced by nuclear burning [L/L_tot]
58	LX	Luminosity by hydrogen burning [L/L_tot]
59	LY	Luminosity by helium burning [L/L_tot]
60	LC	Luminosity by carbon burning [L/L_tot]
61	LNEUTR	Neutrinos luminosity [L/L_tot]
62	L_GRAV	Gravitational luminosity [L/L_tot]
63	L_ACC	Accretion luminosity [L/L_tot]
64	Q_CNV	Mass coordinate depth of convective envelope [M/M_tot]
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 $\tau$ = 20 [log₁₀ K]
70	RH20L10	Atmosphere density of the gas at $\tau$ = 20 [log₁₀ g cm^-3]
71	P20L10	Atmosphere pressure of the gas at $\tau$ = 20 [log₁₀ 10^-1 Pa]
72	TE20L10	Effective temperature at $\tau$ = 20 [log₁₀ K]
73	R20L10	Atmosphere radius at $\tau$ = 20 [log₁₀ cm]
74	MU20	Atmosphere molecular weight at $\tau$ = 20 [log₁₀ cm]
75	T2_3L10	Atmosphere temperature of the gas at $\tau$ = 2/3 [log₁₀ K]
76	RH2_3L10	Atmosphere density of the gas at $\tau$ = 2/3 [log₁₀ g cm^-3]
77	P2_3L10	Atmosphere pressure of the gas at $\tau$ = 2/3 [log₁₀ 10^-1 Pa]
78	TE2_3L10	temperature from Stefan-Boltzmann law at $\tau$ = 2/3 [log₁₀ K]
79	R2_3L10	Atmosphere radius at $\tau$ = 2/3 [log₁₀ cm]
80	MU2_3	Atmosphere molecular weight at $\tau$ = 2/3 [log₁₀ cm]

Stellar ejecta tables

Chemical ejecta are computed for all track from 14 M_$\odot$ 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:

Stellar winds ejecta (*_winds_ejecta.dat), which contains the sum of each ejected elements in solar masses along the evolution, without the explosions.
Total ejecta (*_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_$\odot$]
2	Mfin	Final mass at the pre-SN stage (end of PARSEC computation) [M_$\odot$]
3	M_HE	Final He-core mass at the pre-SN stage [M_$\odot$]
4	M_CO	Final CO-core mass at the pre-SN stage [M_$\odot$]
5	Mrem	Remnant mass [M_$\odot$]
6	Mbar	Barionic mass content before neutrinos escape [M_$\odot$]
7	SNT	Supernova type. Core Collapse SuperNova (CCSN), Failed SN (FSN), Pulsational Pair-Instability SN (PPISN), Pair-Instability SN (PISN), Direct Black Hole collapse (DBH)
8	H	Hydrogen mass ejected [M_$\odot$]
9	HE3	Helium-3 mass ejected [M_$\odot$]
10	HE4	Helium mass ejected [M_$\odot$]
11	LI7	Lithium mass ejected [M_$\odot$]
12	BE7	Berylium mass ejected [M_$\odot$]
13	C12	Carbon mass ejected [M_$\odot$]
14	C13	Carbon-13 mass ejected [M_$\odot$]
15	N14	Nitrogen mass ejected [M_$\odot$]
16	N15	Nitrogen-15 mass ejected [M_$\odot$]
17	O16	Oxygen mass ejected [M_$\odot$]
18	O17	Oxygen-17 mass ejected [M_$\odot$]
19	O18	Oxygen-18 mass ejected [M_$\odot$]
20	F19	Fluorine mass ejected [M_$\odot$]
21	NE20	Neon mass ejected [M_$\odot$]
22	NE21	Neon-21 mass ejected [M_$\odot$]
23	NE22	Neon-22 mass ejected [M_$\odot$]
24	NA23	Sodium mass ejected [M_$\odot$]
25	MG24	Magnesium mass ejected [M_$\odot$]
26	MG25	Magnesium-25 mass ejected [M_$\odot$]
27	MG26	Magnesium-26 mass ejected [M_$\odot$]
28	AL26	Aluminium-26 mass ejected [M_$\odot$]
29	AL27	Aluminium mass ejected [M_$\odot$]
30	SI28	Silicon mass ejected [M_$\odot$]
31	SI29	Silicon-29 mass ejected [M_$\odot$]
32	P	Phosphorus mass ejected [M_$\odot$]
33	S	Sulfur mass ejected [M_$\odot$]
34	CL	Chlorine mass ejected [M_$\odot$]
35	AR	Argon mass ejected [M_$\odot$]
36	K	Potassium mass ejected [M_$\odot$]
37	CA	Calcium mass ejected [M_$\odot$]
38	SC	Scandium mass ejected [M_$\odot$]
39	TI	Titanium mass ejected [M_$\odot$]
40	V	Vanadium mass ejected [M_$\odot$]
41	CR	Chromium mass ejected [M_$\odot$]
42	MN	Manganese mass ejected [M_$\odot$]
43	FE	Iron mass ejected [M_$\odot$]
44	CO	Cobalt mass ejected [M_$\odot$]
45	NI	Nickel mass ejected [M_$\odot$]
46	CU	Copper mass ejected [M_$\odot$]
47	ZN	Zinc mass ejected [M_$\odot$]

The quantities in the winds ejecta files are a subset of those presented above.

Ionizing photons tables

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). All photon rates given below are computed integrating from the wavelength $\lambda_i$ to infinite. The photon rate in the Lyman-Werner band (QLW) can be easily retrieved as follows: QLW = QWERNER - Q_H.

Each table include the following quantities:

Column number	Quantity	Description
1	Myr	Age [Myr]
2	MASS	Current mass of the star [M_$\odot$]
3	LG_L	log₁₀ total luminosity [log₁₀ L_$\odot$]
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	Werner ionizing photons rate [log₁₀ #phot s^-1]