# File formats

You'll find below a description of the columns in:

### Meaning of the columns in the evolution files

Column | Variable | Units | Description |

1: | line number | ||

2: | age | [yr] | |

3: | M | [M_{⊙}] | mass |

4: | log (L/L_{⊙}) | luminosity | |

5: | log (T_{eff}) | [K] | effective temperature |

6: | ^{1}H | [mass fraction] | surface abundances |

7: | ^{4}He | " | " |

8: | ^{12}C | " | " |

9: | ^{13}C | " | " |

10: | ^{14}N | " | " |

11: | ^{16}O | " | " |

12: | ^{17}O | " | " |

13: | ^{18}O | " | " |

14: | ^{20}Ne | " | " |

15: | ^{22}Ne | " | " |

16: | ^{26}Al | " | " |

17: | M_{cc} | [M / M_{tot}] | convective core mass |

18: | log (T_{eff}) | [K] | not corrected for the wind thickness (WR) |

19: | log (Ṁ) | [M_{⊙} / yr] | mass loss |

20: | log (ρ_{c}) | [g cm^{-3}] | central density |

21: | log (T_{c}) | [K] | central temperature |

22: | ^{1}H | [mass fraction] | central abundances |

23: | ^{4}He | " | " |

24: | ^{12}C | " | " |

25: | ^{13}C | " | " |

26: | ^{14}N | " | " |

27: | ^{16}O | " | " |

28: | ^{17}O | " | " |

29: | ^{18}O | " | " |

30: | ^{20}Ne | " | " |

31: | ^{22}Ne | " | " |

32: | ^{26}Al | " | " |

33: | Ω_{surf} | [s^{-1}] | angular velocity at the surface |

34: | Ω_{centre} | [s^{-1}] | angular velocity at the centre |

35: | R_{pol}/R_{eq} | oblateness | |

36: | F_{Ω} | correction factor to Ṁ due to rotation | |

37: | V_{crit,1} | [km s^{-1}] | critical velocity (Ω-limit) |

38: | V_{crit,2} | [km s^{-1}] | critical velocity (ΩΓ-limit) |

39: | V_{eq} | [km s^{-1}] | equatorial velocity |

40: | Ω/Ω_{crit} | fraction of critical rotation | |

41: | Γ_{Edd} | Eddington factor | |

42: | log (Ṁ_{mech}) | [M_{⊙} / yr] | mechanical mass loss at the equator |

43: | ℒ _{tot} | [10^{53} g cm^{2} s^{-1}] | total angular momentum |

44: | log(g_{pol}) | [cm s^{-2}] | polar surface gravity |

45: | R_{pol} | [R_{⊙}] | polar radius |

46: | M_{bol} | [mag] | bolometric magnitude |

47: | M_{V} | [mag] | V-band magnitude |

48: | U-B | colours index | |

49: | B-V | " | |

50: | V-R | " | |

51: | V-I | " | |

52: | J-K | " | |

53: | H-K | " | |

54: | V-K | " | |

55: | BC | Bolometric correction |

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### Meaning of the columns in the isochrone files

Column | Variable | Units | Description |

1: | M_{ini} | [M_{⊙}] | initial mass of the (interpolated) model |

2: | Z_{ini} | initial metallicity | |

3: | V/V_{crit} | initial rotation rate | |

4: | M | [M_{⊙}] | mass at the given age |

5: | log (L/L_{⊙}) | luminosity | |

6: | log (T_{eff}) | [K] | effective temperature |

7: | log (T_{eff}) | [K] | " (not corrected for the wind thickness) |

8: | M_{bol} | [mag] | bolometric magnitude |

9: | M_{V} | [mag] | V-band magnitude |

10: | U-B | colour index | |

11: | B-V | " | |

12: | V-R | " | |

13: | V-I | " | |

14: | H-K | " | |

15: | J-K | " | |

16: | V-K | " | |

17: | BC | bolometric correction | |

18: | R_{pol} | [R_{⊙}] | polar radius |

19: | R_{pol}/R_{eq} | oblateness | |

20: | log (g_{pol}) | [cm s^{-2}] | polar gravity |

21: | Ω_{surf} | [s^{-1}] | angular velocity at the surface |

22: | V_{eq} | [km s^{-1}] | equatorial velocity |

23: | V_{crit,1} | [km s^{-1}] | critical velocity (Ω-limit) |

24: | V_{crit,2} | [km s^{-1}] | critical velocity (ΩΓ-limit) |

25: | Ω/Ω_{crit} | fraction of critical rotation | |

26: | log (Ṁ) | [M_{⊙} / yr] | mass-loss rate |

27: | log (Ṁ_{mech}) | [M_{⊙} / yr] | mechanical mass-loss rate at the equator |

28: | Γ_{Edd} | Eddington factor | |

29: | ^{1}H | [mass fraction] | surface abundances |

30: | ^{4}He | " | " |

31: | ^{12}C | " | " |

32: | ^{13}C | " | " |

33: | ^{14}N | " | " |

34: | ^{16}O | " | " |

35: | ^{17}O | " | " |

36: | ^{18}O | " | " |

37: | ^{20}Ne | " | " |

38: | ^{22}Ne | " | " |

39: | ^{26}Al | " | " |

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### Meaning of the columns in the cluster files

Column | Variable | Units | Description |

1: | M_{ini} | [M_{⊙}] | initial mass of the star |

2: | Z_{ini} | [Z_{⊙}] | initial metallicity of the star |

3: | Ω_{ini}/Ω_{crit} | initial fraction of critical rotation | |

4: | i | [°] | viewing angle |

5: | binarity | 0: single, 1: binary, | |

2: binary, but secondary not interpolated ^{★} | |||

6: | M_{1}/M_{2} | mass ratio if binary | |

7: | M | [M_{⊙}] | mass at age t |

8: | log (L/L_{⊙}) | luminosity | |

9: | log (T_{eff}) | [K] | effective temperature |

10: | log (T_{eff}) | [K] | " (not corrected for the wind thickness) |

11: | log (L/L_{⊙})_{gd} | L corrected for gravity darkening | |

12: | log (T_{eff})_{gd} | [K] | T_{eff} corrected for gravity darkening |

13: | log (L/L_{⊙})_{lgd} | L corrected for gravity+limb darkening | |

14: | log (T_{eff})_{lgd} | [K] | T_{eff} corrected for gravity+limb darkening |

15: | M_{bol} | [mag] | bolometric magnitude |

16: | M_{V} | [mag] | V-band magnitude |

17: | U-B | colour index | |

18: | B-V | " | |

19: | V-R | " | |

20: | V-I | " | |

21: | J-K | " | |

22: | H-K | " | |

23: | V-K | " | |

24: | B_{2}-V_{1} | " | |

25: | M_{V,noise} | [mag] | M_{V} with noise |

26: | B-V_{noise} | B-V with noise | |

27: | R_{pol} | [R_{⊙}] | polar radius |

28: | R_{pol}/R_{eq} | oblateness | |

29: | log (g_{pol}) | [cm s^{-2}] | polar gravity |

30: | Ω_{surf} | [s^{-1}] | surface angular velocity at age t |

31: | V_{eq} | [km s^{-1}] | equatorial velocity |

32: | V_{crit,1} | [km s^{-1}] | critical velocity (Ω-limit) |

33: | V_{crit,2} | [km s^{-1}] | critical velocity (ΩΓ-limit) |

34: | Ω/Ω_{crit} | fraction of critical rotation | |

35: | log (Ṁ) | [M_{⊙} / yr] | mass-loss rate |

36: | log (Ṁ_{mech}) | [M_{⊙} / yr] | mechanical mass-loss rate at the equator |

37: | Γ_{Edd} | Eddington factor | |

38: | ^{1}H | [mass fraction] | surface abundances |

39: | ^{4}He | " | " |

40: | ^{12}C | " | " |

41: | ^{13}C | " | " |

42: | ^{14}N | " | " |

43: | ^{16}O | " | " |

44: | ^{17}O | " | " |

45: | ^{18}O | " | " |

46: | ^{20}Ne | " | " |

47: | ^{22}Ne | " | " |

48: | ^{26}Al | " | " |

^{★} In case the secondary is below the minimum mass for the grids used,
only the flux of the primary is considered, but the binary nature and the mass ratio are still computed.

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