A comparison of evolutionary tracks for single Galactic massive stars

F. Martins; A. Palacios

doi:10.1051/0004-6361/201322480

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Volume 560 (December 2013)

A&A, 560 (2013) A16

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Table 2

Properties of the 20 M_⊙ model computed with different codes, without rotation, and evaluated at four different evolutionary phases.

Phase	STERN²	Geneva	FRANEC	Padova	MESA	STAREVOL

X_c = 0.5

T_eff(K)	33 522	33 758	33 709	32 538	33 011	33 365
	4.764	4.733	4.736	4.747	4.745	4.733
age (Myr)	3.598	3.745	4.079	4.279	4.073	3.963


TAMS³

T_eff(K)	24 630	29 297	28 094	25 972	28 733	27 902
	5.096	5.001	5.036	5.045	5.007	4.995
age (Myr)	8.173	7.819	9.085	9.100	8.598	8.535


ZAHeMS

T_eff(K)	5388	24 014	27 382	15 657	23 200	24 259
	4.987	5.025	5.012	5.044	5.042	5.015
age (Myr)	8.185	7.828	9.088	9.111	8.610	8.541


TAHeMS³

T_eff(K)	−	3753	3817	3550	3702	3462
	−	5.050	5.206	5.090	5.049	5.027
age (Myr)	−	8.713	9.690	9.820	9.530	9.748

Notes. When the central H mass fraction is 0.5 (X_c = 0.5); at the terminal age main sequence (TAMS); at the zero age helium burning main sequence (ZAHeMS); at the terminal age helium burning main sequence (TAHeMS).

⁽²⁾

For the STERN grid, the data available stop at the beginning of the core He burning phase.

⁽³⁾

The TAMS and TAHeMS are defined as the points where the mass fraction of H (resp. He) is lower than 10^-5.

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