Revisiting the pre-main-sequence evolution of stars - II. Consequences of planet formation on stellar surface composition

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Table C.1.

Stellar evolutionary models.

Settings				Results
ξ	X_D [ppm]	m^a_ke	M_final [M_⊙]	Age [yr]	M_⋆ [M_⊙]	M_CZ [M_⊙]	^b [M_⊙]	R_⋆ [R_⊙]	L_⋆ [L_⊙]	T_eff [K]
0.1	28	-1.0	1.0	0.0E+00	1.00000E-02	1.00000E-02	-1.00000E+00	1.51399E+00	5.44190E-02	2.21056E+03
0.1	28	-1.0	1.0	1.0E+03	1.99973E-02	4.35589E-03	-1.00000E+00	1.13449E+00	3.29172E-02	2.30986E+03
⋮
Continued

Notes. Accretion history described in Sect. 3.2 with Z_acc = Z_ini is assumed. A complete table is available at CDS.

^(a)

Although m_ke is defined from 0 to 1, here for simplicity m_ke = −1 indicates a uniform heat distribution (Sect. 3.1).

^(b)

is available only between 0.3 and 10 Myr and is set to −1 if not available. The full table is available at the CDS.

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