Effects of the variation of fundamental constants on Population III stellar evolution

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Table 2:

Characteristics of the 15 $M_{\odot }$ models with varying $\delta _{\rm NN}$ at the end of core He burning.
$\delta _{\rm NN}$	$\tau_{\rm MS}$	$\tau_{\rm CHeB}$	$M_{\rm CO}$ ^a	$X({\rm C})$ ^b	C/O^c	Case^d
	[Myr]	[Myr]	[ $M_{\odot }$ ]
-0.009	8.224	1.344	3.84	4.4e-10	-	III
-0.008	8.285	1.276	3.83	2.9e-10	-
-0.007	8.308	1.200	3.38	8.5e-10	-
-0.006	8.401	1.168	3.61	4.2e-07	-
-0.005	8.480	1.130	3.59	5.9e-06	3.0e-05	II
-0.004	8.672	0.933	3.60	3.2e-05	5.2e-05
-0.003	8.790	0.905	3.60	1.3e-04	1.7e-04
-0.002	9.046	0.892	3.61	5.6e-04	6.4e-04
-0.001	9.196	0.888	3.70	0.013	0.014	I
0	9.640	0.802	3.65	0.355	0.550
+0.001	9.937	0.720	3.61	0.695	2.278
+0.002	10.312	0.684	3.62	0.877	7.112
+0.003	10.677	0.664	3.62	0.958	22.57	IV
+0.004	10.981	0.659	3.62	0.981	52.43
+0.005	11.241	0.660	3.61	0.992	123.9
+0.006	11.447	0.661	3.55	0.996	270.2

Notes. ^(a) Mass coordinate where the abundance of ⁴He drops below 10^-3; ^(b) here, $X({\rm C}) = X(^{12}{\rm C})$ , the central value for the carbon mass fraction; ^(c) ratio of the carbon to oxygen mass fractions; ^(d) see text, p. 8 for the description of the different cases.

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