The evolution of runaway stellar collision products

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Table 4:

As Table 3 but for Z=0.001^a.
N	t	$M_{1,N\mbox{-}{\rm body}}$	$M_{1,{\rm mix}}$	M₂	$M_{\rm merger}$
1	0.53120	77.8	77.7	70.7	135.4
2	0.57294	148.5	135.4	82.8	198.3
3	0.65612	231.3	198.1	58.5	239.6
4	0.89154	289.8	239.1	96.6	308.5
5	0.89155	386.4	308.5	78.5	364.2
6	1.02208	464.9	363.5	1.5	364.9
7	1.31086	466.4	363.4	56.3	404.7
8	1.50575	522.6	403.4	48.9	440.2
9	2.05327	571.3	434.9	72.7	487.5
10	2.27966	643.8	390.1	2.0	392.0
11	2.60213	645.0	260.1	3.5	263.3
	2.83153	648.5	171.9^b

^a: Note that the merger sequence was terminated earlier than for Z=0.02 and that the merger remnant did not finish its evolution before the evolution code broke down.
^b: Mass and time at the moment the evolution code broke down, rather than the onset of carbon burning.

Source LaTeX | All tables | In the text

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