Effects of thermohaline instability and rotation-induced mixing on the evolution of light elements in the Galaxy: D, 3He and 4He

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Table 1

Abundances of deuterium, ³He, and ⁴He at different epochs.

Chemicals	Units	SBBN+WMAP	Protosolar cloud	Local intestellar medium
		(t = 0 Gyr)	(t = 9.2 Gyr)	(Present time)

D	10⁵ (D/H)	2.49 ± 0.17^a	2.1 ± 0.5^c	2.31 ± 0.24^d
		2.60 ^b		0.98 ± 0.19^e
				2.0 ± 0.1^f
³He	10⁵ (³He/H)	1.00 ± 0.07^a	1.5 ± 0.2^c	2.4 ± 0.7^g
		1.04 ± 0.04^b
⁴He	Y	0.2486 ± 0.0002^a	0.2703^h
		0.2479 ^b

References.

^(a)

Cyburt et al. (2008);

^(b)

Coc et al. (2004);

^(c)

Geiss & Gloeckler (1998);

^(d)

Linsky et al. (2006);

^(e)

Hébrard et al. (2005);

^(f)

Prodanović et al. (2010);

^(g)

Gloeckler & Geiss (1996);

^(h)

Asplund et al. (2009).

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