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The distribution of the HI surface mass density is reasonably well determined from 21 cm line observations, the main uncertainty residing in the optical depth 42 • • 3 -a • c • .... •• . • " • • • '"1"• • " '" """ ': • iI'~ ' c" " a . ' ~_ ••••• x iii "i D ~" • 2 ~ • • •• •• • • • •• o a "C " >II o •_• • '-_ •••" .. "".... ' I • • • • I • • • • Figure 1. 20. A(Li) vs. [Fe/HJ as traced by stars in t he solar neighbourhood, A(Li) ;:::0 log (N( Li )/ H ) + 12, where N( Li ) is t he abundance by number.
5. Vol. 265 , 271 ; reproduced by kind permission of Kluwer Academic Publishers (copy right 1999). 18). nd recent studies. 3. Element Summary of abundance gradients along the galactic disk. Study Gradient (dex Oxygen Sulphur Nroo Iron Helium Carbon Magnesium Silicon Kilian-Montenbr uck et aI. Maciel & Koppen 1994 VOchez & Esteban 1996 Afflerbach et aI. 1997 Smartt & Rollcston 1997 Gummersbach et aI. 1998 Maciel & Quireza 1999 Shaver et al. 1983 Kaufer et aI. 1994 Kilian-Montenbruck et al. Simpson ct al.
10- 10 5,6, 11 6, 7, 12,13 8,9,6 10,6 6,10 6,10 6,10 3H el H 4Hel H 'rLiI H 6Lil H 9Bel H 10 BIH llBI H 1. Buries and Tytler (1998); 2. Webb et al. (1997); 3. Lins kyet aI. (1993;1995) ; Scully et aI. (1996); 5. Gloecklcr and Geiss (1996); 6. Grevesse and Noels (1993); 7. Isotov et aI. (1999) ; 8. Bonifacio and Molaro (1997); 9. Duncan and Rebull (1996); 10. Thomas et aI. (1993); II. Olive and Fields (1999); 12. Olive et aI. (1997) ; 13. Chiappini et aI . (1997). The light elements D, 3 H e, 4 H eand 1 Li are thought to be produced during the Big Bang and also during the galactic evolution , wit h the exception of D which is only destroyed inside stars.
