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Recommended Elemental Abundances in the Solar Photosphere Derived from Spectroscopy and CI Chondrites

	RECOMMENDED ABUNDANCE			CI CHONDRITES		SPECTROSCOPY
ELEMENT (1)	A(El) (2)	N(El) (3)	SELECTION METHODa (4)	N(El) (5)	A(El) (6)	N(El) (7)	A(El) (8)	DATE AND NOTES FOR SPECTROSCOPIC VALUES (9)	REFERENCE (10)
H...	12	2.884 × 1010	s	5.498 × 106	8.28 ± 0.05	2.884 × 1010	12	By definition
He...	10.899 ± 0.01	2.288 × 109	s	0.6040	1.32	2.288 × 109	10.899 ± 0.01	See § 2.3.1.1
Li...	3.28 ± 0.06	55.47	m	55.47	3.28 ± 0.06	0.3631	1.10 ± 0.10	1994	1
Be...	1.41 ± 0.08	0.7374	m	0.7374	1.41 ± 0.08	0.4074	1.15 ± 0.20	1975	2
B...	2.78 ± 0.04	17.32	m	17.32	2.78 ± 0.04	14.45	2.7+0.21 - 0.12	1999	3
C...	8.39 ± 0.04	7.079 × 106	s	7.724 × 105	7.43 ± 0.06	7.079 × 106	8.39 ± 0.04	2002	4
N...	7.83 ± 0.11	1.950 × 106	s	5.535 × 104	6.28 ± 0.07	1.950 × 106	7.83 ± 0.11	2001, 2002	4, 5
O...	8.69 ± 0.05	1.413 × 107	s	7.552 × 106	8.42 ± 0.02	1.413 × 107	8.69 ± 0.05	2001	6
F...	4.46 ± 0.06	841.1	m	841.1	4.46 ± 0.06	1047	4.56 ± 0.30	1969, sunspot	7
Ne...	7.87 ± 0.10	2.148 × 106	s	2.355 × 10-3	-1.09	2.148 × 106	7.87 ± 0.10	See § 2.3.1.2
Na...	6.30 ± 0.03	5.751 × 104	a	5.747 × 104	6.30 ± 0.03	5.754 × 104	6.30 ± 0.03	1998	8
Mg...	7.55 ± 0.02	1.020 × 106	a	1.040 × 106	7.56 ± 0.02	1.000 × 106	7.54 ± 0.06	2001	5
Al...	6.46 ± 0.02	8.410 × 104	a	8.308 × 104	6.46 ± 0.02	8.511 × 104	6.47 ± 0.07	1984	9
Si...	7.54 ± 0.02	1.000 × 106	a	1.00 × 106	7.54 ± 0.02	1.00 × 106	7.54 ± 0.05	2001	5
P...	5.46 ± 0.04	8373	a	7833	5.43 ± 0.04	8913	5.49 ± 0.04	1997	10
S...	7.19 ± 0.04	4.449 × 105	m	4.449 × 105	7.19 ± 0.04	4.634 × 105	7.20 ± 0.05	See § 2.3.4
Cl...	5.26 ± 0.06	5237	m	5237	5.26 ± 0.06	9120	5.5 ± 0.3	1972, sunspot	11
Ar...	6.55 ± 0.08	1.025 × 105	t	9.622 × 10-3	-0.48	1.025 × 105	6.55 ± 0.08	See § 2.3.1.3
K...	5.11 ± 0.05	3692	a	3582	5.09 ± 0.05	3802	5.12	1978	12
Ca...	6.34 ± 0.03	6.287 × 104	a	5.968 × 104	6.32 ± 0.03	6.607 × 104	6.36 ± 0.02	1984	9
Sc...	3.07 ± 0.04	34.20	m	34.20	3.07 ± 0.04	42.66	3.17 ± 0.10	1993	13, 14
Ti...	4.92 ± 0.03	2422	m	2422	4.92 ± 0.03	3020	5.02 ± 0.06	1996	15
V...	4.00 ± 0.03	288.4	a	288.4	4.00 ± 0.03	288.4	4.00 ± 0.02	1989	16
Cr...	5.65 ± 0.05	1.286 × 104	a	1.313 × 104	5.66 ± 0.05	1.259 × 104	5.64 ± 0.13	1978	17
Mn...	5.50 ± 0.03	9168	m	9168	5.50 ± 0.03	7079	5.39 ± 0.03	1984	18
Fe...	7.47 ± 0.03	8.380 × 105	a	8.632 × 105	7.48 ± 0.03	8.128 × 105	7.45 ± 0.08	2001	5
Co...	4.91 ± 0.03	2323	a	2246	4.89 ± 0.03	2399	4.92 ± 0.08	1982	19
Ni...	6.22 ± 0.03	4.780 × 104	a	4.780 × 104	6.22 ± 0.03	4.780 × 104	6.22 ± 0.13	1980	20
Cu...	4.26 ± 0.06	527.0	m	527.0	4.26 ± 0.06	467.7	4.21 ± 0.04	1989	21
Zn...	4.63 ± 0.04	1226	a	1250	4.64 ± 0.04	1202	4.62 ± 0.15	1988	22
Ga...	3.10 ± 0.06	35.97	m	35.97	3.10 ± 0.06	21.88	2.88 ± 0.10	1984, 1989	9, 21
Ge...	3.62 ± 0.05	120.6	m	120.6	3.62 ± 0.05	109.6	3.58 ± 0.05	1999	23
As...	2.32 ± 0.05	6.089	m	6.089	2.32 ± 0.05	...	...	...
Se...	3.36 ± 0.04	65.79	m	65.79	3.36 ± 0.04	...	...	...
Br...	2.59 ± 0.09	11.32	m	11.32	2.59 ± 0.09	...	...	...
Kr...	3.28 ± 0.08	55.15	t	1.643 × 10-4	-2.24	55.15	3.28 ± 0.08	1993, see § 2.3.1.4	24
Rb...	2.36 ± 0.06	6.572	m	6.572	2.36 ± 0.06	11.48	2.60	1972	25
Sr...	2.91 ± 0.04	23.64	a	23.30	2.91 ± 0.04	23.99	2.92 ± 0.05	2000	26
Y...	2.20 ± 0.03	4.608	a	4.538	2.20 ± 0.04	4.677	2.21 ± 0.02	1994	27
Zr...	2.60 ± 0.03	11.33	a	11.45	2.60 ± 0.02	11.22	2.59 ± 0.04	1994	27
Nb...	1.42 ± 0.03	0.7554	a	0.7522	1.42 ± 0.03	0.7586	1.42 ± 0.06	1985	28
Mo...	1.96 ± 0.04	2.601	a	2.804	1.99 ± 0.04	2.399	1.92 ± 0.05	1983	29
Ru...	1.82 ± 0.08	1.900	a	1.806	1.80 ± 0.08	1.995	1.84 ± 0.07	1984	30
Rh...	1.11 ± 0.03	0.3708	a	0.3613	1.10 ± 0.02	0.3802	1.12 ± 0.12	1982	31
Pd...	1.70 ± 0.03	1.435	a	1.457	1.70 ± 0.02	1.413	1.69 ± 0.04	1982	31
Ag...	1.23 ± 0.06	0.4913	m	0.4913	1.23 ± 0.06	(0.251)	(0.94)	1984	9
Cd...	1.74 ± 0.03	1.584	m	1.584	1.74 ± 0.03	1.698	1.77 ± 0.11	1990	32
In...	0.80 ± 0.03	0.1810	m	0.1810	0.80 ± 0.03	1.047	1.56 ± 0.2	2002	33
Sn...	2.11 ± 0.04	3.733	m	3.733	2.11 ± 0.04	2.884	2.0 ± 0.3	1976	34
Sb...	1.06 ± 0.07	0.3292	m	0.3292	1.06 ± 0.07	0.2884	1.0 ± 0.3	1976	34
Te...	2.22 ± 0.04	4.815	m	4.815	2.22 ± 0.04	...	...	...
I...	1.54 ± 0.12	0.9975	m	0.9975	1.54 ± 0.12	...	...	...
Xe...	2.27 ± 0.02	5.391	t	3.495 × 10-4	-1.92	5.391	2.27 ± 0.02	2002, see § 2.3.1.4	35
Cs...	1.10 ± 0.03	0.3671	m	0.3671	1.10 ± 0.03	...	...	...
Ba...	2.18 ± 0.03	4.351	a	4.436	2.19 ± 0.03	4.266	2.17 ± 0.07	1994	27
La...	1.18 ± 0.06	0.4405	m	0.4405	1.18 ± 0.06	0.3890	1.13 ± 0.03	2001	36
Ce...	1.61 ± 0.02	1.169	m	1.169	1.61 ± 0.02	1.096	1.58 ± 0.09	1994	27
Pr...	0.78 ± 0.03	0.1737	m	0.1737	0.78 ± 0.03	0.1479	0.71 ± 0.08	1979	37
Nd...	1.46 ± 0.03	0.8355	m	0.8355	1.46 ± 0.03	0.912	1.50 ± 0.12	1985	38
Sm...	0.95 ± 0.04	0.2542	m	0.2542	0.95 ± 0.04	0.2818	0.99	1994	27
Eu...	0.52 ± 0.04	0.09513	a	0.09475	0.52 ± 0.04	0.09550	0.52 ± 0.04	2001	39
Gd...	1.06 ± 0.02	0.3321	m	0.3321	1.06 ± 0.02	0.3802	1.12 ± 0.04	1988	40
Tb...	0.31 ± 0.03	0.05907	m	0.05907	0.31 ± 0.03	0.05495	0.28 ± 0.30	2001	41
Dy...	1.13 ± 0.04	0.3862	m	0.3862	1.13 ± 0.04	0.3981	1.14 ± 0.08	1993	42
Ho...	0.49 ± 0.02	0.08986	m	0.08986	0.49 ± 0.02	0.09772	0.53 ± 0.10	2002	33
Er...	0.95 ± 0.03	0.2554	m	0.2554	0.95 ± 0.03	0.2455	0.93 ± 0.06	1984	43
Tm...	0.11 ± 0.06	0.03700	m	0.03700	0.11 ± 0.06	(0.0288)	(0.00 ± 0.15)	1984	9
Yb...	0.94 ± 0.03	0.2484	m	0.2484	0.94 ± 0.03	0.3467	1.08 ± 0.15	1984, 1989	9, 21
Lu...	0.09 ± 0.06	0.03572	m	0.03572	0.09 ± 0.06	0.03311	0.06 ± 0.10	1998	44
Hf...	0.77 ± 0.04	0.1699	m	0.1699	0.77 ± 0.04	0.2188	0.88 ± 0.08	1976	45
Ta...	-0.14 ± 0.03	0.02099	m	0.02099	-0.14 ± 0.03	...	...	...
W...	0.65 ± 0.03	0.1277	m	0.1277	0.65 ± 0.03	(0.372)	(1.11 ± 0.15)	1984	9
Re...	0.26 ± 0.04	0.05254	m	0.05254	0.26 ± 0.04	...	...	...
Os...	1.37 ± 0.03	0.6738	m	0.6738	1.37 ± 0.03	0.8128	1.45 ± 0.10	1984	46
Ir...	1.35 ± 0.03	0.6448	m	0.6448	1.35 ± 0.03	0.6918	1.38 ± 0.05	1988	47
Pt...	1.67 ± 0.03	1.357	m	1.357	1.67 ± 0.03	1.585	1.74	1987	48
Au...	0.83 ± 0.06	0.1955	m	0.1955	0.83 ± 0.06	(0.295)	(1.01)	1989	21
Hg...	1.16 ± 0.18	0.4128	m	0.4128	1.16 ± 0.18	...	...	See § 2.3.6
Tl...	0.81 ± 0.04	0.1845	m	0.1845	0.81 ± 0.04	(0.15 0.36)	(0.721.10)	1972, sunspot	49
Pb...	2.05 ± 0.04	3.258	m	3.258	2.05 ± 0.04	2.884	2.00 ± 0.06	2000	50
Bi...	0.68 ± 0.03	0.1388	m	0.1388	0.68 ± 0.03	...	...	...
Th...	0.09 ± 0.04	0.03512	m	0.03512	0.09 ± 0.04	...	...	1996, blended line	15
U...	-0.49 ± 0.04	9.306 × 10-3	m	9.306 × 10-3	-0.49 ± 0.04	<9.772 × 10-3	<-0.47	1984	9

NOTE.See text for detailed description of table. Data in parentheses are uncertain. Mass fractions in photosphere: X = 0.7491, Y = 0.2377, Z = 0.0133; Z/X = 0.0177. The astronomical log scale and the cosmochemical abundance scale by number are coupled by A(El) = log[N(El)] + 1.540.
     ^a Recommended photospheric value from s = spectroscopy, m = meteoritic, a = average of spectroscopy and CI chondrites, t = theoretical value.

References.(1) Carlsson et al. 1994; (2) Chiemlewski et al. 1975; (3) Cunha & Smith 1999; (4) Allende Prieto et al. 2002; (5) Holweger 2001; (6) Allende Prieto et al. 2001; (7) Hall & Noyes 1969; (8) Baumüller, Butler, & Gehren 1998; (9) Grevesse 1984; (10) Berzonsh, Svanberg, & Biémont 1997; (11) Hall & Noyes 1972; (12) Lambert & Luck 1978; (13) Grevesse & Noels 1993; (14) Neuforge 1993; (15) Grevesse et al. 1996; (16) Biémont et al. 1989; (17) Biémont, Grevesse, & Huber 1978; (18) Booth, Blackwell, & Shallis 1984; (19) Cardon et al. 1982; (20) Biémont et al. 1980; (21) Anders & Grevesse 1989; (22) Sneden & Crocker 1988; (23) Biémont et al. 1999; (24) Palme & Beer 1993; (25) Hauge 1972; (26) Barklem & O'Mara 2000; (27) Gratton & Sneden 1994; (28) Hannaford et al. 1985; (29) Biémont et al. 1983; (30) Biémont et al. 1984; (31) Kwiatkowski et al. 1982; (32) Youssef, Dönszelmann, & Grevesse 1990; (33) Bord & Cowley 2002; (34) Ross & Aller 1976; (35) Reifarth et al. 2002; (36) Lawler, Bonvallet, & Sneden 2001; (37) Biémont, Grevesse, & Hauge 1979; (38) Ward et al. 1985; (39) Lawler et al. 2001b; (40) Bergström et al. 1988; (41) Lawler et al. 2001a; (42) Grevesse, Noels, & Sauval 1993; (43) Biémont & Youssef 1984; (44) Bord, Cowley, & Mirijanian 1998; (45) Andersen, Petersen, & Hauge 1976; (46) Kwiatkowski et al. 1984; (47) Youssef & Khalil 1988; (48) Youssef & Khalil 1987; (49) Lambert, Mallia, & Smith 1972; (50) Biémont et al. 2000.