Ground-based observations of the β Cephei CoRoT main target HD 180 642: abundance analysis and mode identification

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Volume 506 / No 1 (October IV 2009)

A&A, 506 1 (2009) 269-280

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The CoRoT space mission: early results

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Table 4:

Mean NLTE abundances (on the scale in which $\log \epsilon$ [H] = 12) and total 1- $\sigma$ uncertainties (in brackets), in units of the last digits.
	HD 180 642	B stars	Sun 1-D	Sun 3-D
He/H(4)	0.088(18)	$\sim$ 0.089	0.085(1)	0.085(2)
$\log \epsilon$ (C) (9)	8.21(10)	$\sim$ 8.20	8.52(6)	8.39(5)
$\log \epsilon$ (N) (21)	8.00(19)	$\sim$ 7.79	7.92(6)	7.78(6)
$\log \epsilon$ (O) (25)	8.53(14)	$\sim$ 8.58	8.83(6)	8.66(5)
$\log \epsilon$ (Ne) (6)	7.86(16)^a	$\sim$ 8.07	8.08(6)	7.84(6)
$\log \epsilon$ (Mg) (1)	7.34(20)	$\sim$ 7.48	7.58(5)	7.53(9)
$\log \epsilon$ (Al) (3)	6.22(15)	$\sim$ 6.08	6.47(7)	6.37(6)
$\log \epsilon$ (Si) (7)	7.19(19)	$\sim$ 7.20	7.55(5)	7.51(4)
$\log \epsilon$ (S) (4)	7.10(34)	$\sim$ 7.19	7.33(11)	7.14(5)
$\log \epsilon$ (Fe) (21)	7.34(21)	$\sim$ 7.36	7.50(5)	7.45(5)
${\rm [N/C]}$	-0.21(22)	$\sim$ -0.41	-0.60(9)	-0.61(8)
${\rm [N/O]}$	-0.53(24)	$\sim$ -0.79	-0.91(9)	-0.88(8)
Z	0.0099(16)	$\sim$ 0.0108	0.0172(12)	0.0124(7)

The number of spectral lines used is given in brackets in the first column. For comparison purposes, we provide typical values found for early B dwarfs in the solar neighbourhood (Morel 2009, and references therein; B stars), the standard solar composition of Grevesse & Sauval (1998, Sun 1-D), and updated values derived from three-dimensional hydrodynamical models (Asplund et al. 2005, Sun 3-D). We define [N/C] and [N/O] as $\log$ [ $\epsilon$ (N)/ $\epsilon$ (C)] and $\log$ [ $\epsilon$ (N)/ $\epsilon$ (O)], respectively. The metallicity, Z, is given in the last row. To compute this quantity, we assumed the abundances of Grevesse & Sauval (1998) for the trace elements not under study.
^a A negligible difference amounting to 0.01 dex is obtained when using the $T_{\rm eff}$ derived from the Ne ionisation balance (Morel & Butler 2008).

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