The solar photospheric nitrogen abundance - Analysis of atomic transitions with 3D and 1D model atmospheres

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Volume 498 / No 3 (May II 2009)

A&A, 498 3 (2009) 877-884

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Table 3:

A(N) of N I from line fitting using 1D models with SYNTHE.
Observed	$\lambda$	A(N) $_{\rm LTE}$			A(N) $_{\rm NLTE}$
spectrum	(nm)	HM	ATLAS9	$\ensuremath{\left\langle {\rm 3D}\right\rangle}$	$\ensuremath{\left\langle {\rm 3D}\right\rangle}$
KF	746.8	7.861	7.824	7.809	7.750
NF	746.8	7.874	7.837	7.827	7.768
NI	746.8	7.890	7.834	7.823	7.785
DI	746.8	7.908	7.849	7.840	7.802
KF	821.6	7.847	7.811	7.805	7.730
NF	821.6	7.918	7.870	7.867	7.792
NI	821.6	7.944	7.879	7.873	7.821
DI	821.6	7.808	7.752	7.746	7.694
KF	868.3	7.910	7.889	7.857	7.783
NF	868.3	7.906	7.877	7.857	7.783
NI	868.3	7.933	7.878	7.875	7.831
DI	868.3	7.932	7.886	7.882	7.838

Notes: Col. (1) is the observed spectrum identification, KF: Kurucz Flux, NF: Neckel Flux, NI: Neckel Intensity, and DI: Delbouille Intensity; Col. (2) is the wavelength; Cols. (3)-(5) the A(N) $_{\rm LTE}$ from line fitting with HM, ATLAS9, and $\ensuremath{\left\langle {\rm 3D}\right\rangle}$ model; Col. (6) is the A(N) $_{\rm NLTE}$ for the $\ensuremath{\left\langle {\rm 3D}\right\rangle}$ model, obtained by adding the NLTE-correction computed with $S_{\rm H}=1/3$ to the abundances given in Col. (5).

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