000002074 001__ 2074
000002074 005__ 20160701171658.0
000002074 0247_ $$2DOI$$a10.1051/0004-6361:20041951
000002074 037__ $$aASTROimport-231
000002074 100__ $$aAsplund, M.
000002074 245__ $$aLine formation in solar granulation. VI. [C I], C I, CH and C2 lines and the photospheric C abundance
000002074 260__ $$c2005
000002074 520__ $$aThe solar photospheric carbon abundance has been determined from [C I], C I, CH vibration-rotation, CH A-X electronic and C2 Swan electronic lines by means of a time-dependent, 3D, hydrodynamical model of the solar atmosphere. Departures from LTE have been considered for the C I lines. These turned out to be of increasing importance for stronger lines and are crucial to remove a trend in LTE abundances with the strengths of the lines. Very gratifying agreement is found among all the atomic and molecular abundance diagnostics in spite of their widely different line formation sensitivities. The mean value of the solar carbon abundance based on the four primary abundance indicators ([C I], C I, CH vibration-rotation, C2 Swan) is log ɛC = 8.39 ± 0.05, including our best estimate of possible systematic errors. Consistent results also come from the CH electronic lines, which we have relegated to a supporting role due to their sensitivity to the line broadening. The new 3D based solar C abundance is significantly lower than previously estimated in studies using 1D model atmospheres. 
000002074 700__ $$a Grevesse, N.
000002074 700__ $$a Sauval, A. J.
000002074 700__ $$a Allende Prieto, C.
000002074 700__ $$a Blomme, R.
000002074 773__ $$c693-705$$pAstronomy and Astrophysics$$v431$$y2005
000002074 85642 $$ahttp://esoads.eso.org/abs/2005A%26A...431..693A
000002074 905__ $$apublished in
000002074 980__ $$aREFERD