منابع مشابه
Line formation in solar granulation III .
Using realistic hydrodynamical simulations of the solar surface convection as 3D, time-dependent, inhomoge-neous model atmospheres, the solar photospheric Si abundance has been determined to be log ǫ Si = 7.51 ± 0.04. This constitutes a difference of 0.04 dex compared with previous estimates based on the 1D Holweger-Müller (1974) model, of which half is attributable to the adopted model atmosph...
متن کاملLine formation in solar granulation: V. Missing UV-opacity and the photospheric Be abundance
The possibility of unaccounted for opacity sources in the UV for late-type stars has often been invoked to explain discrepancies between predicted and observed flux distributions and spectral line strengths. Such missing UV-opacity could among other things have a significant impact on abundance determination for elements whose only relevant spectral features are accessible in this wavelength re...
متن کاملLine formation in solar granulation III. The photospheric Si and meteoritic Fe abundances
Using realistic hydrodynamical simulations of the solar surface convection as 3D, time-dependent, inhomogeneous model atmospheres, the solar photospheric Si abundance has been determined to be log Si = 7.51 ± 0.04. This constitutes a difference of 0.04 dex compared with previous estimates based on the 1D Holweger-Müller (1974) model, of which half is attributable to the adopted model atmosphere...
متن کاملThe 671 nm Li i line in solar granulation
The astrophysically very interesting Li i 671 nm line has been observed with high spatial resolution in solar granulation with the intention to diagnose departures from local thermodynamic equilibrium (LTE) in the line formation. The spectral feature is very weak, so this is also a test on the limits of such observations. The observations of the Li i line and other weak lines nearby are compare...
متن کاملOxygen lines in solar granulation II. Centre-to-limb variation, NLTE line formation, blends and the solar oxygen abundance
Context. There is a lively debate about the solar oxygen abundance and the role of 3D models in its recent downward revision. These models have been tested using high resolution solar atlases of flux and disk-centre intensity. Further testing can be done using centreto-limb variations. Aims. Using high resolution and high S/N observations of neutral oxygen lines across the solar surface we seek...
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ژورنال
عنوان ژورنال: Astronomy & Astrophysics
سال: 2005
ISSN: 0004-6361,1432-0746
DOI: 10.1051/0004-6361:20034328e