منابع مشابه
Oxygen 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...
متن کاملlines in photospheric granulation
The possibility of significant systematic errors due to the use of 1D homogeneous atmospheres in lithium-abundance determinations of cool stars motivates a study of non-localthermodynamic-equilibrium (nlte) effects on Li I line formation in a 3D solar-granulation simulation snapshot. The nlte effect on the equivalent width of the 671nm resonance line is small in 1D models or in integrated light...
متن کاملOxygen lines in solar granulation I. Testing 3D models against new observations with high spatial and spectral resolution
Aims. We seek to provide additional tests of the line formation of theoretical 3D solar photosphere models. In particular, we set out to test the spatially-resolved line formation at several viewing angles, from the solar disk-centre to the limb and focusing on atomic oxygen lines. The purpose of these tests is to provide additional information on whether the 3D model is suitable to derive the ...
متن کاملDynamics of the solar granulation
Excellent spectrograms can yield observational insight in the dynamics of the solar surface not yet accessible to numerical simulations. We present results of the elaboration of a series of spectrograms taken at the center of the solar disk. Each of the spectrograms includes more than 250 granules, while the series covers a time of 12 min. Our main emphasis is to study the dynamics of the visib...
متن کاملLine 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 کاملذخیره در منابع من
با ذخیره ی این منبع در منابع من، دسترسی به آن را برای استفاده های بعدی آسان تر کنید
ژورنال
عنوان ژورنال: Astronomy & Astrophysics
سال: 2009
ISSN: 0004-6361,1432-0746
DOI: 10.1051/0004-6361/200912840