๐”– Bobbio Scriptorium
โœฆ   LIBER   โœฆ

Depth of formation of lines in the solar atmosphere

โœ Scribed by L. Achmad

Publisher
Springer
Year
1992
Tongue
English
Weight
368 KB
Volume
138
Category
Article
ISSN
0038-0938

No coin nor oath required. For personal study only.

โœฆ Synopsis

A simple and reliable method has been established for the definition of the depth of formation of lines in a stellar atmosphere. It is based on the determination of the level of emission of the reemitted line radiation. The new definition, which is applied in this paper to the solar case, does not suffer from the ambiguities of previously derived expressions. We apply this method to two artificial weak Oxygen I lines as examples.

๐Ÿ“œ SIMILAR VOLUMES

A reconsideration of the effective depth
A reconsideration of the effective depth of line formation in planetary atmospheres
โœ K. D. Abhyankar; R. K. Bhatia ๐Ÿ“‚ Article ๐Ÿ“… 1984 ๐Ÿ› Springer Netherlands ๐ŸŒ English โš– 546 KB

A new definition of the effective depth of line formation is given which incorporates its dependence on the angle of emergence as well as on the position within the line. Solution obtained for isotropic scattering in the third approximation of discrete ordinates explains: (i) Variation of equivalent

The formation of Mgi4571 ร… in the solar
The formation of Mgi4571 ร… in the solar atmosphere
โœ Richard C. Altrock; C. J. Cannon ๐Ÿ“‚ Article ๐Ÿ“… 1972 ๐Ÿ› Springer ๐ŸŒ English โš– 426 KB

A one-dimensional analysis of the 4571 A, line of neutral magnesium is presented. The Harvard-Smithsonian Reference Atmosphere (HSRA) and the Bilderberg Continuum Atmosphere (BCA) are used to compute the emergent line profiles at various positions on the solar disc. The resultant profiles, when comp

The formation of Mgi4571 ร… in the solar
The formation of Mgi4571 ร… in the solar atmosphere
โœ Richard C. Altrock; C. J. Cannon ๐Ÿ“‚ Article ๐Ÿ“… 1973 ๐Ÿ› Springer ๐ŸŒ English โš– 624 KB

An analysis of the 4571 A line of neutral magnesium is presented in which one-dimensional macroscopic velocity fields are included. It is shown that gradients over restricted heights in the vertical and horizontal components of the velocity field of order --0.005 s -1 and --0.004 s -1 (such that vel