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Some comments on the limb shift of solar lines

✍ Scribed by Jacques M. Beckers; William R. Taylor

Publisher
Springer
Year
1980
Tongue
English
Weight
344 KB
Volume
68
Category
Article
ISSN
0038-0938

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πŸ“œ SIMILAR VOLUMES

Some comments on the limb shift of solar
Some comments on the limb shift of solar lines
✍ Jacques M. Beckers; Paul Vegvar πŸ“‚ Article πŸ“… 1978 πŸ› Springer 🌐 English βš– 400 KB

It has been suggested that pressure shifts are the sole cause for the systematic blue shift of solar fraunhofer lines (Hart, 1974). To check this we evaluate the significance of pressure shifts for Fe I lines. The observed wavelength shifts of a large number of lines are compared with the shifts cal

Some comments on the limb shift of solar
Some comments on the limb shift of solar lines
✍ Jacques M. Beckers; George Driver Nelson πŸ“‚ Article πŸ“… 1978 πŸ› Springer 🌐 English βš– 943 KB

The well-known correlation between granulation intensity and velocity fluctuations causes a shift of the average line position called the 'convective blue shift'. It is argued that this convective blue shift is most likely reponsible for the limb effect of solar Fraunhofer lines. To explain the cent

The center-limb behavior of solar molecu
The center-limb behavior of solar molecular lines
✍ George L. Withbroe πŸ“‚ Article πŸ“… 1968 πŸ› Springer 🌐 English βš– 553 KB

The center-limb behavior of C2, CH, CN, CO, and MgH lines have been analyzed using five photospheric models. A three-stream model developed by G. Elste gave the most satisfactory results, providing evidence for the existence of inhomogeneities in the photospheric layers --2.5 ~< logzs0oo ~< --0.5.

Center-to-limb analysis of the solar oxy
Center-to-limb analysis of the solar oxygen lines
✍ Edith A. MΓΌller; Bodo Baschek; Hartmut Holweger πŸ“‚ Article πŸ“… 1968 πŸ› Springer 🌐 English βš– 965 KB

Several lines of neutral oxygen observed at various positions on the solar disk were used to study the influence of (1) the temperature distribution, (2) the velocity field, and (3) the damping on the line profiles and the abundance of oxygen in the photosphere. Theoretical profiles were calculated