๐”– Bobbio Scriptorium
โœฆ   LIBER   โœฆ

On the microturbulence in the solar photosphere

โœ Scribed by R. I. Kostik; T. V. Orlova

Publisher
Springer
Year
1979
Tongue
English
Weight
175 KB
Volume
62
Category
Article
ISSN
0038-0938

No coin nor oath required. For personal study only.

โœฆ Synopsis

The velocity of microturbulent motions in the solar photosphere at the level of formation of weak Fraunhofer lines (h-150 km) is found to be 0.1โ€ข kms -~. The observations have been performed with the double-pass spectrometer in Kiev. Apart from thermal motions and damping effects we have taken into account convective and wave motions when calculating the broadening of absorption lines.

As/nany investigators have shown (see review by Canfield and Beckers, 1976) the microturbulent component s of the velocity field in the solar photosphere is 1.0-3.5 km s -1. The accuracy of its determination depends strongly on the damping constant (in all methods) and on the velocity of regular currents in the solar photosphere (by trial and error method, the method of line halfwidths).

The values of damping constant y obtained recently in laboratories (BlackweU et al.

๐Ÿ“œ SIMILAR VOLUMES

Microturbulence and the effect of depart
Microturbulence and the effect of departures from LTE on photospheric iron lines
โœ H. Holweger ๐Ÿ“‚ Article ๐Ÿ“… 1973 ๐Ÿ› Springer ๐ŸŒ English โš– 149 KB

It is shown that depth-dependent departures from LTE such as obtained by Athay and Lites (1972) will not notably affect tile solar curve-of-growth of Fe L This implies that both abundance and microturbulence may be determined from this curve-of-growth assuming LTE, and excludes that microturbulence

Inhomogeneities in the solar photosphere
Inhomogeneities in the solar photosphere
โœ Thomas E. Margrave; Thomas L. Swihart ๐Ÿ“‚ Article ๐Ÿ“… 1969 ๐Ÿ› Springer ๐ŸŒ English โš– 293 KB

A model of the solar photosphere incorporating a simple two-stream representation of granulation is found to give a small but significant improvement in the continuous radiation field over a homogeneous model. It is common to assume that the pressure does not vary with horizontal position; however,

Molecules in the solar photosphere
Molecules in the solar photosphere
โœ M. C. Pande; V. P. Gaur; B. M. Tripathi ๐Ÿ“‚ Article ๐Ÿ“… 1969 ๐Ÿ› Springer ๐ŸŒ English โš– 230 KB

A consideration of the dissociation equilibrium of diatomic molecules in the Utrecht Reference Photosphere leads us to conclude that SH, SiO, CS, HF and HC1 may show up in enough concentrations in the solar atmosphere. The number above photosphere for these molecules is comparable with or more than

On the structure of the solar photospher
On the structure of the solar photosphere
โœ V. A. Krat ๐Ÿ“‚ Article ๐Ÿ“… 1973 ๐Ÿ› Springer ๐ŸŒ English โš– 416 KB

The current models of the solar photosphere consisting of a large number of vertical columns of plasma seem to be in contradiction with the new observational data obtained from the spectrograms taken during the third flight of the Soviet Solar Stratospheric Observatory (SSO) on 1970, July 30. As it