๐”– Bobbio Scriptorium
โœฆ   LIBER   โœฆ

The height of 9.1 cm solar emission from latitude shift

โœ Scribed by W. Graf; R. N. Bracewell

Publisher
Springer
Year
1973
Tongue
English
Weight
416 KB
Volume
28
Category
Article
ISSN
0038-0938

No coin nor oath required. For personal study only.

โœฆ Synopsis

Active regions that are sources of microwave solar emission should appear displaced in latitude relative to the associated optical feature and from this displacement it should be possible to deduce the height. Although the displacement is only about one-third of a rain of' arc at the most, it was found possible, in an investigation based on 1264 cases in 1970, to obtain a height with a precision as good as or better than has generally been achieved in previous studies based on the rate of motion in longitude. This success could be due to the possibility of using large quantities of data or to tolerance of the method to both terrestrial atmospheric refraction and proper motion in heliographic longitude. The result obtained for 1970 was 18000 โ€ข 5000 km (standard deviation). Application of the latitude method at other wavelengths would be desirable.

๐Ÿ“œ SIMILAR VOLUMES

Latitude and solar-cycle dependence of t
Latitude and solar-cycle dependence of the height of 9.1 cm radio emission
โœ W. Graf; R. N. Bracewell ๐Ÿ“‚ Article ๐Ÿ“… 1973 ๐Ÿ› Springer ๐ŸŒ English โš– 602 KB

The apparent height of radio sources above the photosphere was determined for the period of 1968-1971, by a method which makes use of the displacement in latitude of the centroid of the radio emission relative to the associated optical feature. The apparent height fell progressively in time by amou

Comparison of the 9.1cm and soft X-ray e
Comparison of the 9.1cm and soft X-ray emission from an active region
โœ M. Gerassimenko; J. T. Nolte; R. D. Petrasso ๐Ÿ“‚ Article ๐Ÿ“… 1976 ๐Ÿ› Springer ๐ŸŒ English โš– 393 KB

Thermal bremsstrahlung from the X-ray observed plasma accounts for most of the observed 9.1 cm emission from McMath 12336, an old, spotless active region, on June 2, 1973. This implies that only a small fraction of the emission measure within the active region is in the range around 106 K and below.