On the large scale brightness fluctuations in the solar atmosphere

✍ Scribed by V. A. Krat; V. I. Makarov; K. S. Tavastsherna

• Publisher: Springer
• Year: 1980
• Tongue: English
• Weight: 250 KB
• Volume: 68
• Category: Article
• ISSN: 0038-0938
• DOI: 10.1007/bf00156862

✦ Synopsis

The October 1976 spectroscopic observations of the solar chromosphere with the great coronagraph of the Kislovodsk Station of the Pulkovo Observatory were analysed using the autocorrelation method. The autocorrelation function and the power spectrum were calculated. It was found that the brightness distribution in the chromosphere is essentially bimodal and has characteristic scales of 1.2 • 104 km and 2.4 • 104 km. The supergranulation (3.5 x 104 km) in the brightness field was found to show up more faintly at all heights.

The large scale structure of the chromosphere in the chromospheric network (supergranulation) with specific systematic motions and considerable magnetic fields (Leighton et al., 1962;Simon and Leighton, 1964) has allowed us to draw the conclusion that large scale hydro-dynamic processes in the solar atmosphere through all levels may be connected with convection. This concept was later evolved and partly revised in a number of investigations (Mein