๐”– Bobbio Scriptorium
โœฆ   LIBER   โœฆ

Coronal magnetic field patterns inferred from radio observations

โœ Scribed by M. F. Lantos-Jarry

Publisher
Springer
Year
1970
Tongue
English
Weight
316 KB
Volume
15
Category
Article
ISSN
0038-0938

No coin nor oath required. For personal study only.

โœฆ Synopsis

A noise storm center clearly associated to an active center has been followed from January 2 to January 8, 1969. The study of the mean distribution of continuum and of type 1 bursts has shown a global and systematic displacement interpreted in terms of the coronal magnetic structure. This structure is formed by field lines connecting the active center to a stable region of inverse polarity, characterized by the existence of a coronal condensation. These results show the possibility of using this method for the systematic study of coronal magnetic structures, the knowledge of which is vital as far as the problems of particle propagation in the corona and in the interplanetary medium are concerned.

๐Ÿ“œ SIMILAR VOLUMES

Coronal magnetic fields from microwave p
Coronal magnetic fields from microwave polarization observations
โœ C. E. Alissandrakis; F. Borgioli; F. Chiuderi Drago; M. Hagyard; K. Shibasaki ๐Ÿ“‚ Article ๐Ÿ“… 1996 ๐Ÿ› Springer ๐ŸŒ English โš– 963 KB

The solar active region (AR) 7530 was observed at 6 cm on July 3 and 4, 1993 with the Westerbork Synthesis Radio Telescope, using a multi-channel receiver with very narrow bandwidth. We compare the radio data with Yohkoh SXT observations and with the magnetic field extrapolated from the Marshall ve

Coronal magnetic field structure derived
Coronal magnetic field structure derived from two-frequency radioheliograph observations
โœ K. Kai; K. V. Sheridan ๐Ÿ“‚ Article ๐Ÿ“… 1974 ๐Ÿ› Springer ๐ŸŒ English โš– 577 KB

An exceptional variety of positions and polarizations was found for two type I storms and numerous sporadic bursts observed during 15 consecutive days with the Culgoora radioheliograph at 80 and 160 MHz. The radio data are combined with optical data to derive a model of the coronal magnetic field st