Coronal magnetic fields
โ Scribed by G. A. Dulk; D. J. McLean
- Publisher
- Springer
- Year
- 1978
- Tongue
- English
- Weight
- 994 KB
- Volume
- 57
- Category
- Article
- ISSN
- 0038-0938
No coin nor oath required. For personal study only.
โฆ Synopsis
The observational evidence on the strength of the coronal magnetic field above active regions is reviewed. Recent advances in observations and plasma theory are used to determine which data are the more reliable and to revise some earlier estimates of field strength. The results from the different techniques are found to be in general agreement, and the relation B=O.5[(R/Ro)-l]-lSG, 1.02 ~< R/R| <<-10 is consistent with all the data to within a factor of about 3.
๐ SIMILAR VOLUMES
Slow photospheric motions can produce flow speeds in the corona which are fast enough to violate quasi-static evolution. Therefore, high-speed flows observed in the corona are not necessarily due to a loss of equilibrium or stability. In this letter we present an example where the flow speed increas
Coronal electric currents are superposed on the calculated large-scale current-flee (potential) magnetic field of the solar corona and the new magnetic configurations are mapped. The results indicate that relatively large coronal electric currents are required before significant topological deviatio
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
A long-standing misconception about the mathematical validity of utilizing Green's function solutions to coronal magnetic fields is discussed. Although this type of solution does not fit the observed line-of-sight component of the photospheric magnetic field, but rather the net flux in a region, the