Observations of the Coronal Network
- 1 January 1971
- journal article
- Published by Cambridge University Press (CUP) in Symposium - International Astronomical Union
- Vol. 43, 663-666
- https://doi.org/10.1017/s0074180900023123
Abstract
Spectroheliograms of quiet regions obtained by the OSO-G satellite in chromospheric, transition zone, and coronal lines indicate that the chromospheric network as seen in Ca K can be resolved despite the low resolution (30 arc s) of OSO-G. The network pattern becomes more diffuse with increasing height, indicating that the magnetic field pattern spreads with height.Keywords
This publication has 20 references indexed in Scilit:
- 80 MHz observations of a moving type IV solar burst, March 1, 1969Solar Physics, 1970
- Observation of the magnetic structure of a type IV solar radio outburstSolar Physics, 1969
- Magnetic fields and the structure of the solar coronaSolar Physics, 1969
- Radio Evidence for the Propagation of Magnetohydrodynamic Waves along Curved Paths in the Solar CoronaPublications of the Astronomical Society of Australia, 1969
- A model for Type-IV emission in the solar burst of June 9, 1959 at decametric wavelengthsSolar Physics, 1968
- 80 MHz Photography of the Eruption of a Solar ProminenceNature, 1968
- Model of the High-Energy Phase of Solar FlaresNature, 1966
- Sweep-Frequency Measurements of Solar BurstsPublished by Springer Nature ,1965
- The Type IV Solar Radio Burst at Metre WavelengthsAustralian Journal of Physics, 1963
- The Solar Corona in Active Regions and the Thermal Origin of the Slowly Varying Component of Solar Radio Radiation.The Astrophysical Journal, 1961