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Observation of a Coronal Disturbance from 1 to 9 R⊙

Published online by Cambridge University Press:  25 May 2016

R. T. Stewart ,
Marie K. McCabe ,
M. J. Koomen ,
R. T. Hansen  and
G. A. Dulk
R. T. Stewart
Affiliation:
Institute for Astronomy, University of Hawaii, Honolulu, HI, U.S.A.
Marie K. McCabe
Affiliation:
On leave from Division of Radiophysics, CSIRO, Sydney, Australia
M. J. Koomen
Affiliation:
Naval Research Laboratory, Washington, D.C., U.S.A.
R. T. Hansen
Affiliation:
High Altitude Observatory, NCAR, Boulder, Colo., U.S.A.
G. A. Dulk
Affiliation:
Institute for Astronomy, University of Hawaii, Honolulu, HI, U.S.A.

Abstract

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(Solar Phys.). On 1973 January 11, a flare near the west limb of the Sun caused a coronal disturbance which was observed with a unique variety of instruments. Radio observations of a type II and a moving type IV burst were obtained by the CSIRO Division of Radiophysics at Culgoora, Australia; white-light observations of a large, moving cloud were made by the U.S. Naval Research Laboratory coronagraph on OSO-7; K-corona observations of a decrease in coronal density were made by the High Altitude Observatory at Mauna Loa, Hawaii and Hα observations of a flare spray were made by the Institute for Astronomy, University of Hawaii at Haleakala (and also by H.A.O.).

Type
Part III Shock Waves and Plasma Ejection
Information
Symposium - International Astronomical Union , Volume 57: Coronal Disturbances , 1974 , pp. 337 - 341
Copyright
Copyright © Reidel 1974