Plans for Coronascope II.

Abstract

One of the most outstanding problems of solar physics concerns the changes in the structure of the corona which may occur during transient disturbances on the solar disk as well as during the development and decay of a solar active region. The high spatial and time resolution available on photographs from a balloon- borne coronagraph suggests the advantage that such an instrument has in investigating the shorter term transients. The longer term development of the corona is, of course, more advantageously studied from a satellite-borne coronagraph. Since the sky at an altitude of 95 000 ft has a radiance of about 2 X 10-~ that of the mean solar disk in the near infrared, coronal photography to approximately 4 or 5 solar radii appears feasible. Since even the best coronagraph lens contributes a radiance of approximately 2 X 10-~, the lens must be shielded from direct photospheric light by an external occulting disk. A simple external occulting disk allows a reduction of the level of instrumentally scattered light to approximately 10-~. "Apodization" of the external occulting disk by one of several equivalent techniques allows the scattered light in the coronagraph to be reduced by another factor of 10. These apodization techniques are compared. The Coronascope II optical system, scheduled for flight late in the summer of 1963, is explained. The program has received continued support from the Office of Naval Research while the burden of the balloon operations will be borne by the National Center for Atmospheric Research Balloon Flying Facilit~~.

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