Infrared Coronal Observations at the 1991 Solar Eclipse

OBSERVATIONS OF THE 1991 ECLIPSE AT 3.5 mm WAVELENGTH

We report preliminary results of the partial eclipse seen from the BIMA millimeterwavelength interferometer in northern California. The use of an interferometer has many advantages over previous single-dish eclipse observations at 3 mm, and in particular it allows a quite different type of measurement of the height of the "3-mm limb" which is direct and precise : we find it to be 11.9" ± 0.4" a...

Solar coronal observations at high frequencies

The Solar Eclipse Coronal Imaging System (SECIS) is a simple and extremely fast, high-resolution imaging instrument designed for studies of the solar corona. Light from the corona (during, for example, a total solar eclipse) is reflected off a heliostat and passes via a Schmidt-Cassegrain telescope and beam splitter to two CCD cameras capable of imaging at 60 frames a second. The cameras are at...

Observations of Solar Coronal Magnetic

This review discusses methods for determining solar coro-nal magnetic elds, with an emphasis on radio measurements of eld strengths in solar active regions.

Observations of shadow bands at the total solar eclipse of 16 February 1980.

Photoelectric observations of short term light variations (shadow bands) at the 16 Feb. 1980 total solar eclipse have been made using a set of spatially separated PIN diodes. Light variations in a bandpass of 1-500 Hz were detected during the half-minutes preceding and following the total phase. Fourier analysis of the noise spectrum of the variations reveals a sharp drop-off for frequencies ab...

Solar eclipse safety.