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-2- Fifteen craters recommended for this project are , from east to west Grinaldi, Aristarchus, Kepler, Copernicus, Pytheas (bright), Tinocharis, Tycho, Plato, Aristotelos, Eudoxus, Menelaus, Plinius, Taruntius, a bright ring arid Proclus. Colour and Intensity Observations The colour of the eclipsed moon, and also the degree of darkness of the eclipse, vary from one eclipse to another and depend in part upon conditions in the eartht atmosphere where refraction of the light from the sun into the earth's shadow takes place. Descriptions of the moon's colour vary with each observer, colour being subjective; therefore, observers are requested to use the tens in the accanpanying Danjon Scale unless the colour as seen differs completely with the Scale. In this case, the ob- server should describe it in his own Words. It will be seen that the Danjan Scale is also applicable to the darkness of the eclipse and wifl be used in conjunction with Fisher's Scale, which measures only the degree of darkness. Observers are requested to fantliarize themselves with each scale, and to use this terminology when reporting. It is important that the time of the observatiai be recorded as well as information about any optical aid employed. DANJON SCALE: (0) Very dark eclipse, moon almost invisible, especially mid-eclipse; (1) Dark eclipse, gray Or brownish oolounticsi, detail very vague; (2) Deep red or rust colour, very dark central area, outer edge relatively bright; (3) Brick red eclipse, usually with a bright Or yellow shadow rim; (4) Very bright copper red or orange eclipse with bluish, bright shadow edge. FISHER'S SCALE: (0) 6" telescope or larger needed to see "seas" and principal craters. (1) 2" or 3" aperture required for major detail. (2) Naked eye only needed to see principal details. The appearance of the shadow edge may not correspond with the general eclipse colour as outlined in the Danjon Scale. A notation should be made if this occurs and any unusual shape exhibited by the shadow edge should be noted. Soon after totality begins, intensity observations should be made and at 10-minute intervals thereafter until third contact. This should be the responsibility of those assigned to this observation (assuming a group is organized). The enclosed fonu for recording such data, in addition to the outlined discs which are to be used to indicate colour boundaries, may be obtained from the writer. Special Area Observation During a total lunar eclipse, the moon's surface is subject to rapid changes in temperature. These rapid changes may trigger observable effects in certain areas which have, on occasion, exhibited transitory changes in appearance which so far are not explained. Many such areas have bcen reported but it is not possible to devote the necessary study to all of these; hence three easily found craters which are suitable for most eclipse conditions have been selected. The first is the very bright crater Aristarchus and adjacent area. Late in 1963, astronomers at Larefl Observatory reported a redness surrounding this crater which seemed to change shape from minute to minute. This report was confirmed by a group of amateurs in Japan which observed a similar phenomenon on December 28th, 1963. This will be of prime interest in the forthcoming eclipse and should be observed with the largest aperture available at a magnification not less than 200 times. Close attention should also be paid to the adjoining crater Herodotus and cleft, all located on the north-east quadrant of the moon.