640612Lunar5_p2

Click on the thumbnail at the bottom right of this page to go to the bitmap scan of this document. The text of this document appears immediately below.

-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.