Solar Eclipse Observing--the Lunar Shadow and Sky Darkness
Introduction. As the moment of
totality approaches, the shadow of the moon sweeps out of the
west to immerse observers along its path. This spectacular
sight, often compared with that of an approaching thunderstorm,
is even visible—indeed, sometimes enhanced—when cloudy
weather threatens to obscure totality itself. With the arrival
of totality or a particularly deep annularity, the sky darkens
appreciably and the brighter stars and planets become visible.
Appearance. Noted portrait painter
Howard Russell Butler described the shadow’s appearance
through thin cloud cover over the Elkhorn Range and intervening
valley at Baker, Oregon for the eclipse of 8 June 1918:
…a greenish pallor overspread the
landscape,—but it was not very dark. To the northwest,
however, the sky was growing dark. The last half minute seemed
long. My eyes were fixed on the sky line. Suddenly the entire
range fell to a deep low–valued blue, and simultaneously the
lower part of the sky above the range turned to a rich yellow,
inclining to orange, streaked with two horizontal blue–gray
clouds. Above me the sky darkened rapidly. For an instant the
valley retained its light green color and then the shadow seemed
to rush toward us and all was engulfed…
Overcast skies disappointed unfortunate
observers viewing the 7 March 1970 total eclipse from
Florida’s panhandle. As consolation, however, the heavy cloud
cover provided an impressive canvas for an especially striking
apparition of the rolling, wave–like shadow as it swept out of
the Gulf of Mexico and across the Southeastern United States.
The appearance of the shadow varies
considerably depending upon the circumstances of the eclipse,
atmospheric conditions and the location of the observer with
respect to the center line. For instance, a sunrise eclipse will
cast a shadow resembling a truncated cone with its narrow end
pointing towards the horizon, while observers near the northern
or southern limits of the path find themselves surrounded by
asymmetrically illuminated horizons.
Even observers several hundred miles
outside of the path of totality have reported sightings of the
shadow sweeping along the horizon. Certainly, observers who, for
one reason or another, find themselves close to the path of
totality but unable to travel the remaining distance, would want
to attempt shadow sightings along with their observations of the
partial eclipse. Brilliant red and orange hues (the
sunrise–sunset effect) appear as horizon colors prior to,
during and just after totality.
Once the shadow’s leading edge has swept
over your site, the sky darkens significantly. Observers who
have adapted their vision with dark goggles prior to the onset
of totality have reported bright stars and planets becoming
visible more than a minute before the thin solar crescent is
obscured.
Similar sightings of celestial objects have
been reported in the much brighter skies of annular eclipses
since antiquity; observers are encouraged to include such
attempted sightings in their observing programs for annular and
very deep partial eclipses as well as for total eclipses of the
sun.
Procedures. In the 1970’s William
H. Glenn, York College of the City University of New York at
Jamaica, conducted and compiled extensive observations on the
appearance of the shadow. He developed a questionnaire which
still provides one of the best sets of guidelines for lunar
shadow and sky darkness observations. Among the major shadow and
sky aspects to note, Glenn includes:
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How many seconds before totality was
the shadow seen?
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In what direction did the shadow become
visible?
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How did its darkness, appearance and
color compare with the surrounding unshadowed sky?
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How would you describe its very rapid
motion and changing appearance, color and shape?
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In what directions did you have time to
look during as well as immediately before and after
totality?
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How would you describe the appearance
and color of the sky in each of these directions as totality
progressed?
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When and how did the shadow disappear?
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Describe how the light changed as the
eclipse progressed (include any times as accurately as
possible).
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What stars and planets were you able to
identify?
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How soon before totality did stars and
planets become visible?
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How long after the end of totality did
stars and planets disappear?
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What kind of weather conditions existed
during the eclipse (include the fraction of sky obscured by
clouds and the direction of clouds, types of clouds, cloud
coloration, sky coloration, haze, etc.)?
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Did you detect any color on the disk of
the moon during totality?
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How did the darkness and color of the
moon’s disk compare to the sky a few degrees away from the
eclipsed sun?
Observers should also estimate the degree
of darkness using such criteria as the readability of newspaper
headlines, ordinary newsprint, the hour or second hand of an
ordinary wrist watch, a standard eye chart or some similar
method. Measurements made with photoelectric cells or
photographic light meters would be of even greater value. Use
devices capable of measuring the incident light on a scale that
can be readily converted to lumens per square meter (or
foot–candles), and make frequent carefully–timed readings of
the intensity of illumination at the zenith and at the four
compass points along the horizon.
Locating even the brightest stars and
planets prior to totality can be difficult unless you know
exactly where to look and have taken some steps to dark–adapt
your vision in advance. This task has been greatly simplified by
widely published charts of the sky around the eclipsed sun. Such
charts, which appear in most periodicals and astronomical
handbooks for total and annular eclipses and a number of
excellent computer programs that produce such charts (see
Chapter 2), can be very useful in estimating the faintest
stellar magnitude visible. This, in turn, provides yet another
strong indicator of sky darkness.
Selecting a star or planet you have
identified during totality, and attempting to keep it in sight
in the rapidly brightening sky following totality, is an easier
chore.
Photography. While capturing the
essence of the lunar shadow is a task especially suited to
artists and poets, photographers having cameras equipped with
fish–eye lenses (a 180–degree field is ideal) have enjoyed
considerable success. Mount your camera on a level tripod, point
it at the zenith and orient it with respect to the compass
points (corrected for any difference between the earth’s
magnetic and geographic poles at the observing site), and each
frame should capture the entire sky from horizon to horizon,
showing the sunrise–sunset effect and darkness as the shadow
advances.
Glenn achieved good results by leaving the
lens wide open (about f/5.6) and making one–second exposures
every 15 seconds from a minute before until a minute after
totality on a moderately fast film (around ISO 200). This will
yield overexposed images at first, but as the shadow sweeps
over, exposures become ideal and produce a sequence of images
that is both pleasing and useful. Frames taken during totality
frequently show brighter stars and planets as well.
With the compass points penned onto each
photograph, it is a simple matter to determine the azimuth of
the approaching and receding shadow, and to relate any
sunrise–sunset effect noticed to an accurate position on the
horizon. The exact time of each exposure can be determined later
if a tape recorder is used to simultaneously record the
triggering of the camera shutter and WWV or CHU radio time
signals (see Chapter 5).
Video cameras with wide–field lenses or
attachments should produce impressive results as well, but
should be adjusted for full manual operation to prevent them
from automatically correcting for the diminishing light by
adjusting exposure times or f/–stops or both throughout the
eclipse.
Photograph 8-1 A 165º fish-eye lens was
used to capture the lunar shadow, easily seen in this 1/8
second exposure on Ektachrome 100 of the 26 February 1979
total solar eclipse north of Winnipeg, Manitoba. Photograph
taken by Mike Reynolds.
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