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Standing Committee on Observational Activities
Programme for Solar Eclipse of July 20, 1963,

Bulletin No. 3	   Basic Observation Programme	March 15, 1963
Section A. Precision Observations

    In this bulletin we cover briefly the procedure to be followed for each of the
projects that come under the heading of Precision Observations, as outlined in Bulletin


    All reports must give the observer's co-ordinates - latitude, longitude and elevation
above sea level for there is little value in making precision observations unless the
observer knows exactly where he is when he. makes then. For those who have neither the
instruments nor the experience to make an actual survey, the best method is to plot one's
position on a government survey map from which the co-ordinates can then be calculated
with a fair degree of accuracy. If survey maps are not obtainable, the observer's pos-
ition can be plotted on a road map, with a notation giving the distance, as measured by
car speedometer, from the nearest intersection. This road map is then attached to the
observation report. The method of determining co-ordinates or position should always
be stated in the report.


    There are several methods of timing and the one selected will depend on the degree
of accuracy required, the equipment available and personnel available. Four methods
are described below. (Anyone using more elaborate methods needs no guidance from us!)
The timing method used should be stated on the observation report.

(1) With Ordinary Watch. If an ordinary watch or clock with a second hand is used,
    two persons are required - one to watch the phenomenon and one to watch the watch.
    When the observer calls "Time!" the timekeeper notes the time, to the split second
    if possible. This involves some sacrifice on the part of the timekeeper, for he
    cannot take his eyes off the watch. The timekeeper has a record sheet handy and
    several minutes before the phenomenon is scheduled to occur he begins to write
    down the time each minute, making a pencil stroke as each second elapses. He then
    has a means of re-checking his timings later.

        The watch used should be set by radio time signals and its accuracy checked
    for some period both before and after the event. If short-wave time signals are
    not available, then the Dominion Observatory one o'clock time signal on the broad-
    cast band can be used, in which ease the watch must be checked for several days,
    both before and after, and the error noted. The timings should not be adjusted
    for watch error but the record of watch errors should accompany the report.

(2) With Short-Wave Radio. Two persons. are required for this method - one to observe
    the phenomenon and one to record the tine. The timekeeper follows much the same
    procedure as under (1) above, except that he listens instead of watches, writing
    down the time each minute and recording each second that elapses. This method is
    somewhat more accurate than Method (1) but requires great concentration on the
    part of the timekeeper, who will be completely lost if he allows his attention to
    be distracted even momentarily. Also, it is, dependent on good reception throughout.

Eclipse Bulletin No. 3 cont'd.


(3) With stopwatch and Short-Wave Radio. Equipped With a stopwatch and short-wave
    radio, the observer can be his own timekeeper. He starts the watch when the
    phenomenon occurs and then stops it at a given time signal. By deducting the
    watch reading from the given time, one obtains tie observed time of the phenon3enon.
    The stopwatch should be stopped on the next time signal possible, preferably with-
    in five minutes, for if it is allowed to ran too long, the accuracy of the watch
    will have to be checked as under (i) above, Method (3) is much more accurate than
    either (1) or (2) but is dependent on good radio reception,

(4) With Short-Wave Radio and Tape Recorder. With radio and tape recorder running
    continuously, both time signals arid the voice of the observer as he calls "Time!"
    are it corded on the tape. This method has both advantages and disadvantages. It
    can be extremely accurate and the observer can record all other details of this
    observation on the tape. However, reports are not available immediately. Much
    playback time is required before written: reports can be produced. Also, because
    extraneous noise can be a serious handicap, the method is probably better suited
    to a lone observer than a group effort. 

    It can be seen that the timekeeper is a very important member of the team. Both
timekeeper and observer must become thoroughly familiar with the procedure to be foll
owed, the equipment end time signals to be used. It is recommended that several drills
be held well in advance of eclipse day.


    Attached is a copy of Report Form No I that can be adapted to most observations
in this section of the programne ù Where the observer makes a series of observations
of the same nature, such as the occultation of sun-spots, the information could be
arranged in tabular form on one report. Otherwise, a separate form should,be completed
for each. observation made. (In an organized field station, some of the work will be
centralized such as recording of seeing conditions, etc. thus relieving the indiv-
idual observers of the necessity of recording this detail. This will be described in
a later bulletin.) 


    It cannot be emphasized too strongly.that where binoculars or telescopes are to
be used, extreme care must be taken to protect the eyes during the partial phases,''
for permanent blindness would result if the eyes are exposed even momentarily to the
light of the sun. For binoculars, a welder's glass placed over the objectives would
be sufficient. For telescopes, union one has proper solar equipment an objective
diaphragm, Herschel wedge and solar eyepiece filter - it is safer to use the projection.
method, projecting the sun's image onto. a screen attached by rods to the telescope
the eye will be exposed to the sun's heat.

    Even those who just want to watch the partial phases of the eclipse with the
unaided eye should quip themselves with some protection a piece of heavily exposed
film or dark glass, preferably welder's glass.

                                         - 2 -

Eclipse Bulletin No. 3 cont'd.



    This is a straightforward observation that can be performed, without optical
equipment, by junior members or by members who feel that they lack the experience
to undertake anything more difficult.  It can be developed into a project in which
the general public can participate, as will be described in a later bulletin. For
this observation we are not interested in the time at which totality occurs but
simply in the length of the period of totality. This should be timed, as accurately
as possible, using an ordinary watch with a second hand or a short-wave radio (see
timing methods (1) and (2) or a stopwatch.


    The main purpose for the accurate timing of the eclipse has been to determine
geodetic positions. While it is true that more accurate results can now be obtained
using satellite orbits, the timing of contacts is nevertheless of considerable
interest. The beginning and end of totality (2nd and 3rd contacts) are very defin-
ite and can be observed without optical aid. They should be timed with great acc-
uracy, to the split second if possible. If Timing Method (3) is used, two stop-
watches are needed, for there will not be time between contacts to check the watch
to time signals and have it ready for use again. Telescopes are needed to observe
the 1st and 4th contacts (the first and last contacts of the moon's disk with that
of the sun) which are very indefinite and cannot be timed with the same accuracy.
It might be better to reserve the telescopes for other work or possibly combine
timing of 1st and 4th contacts with observation of the occultation of sun-spots,
which is described below.


    The purpose of this project is to make available accurate timings of occultation
of sun-spots for correlation with radio observations of the sun made during the
eclipse. Preferably, the project should be undertaken by art experienced solar
observer, using a telescope equipped with a Herschel wedge, etc. or a projection
screen. The observer makes a regular solar observation earlier in the day, record-
ing the usual data, plotting on a disk the positions of all sun-spot groups and
ù assigning a number to each for ready reference in the eclipse report. During the
eclipse, between first contact and the beginning of totality, the observer clocks
the time at which each sun-spot. group is occulted by the moon.  If it is a large
group, contacts with both preceding and following edges should be clocked.  If it
is a small group, the time at which it is bisected should be clocked.  Although we
are going through a period of minimum solar activity, let us hope that there are
some conspicuous spots on the sun's disk that day. If there are a number, then
Timing Method (3) would not be practical because of the number of stopwatches
required. Occultations need be timed only to the nearest second and therefore any
of the other three timing methods can be used. The occultation reappearance of
the sun-spots can be clocked, too, of course.

                                      - 3 -

Eclipse Bulletin No 3 cont'd.


    For a brief instant at the beginning and end of totality, the narrow dark
Fraunhofer absorption lines of the sun's spectrum are reversed, that is, they shine
out as bright lines, the more intense background of the light from the surface of
the sun having been cut off. If binoculars are used to observe the flash spectrum,
a grating (4000 lines or more to the inch) should be placed over one objective and
welder's glass over the other. The observer can then watch the approach of totality
through one lens and be ready to observe the flash spectrum through the other. A
telescope can be used with either a grating over the objective or a spectroscope
attachment at. the eyepiece while the finder, with welder's glass over the objective,
can be used to watch the approach of totality The flash spectrum should be timed
as accurately as possible and the observer's impressions as to the, intensity of the
lines, etc. should be recorded. A clock drive on the telescope would be an advantage.


The shadow bands are fleeting shadows that race along the ground before ans
after the main shadow. The direction of these bands and their line of motion differ
before and after totality and with the position of the observer relative to the,line
of totality. They can be best seen against a white background. Therefore, two white
sheets should be spread on level ground- one to observe the bands before totality
and the other for after totality. A team of three is required - one timekeeper and
two observers.  The procession of shadow bands may last from ten to fifteen, seconds.
The observers call "Time!" the instant the bands appear and again when they disapp-
ear, the timekeeper recording the times to the nearest second.  One observer has a
supply of sticks or bamboo rods which, as the bands appear, he quickly places on
the sheet to indicate their direction and line of motion.  The other observer con-
centrates on the width of the bands, whether they are straight or wavy, their colour
and any other characteristics, The rods `are left in position so that, with the aid
of a compass, their true direction can be determined unhurriedly after totality is
over.  All such details as to time, duration, direction, will be of value from every
point on the eclipse path.  It will be seen that for this project the team will need
to practice to get operations down to a routine.


    There are two reasons for recording weather' conditions - (1) because of the.
effect of'the weather on observations made, and (2) because of the effect of the'
eclipse on atmospheric conditions. For the former, one needs no special equipment,
simply recording the observing conditions (seeing, transparency, cloud cover) during
the period of the eclipse. These should be recorded at five-minute intervals and;
in addition, whenever a change in conditions occurs. For the latter, Equipment con-
sisting of wet and dry thermometers, barometer, anometer, photometer, etc., should
be in operation for a full hour before first contact and a full hour again after
fourth contact.  During these two one-hour periods, readings should be made at five-
minute intervals. During the eclipse - the partial phases and totality readings
should be made at two-minute intervals. An electric clock, with sweep second hand,
would be sufficiently accurate for recording the readings. If possible, the equip-
ment should be installed on the previous day and the team should make readings for
the same period as on eclipse day. Not only will this furnish comparison graphs
but will give the team the practice needed to carry out operations smoothly on
eclipse day.

                                      - 4 -

Eclipse Bulletin No. 3 cont'd.


    The purpose of this project is to study the local effect of the eclipse on the
ionosphere by measuring changes in signal strength. The installation consists of
three or four receivers with signal strength meters. These are tuned in on diff-
erent radio stations both in the line of the eclipse and off the path. To establish
a norm, the equipment should be in operation for a full hour before first contact
and a full hour after fourth contact. During these two one-hour periods, signal
strength readings should be taken every minute. During the eclipse partial phases
and totality - readings should be recorded more frequently. Ten-second intervals
are suggested but these should be somewhat longer - 15 or 20 seconds - if it is
found that the signal remains fairly steady.

    If possible, the equipment should be installed on the previous day and the team
should go through the full routine for the same period as on eclipse day. Not only
will this furnish comparison graphs but will give the teams the practice needed to
carry out operations smoothly on eclipse day. Two persons should be assigned to
each receiver so that they can work on shifts.

    A special report form is being drawn up for this project and is available on

                             *    *    *    *    *    *

       We realize that the brief descriptions given here may leave some questions
unanswered. If you have any particular problems, please let us know and we shall try
to help you solve them. Additional copies of this bulletin and the report form are
available, in limited quantity, on request. Bulletins 4 and 5, covering Photo graphic
Projects and Visual Observations, will be issued shortly.

       In planning your programme we would caution you against being too ambitious.
The period of totality is very short. There will be no time for false starts. It is
better to undertake only one project and do it well than to attempt several with in-
different results. Also, if you have never seen a total eclipse of the sun, you will
want some tine just to enjoy this wonderful spectacle. So plan your programme well,
practice the routine, become thoroughly familiar with your equipment, and weather
permitting - all will go well on eclipse day.

       Please let us know about your plans as they develop and about any special
projects you may have in mind.

                                             Isabel K. Williamson
                                             National Co-ordinator 1963 Eclipse
                                             5162 Belmore Avenue,
                                             Montreal 29, Canada.

                                          - 5 -
Bulletin 3: Coordinates, Methods of Timing, etc.
Other Bulletins