PPAS considerations
Prioritysystem
Up to and including June 2008 every satellite acceptable for our PPAS
observation program was assigned a priority for observation. These ran
from 1 (most important) to 6 (least important). In practice the
satellites with priorities 4, 5 and 6 were barely observed. Therefore
I considered a simpler system where only the priorities 1 to 3 are
used:
1. is the priority in case the satellite is found to accelerate or
exhibits an unexpected brightness pattern
2. is the priority when some extra attention is requested
3. All other spacecraft with brightness variations of short duration
Initially a satellite gets priority 3 if it appears that it has
variable brightness.
Variable brightness
Each satellite has a brightness change while it moves from its rising
point through its culmination point to its setting point. The
brightness of the satellite depends on three things:
a. the distance between the observer
b. the phase, this is the angle between the sun, satellite and observer
c. the size and nature of the surface that reflects the sunlight. Some
objects have "diffuse" reflection and some have "specular" reflection.
Typically the latter
will have a larger range of brightness.
The first two cases are to be calculated, the latter not. A satellite
which does not or rotate or rotates very slowly (many minutes) will be
relatively faint when it is in the same direction as the sun and gets
brighter when it is more in the opposite direction. A satellite which
rotates will continuously reflect sunlight by another part of its
surface. If that surface is changing in size, the brightness is
varying. This is the case with rocket stages that rotate around their
minor axis, so tumbling. Often the magnitude variation is smaller at
"full" phase and larger at "half" or worse phase. The PPAS is about
these tumbling spacecraft.What we care about is the tumble period
regardless of the nature of the variation.
Sometimes I get observations within which a variation is reported
while there is only one maximum stated. Then I do not know whether
this is the normal brightness variation of steady objects or
variations due to rotation.
There are sometimes observations with two or three maxima and then no
more. These are often satellites of which I know from experience that
they do not, or sporadic tumble. One possible explanation is that some
flat surfaces are situated that they just reflect the sunlight toward
the observer. The satellite itself does not need to rotate.
Processing of the observations
Each submitted observation will be checked by me and corrected if
necessary. This may be adjustments to the PPAS format, editing the
comments and possibly add a reference to the notes file in which the
too long notes are copied. Observations which do not comply the PPAS
format, i.e. not mentioning a measured or guessed flash period are
copied to an alternate file. Possibly subsequent observations can give
rise to add those as yet to the PPAS file after some reconsideration.
Format of PPAS-observations.
This format was determined in the early nineties by several
BWGS-members and the and is still in use. My contribution dealt with
the mnemonics to keep comments as short as possible. The most
extensive description of format and mnemonics can be found at
http://www.satobs.org/tumble/flashpm.html # PPASformat
On the encodings for the brightness variations described there I have
the following additions:
1. The pattern A'A' can also be expressed simply with A. If only one
symbol, then it is obvious that it was counted on that maximum.
2. The same applies to F'F' that may be replaced by a single F.
3. Because the comma "," is used to indicate that the minima were
counted, this should not be used as a separator between the different
parts of a coded commentary. Since some years I use the semi-colon (;)
as a separator.
4. The word "mag" can be omitted for the magnitude value because the
plus "+" with a number following it is in itself clear.
An example of the four above-mentioned adjustments:
Original:
A'A' mag +3>7
New format:
A; +3>7
Note references
When I started sending the PPAS observations directly to Mike McCants
in 2004, the original notes file was not available to me. In order not
to use double allocations, I started again with notenummers but now
preceded by a "b". Furthermore, the reference are like "note b1". Only
later I realized that a reference "b1)" was better and applied this.
From launch year 2007 I apply the original note number "n)". It is my
intention once to join the two note files with the simplest note
numbers.
Reporting of the end time
When drafting the PPAS format it was agreed to report the time of the
last timed maximum (or minimum). In this way, with a TLE as close as
possible to the observation, a satellite track can be reconstructed.
For a serious analyst of PPAS observations there may be a lot to
derive. There was even suggested to do a positional observation at the
end of the flash observation. In practice, this never occurred perhaps
because this is a great strain.
Reporting of individual timings
It is with some observers increasingly common practice that all
individual timimgs were reported. I did it myself during some years
and found it useful only when the satellite in question shows really
different times between the maxima. For objects with regular flashing
periods it has no additional information. I noticed by myself that
there were sometimes differences of about one second between the
minimum and maximum flashtime on a regular satellite. This has to do
with how clearly defined the maxima are. With well defined flashes the
differences show to be much smaller.
My conclusion: You need not to include them if regular. With
irregularities they can be very useful when determining a period.
Detection of a flash period
By following a satellite in a transit as long as possible the presence
of a flash period can be detected. In case of short periods, many
maxima can be counted. In case of long periods, only few, if any. It
might be that a whole period (preferably between three successive
maxima) lasts longer than that the satellite takes to transit. The
latter also provides the upper limit of a well measurable flash
period. A high orbiting satellite can be followed longer than a low
one, giving more time to determine a flash period. For a geostationary
object one can use the whole night. Note that the changing phase angle
over a longer period if time can affect the accuracy of the
measurement.
Knowing by experience, I now follow a satellite with variable
brightness as long as possible during a transit. In case of doubt,
whether or not a variable brightness other than by change in phase
angle will then become clear. I have experienced more than once that a
satellite seemed steady and started flashing after its culmination
point. It may even happen that in two successive transits one shows a
steady object and the other a flashing one.
There are also many small satellites with flat surfaces causing faint
flashes. Such satellites can be seen steady, show some flashes times
and then become steady again. These are not really PPAS objects.
Observations per satellite
A satellite with the properties of an PPAS object gets more
interesting when more observations are available. In practice it
appears that the Kosmosrocket, Zenitrocket and Centaurrocket are most
observed. Faint satellites, because they are either small or have high
orbits, are much less observed so that there can not be drafted a
sensible evolution of the flash period.
Flashes and flares
A flash is a more or less short increase in brightness caused by the
rotation of the satellite. A flare is mainly caused by the change in
the phase angle or orientation of a satellite when the sunlight is
reflected by a rather large flat surface.
Operational Iridium cause "flares", tumbling Iridiums cause flashes.
Iridium flares are predictable, flashes are not. I suppose that flares
caused by Skymeds, Key Holes and Lacrosses can be predicted as long
their attitudes can be predicted. Almost always such a satellite will
flare under the same conditions in the same area of the sky (at nearly
the same elevation and Azimuth).
In summary:
It is recommended to follow a potential PPAS-object for at least half
of the available arc of visibility.
It is recommended to determine as many maxima as possible when a flash
period has still to be determined. The reporting of individual timings
depends on the present regularity in those times.
Last Note
All observations are scanned, but not all will be written to the PPAS
database. The less suitable observations are kept in a separate file.
Possibly this file will be made available to other observers.
Bram Dorreman,
PPAS collector
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