April 1953 QST
Table of Contents
Wax nostalgic about and learn from the history of early electronics. See articles
QST, published December 1915 - present. All copyrights hereby acknowledged.
Meteor scatter communications is an excellent example of where hobbyists
- in this case amateur radio operators - have contributed mightily
to technology. It could be argued that a big part of the reason
for such occasions is that many people involved in science type
hobbies are employed professionally in a similar capacity, and their
extracurricular activities are a natural extension of what pays
for the pastimes. It seems amazing to me that meteor scatter as
a means of achieving upper atmosphere reflections of radio signals
went undiscovered until 1953, but evidently that is the case. Meteor
scatter is a very popular form of amateur radio challenge these
days, with much activity when the bigger meteor showers are underway.
Prior to 1953, meteor shower study was the sole domain of astronomers.
A Newly-Discovered Means for Extended-Range Communication in
the 15- and 20-Meter Bands
By Oswald G. Villard, Jr.,* W6QYT, and Allen M. Peterson,** W6POH
Although you might not suspect it, in view of this past winter's
experience, the 14-Mc. band is never completely "dead." This article
describes a newly-discovered type of propagation that is always
present, for which the optimum communication distance is of the
order of 800 miles. It has gone undetected for many years because
it is usually masked by other forms of propagation and requires
first-rate equipment for its exploitation - equipment which, however,
is not at all unusual.
Fig. 1 - Point-to-point communication by
ground scattering after layer reflection over the great circle
path has failed.
Want to keep a schedule with someone seven or eight hundred miles
away after the 20-meter band has "gone dead" at night? Thanks to
a recent discovery in which amateurs have played a part, it is now
possible to do this without shifting down to a lower frequency and
battling the usual QRM. By taking advantage of a new type of radio
propagation known as "meteor scatter," two stations can communicate
far beyond ground-wave range all night long and have the band essentially
Furthermore, QSOs can be carried on by this means all day long
too, even though the station at the other end is well inside the
skip zone at all times. And best of all, here is one type of reasonably
long-distance radio transmission which promises not to be subject
to fadeouts, ionospheric storms, and all the other uncertainties
which plague the regular ionospheric layers.
Schedules using this type of propagation should be 100 per cent
The catch? Yes, there is one, for new types of propagation such
as this don't keep themselves hidden all these years without good
reason. The disadvantage is that at amateur power levels, it is
necessary to be content with a fairly weak signal, and one which
fades fairly rapidly between very wide limits. The signal is on
the average too weak for satisfactory telephony, but is adequate
for c.w. It makes occasional brief dips into the noise, but promptly
comes back again. It will often rise twenty or thirty decibels above
the noise, for as much as five or ten seconds at a time. The astonishing
part of the matter is that the signal - at least some signal - is
there substantially all of the time, even when the band, by every
normal criterion, should be completely dead!
What does one need to take advantage of this form of transmission?
Nothing more than an efficient station, and some knowledge of what
to expect. Briefly, the explanation of the signal - at least in
the vicinity of 20 meters - is forward scattering from ionization
trails left behind by the myriads of tiny meteors which pepper the
E region of the ionosphere at all times. Hence the maximum range
for this form of transmission is essentially that for normal one-hop
E-layer transmission, or 1500 miles. For reasons which will be brought
out later a good transmission distance in practice is about half
this value, or around 800 miles.
Visible meteors during a shower: a two-second
exposure during the great Draconid display of October, 1946.
Lines drawn through individual meteor trails (inside circles)
intersect a t a common point known as the shower radiant. Thousands
of meteors too small to be seen - but producing radio reflections
- strike the E region of the ionosphere at all times.
In view of .the low height of the E region - roughly 70 miles
- the vertical angle of take-off even for the shorter distance is
quite low - of the order of 5 or 6 degrees. Thus a good site is
a requirement: one which does not have nearby mountains or apartment
houses screening off low-angle radiation in the desired direction
of communication. An antenna well up in the air, a sensitive receiver,
and a location reasonably free of man-made QRN are also important.
If this sounds formidable, remember that these are no more than
the requirements for reasonably good DX results. A "full gallon"
is not essential - two or three hundred watts will do, although
the more the merrier. It follows that many thousands of operators
throughout the country should be able to take advantage of this
new type of extended-range transmission.
How does this type differ from those to which we are already
accustomed? The story, briefly, is as follows. Consider two cities,
say New York and Chicago, spaced roughly 800 miles apart. (Any other
two cities, spaced the same distance, would do equally well.) Until
fairly recently, it was thought that communication between these
two communities at frequencies below 30 megacycles could only be
conducted when the "regular" layers - F, E and sporadic-E - were
sufficiently ionized to reflect a signal from one city to another.
The distance involved is much too great for ground- or space-wave
communication, and it is also too great for the extension of ground-wave
range caused by tropospheric bending, even if that effect were important
at the lower frequencies.
Not long ago, however, another mechanism for getting a signal
from New York to Chicago in the absence of direct reflection from
an overhead layer has come to be understood. This is the indirect
bounce by back-scattering from the ground. When the skip is so long
that Chicago cannot hear New York directly, both Chicago and New
York may still be able to hear Miami, Florida. If the New York transmitter
uses a beam directed southward, it will lay down a strong signal
all over the state of Florida and the Atlantic Ocean on one side,
and the Gulf of Mexico on the other. A small but detectable part
of this signal will be scattered in all directions by water waves
in the Gulf and the Atlantic, by houses and trees on the land, and
so forth. If the Chicago station also uses a beam directed at Florida,
it will be able to pick up scattered components of the signal originating
in New York, and the two stations will be able to communicate via
Florida, as in Fig. 1. The indirect signal will be much weaker than
a direct bounce over the great circle path, and will have a hollow,
fluttery sound not unlike that of a DX station, but it will be well
above the noise level and perfectly readable for both voice and
code. (See description on page 74 of the 1953 ARRL Handbook.)
This type of scattering has been observed quite regularly by
amateurs interested in 50-megacycle DX, and has been given a variety
of names including "rebound scattering" and "reflected skip." The
authors, who prefer to call it "ground scattering" since this seems
to be the more descriptive term, have shown some photographs illustrating
it in their article on scatter-sounding in the March, 1952, QST.1
Those photographs show scatter echoes received at the same spot
from which the initial signal had been transmitted; it should be
understood, of course, that ground scatter echoes from a given transmitter
can also be heard at other locations inside the skip zone surrounding
that transmitter. Thus a scatter-sounder in New York would be heard
in Chicago under conditions of Fig. 1.
Fig. 2 - "Life history" of the most commonly-encountered
type of radio echo from a meteor trail. Shape is the same for
either backward or forward or forward reflection (see Fig. 3).
Now about the only remaining way to get a signal from New York
to Chicago - if we leave out the possibility of bouncing a signal
from one place to the other via exceptionally strong auroral ionization
to the north - is by means of reflection from a meteor column formed
somewhere in the vicinity of the great-circle path.
It has been thought until recently that these meteor reflections
were always of short duration, and of no practical value for communication
except perhaps during an exceptionally strong meteor shower such
as the great one of October, 1946. This impression has stemmed from
the fact that most observations of meteors have been conducted with
transmitter and receiver at one location, which is clearly the most
convenient experimental arrangement. Under these conditions relatively
isolated reflections, or signal bursts, are obtained.
Recent advances in understanding the nature of these reflections,
however, have led to some interesting conclusions.2 It
is now known that there are in general two types of meteor echoes.
About 10 per cent of the total detected under ordinary conditions
have very long durations (ten seconds to ten minutes), strong fading
fluctuations, and an irregular and unpredictable "life history."
Their behavior is not yet well understood. The other 90 per cent
of the echoes have a surprisingly regular behavior, being characterized
by a rapid rise to peak amplitude, followed by a decay of exponential
form as shown in Fig. 2. Since the decay is exponential, it is convenient
to define duration as the time interval between the peak and the
time at which the echo strength has dropped to roughly one-third
the peak strength. Thus this "duration" is analogous to the time
constant of a condenser discharging through a resistor.
Now it turns out that the height of the peak can be predicted quite
accurately for this type of echo, and varies inversely as the three-halves
power of frequency, assuming all other factors to be held constant.
Thus, an echo having a peak of unit strength at 14 megacycles will
be less than one-third as strong at 28 megacycles. Furthermore,
the duration of this type of echo has been found to vary inversely
as the frequency squared. Thus if an echo lasts for one second at
14 megacycles, the same echo would last only one-fourth of a second
at 28 megacycles.
Lastly - and here is the payoff - it has been discovered that
the duration of a meteor echo at any given frequency, increases
very rapidly when transmitter and receiver are separated by several
hundred miles. This increase factor is proportional to the square
of the secant of the forward-scattering angle 2φ in Fig. 3.
It works out that for a transmitter-to-receiver distance of 800
miles, the remote reflection produced by a meteor column formed
over the midpoint of the path will have a duration more than twenty
times that which it would have if the receiver were adjacent to
Thus, by going to a relatively low frequency, such as 14 megacycles,
we get stronger echoes, and ones which have longer duration. Then,
by changing from a backward to a forward path, we get another increase
in echo duration - and quite a large one at that.
For some years, back-reflection experiments have shown that a
truly astonishing number of meteor echoes can be received even with
relatively low-power equipment. Measurements at Stanford University3
using equipment and power levels substantially equivalent to that
employed in a 1947 amateur experiment4 have shown that
at a frequency of 23.1 megacycles, during the early morning hours,
several thousand meteor reflections per hour can be detected. This
is at a rate of nearly one per second. The average duration of each
echo at this frequency may be taken (conservatively) to be one-quarter
of a second. This implies that on the average, meteor echoes are
present for nearly one-quarter of the total time.
If now the frequency is lowered to 14 megacycles, and an 800-mile
forward bounce is considered, the average duration of the meteor
reflections is multiplied by a factor of roughly 50 times! Thus,
if one echo occurs each second, and each echo lasts on the average
twelve seconds, there will clearly be more than enough meteors present
to guarantee a continuous signal by meteor reflections alone.
This picture is, of course, greatly oversimplified, although
it does represent a fair approximation. For example, the area of
the sky from which meteor echoes are obtained for overhead reflection
is not the same as it is for distant reflection. However, when all
the details are worked out, to the best of present knowledge, there
will be at 14 megacycles enough meteor reflections on the average
at all times of the day and year to guarantee a continuous signal
between two amateur stations separated by 800 miles and having moderate
transmitter powers, good locations, and simple beam antennas.
Fig. 3 - Illustrating backward and forward
reflection (or "scattering") from a meteor trail.
This effect was turned up accidentally by the authors during
the course of the W6YX scatter-sounding experiment,1
which consisted of a demonstration that when echoes from a particular
area appear on the scatter-sounder, strong signals can actually
be heard from amateur stations located in that area. The converse,
of course, was also investigated at the same time. In other words,
the authors were just as eager to be able to show that when no echoes
appeared from a given area, amateur signals could not be received
from that area, either. This proved to be a tricky proposition,
as was pointed out, because as long as any echoes appear anywhere
on the indicator, it is always possible for a station in a supposedly
"dead" region to be heard weakly by ground scattering via the area
from which the echoes are coming.
It was decided that the most convincing test would be to wait
until late on a night after all F, E, and sporadic-E activity had
disappeared, and the indicator showed no echoes at all. Such nights
are actually few and far between on the West Coast during the months
of November and December. When one was at last found, a 'phone call
was put through to Rod Beaudette, W7FXI, at Spokane, Washington,
about 750 miles airline from Palo Alto. Rod, a Stanford graduate
who had participated in the early meteor experiments at W6YX, has
500 watts on the air feeding a 3-element beam perched 30 feet above
the roof of his house in suburban Spokane. At his location the ground
slopes off toward the south (the direction to Palo Alto), and there
are no intervening mountains to block off the horizon. Aside from
this, Rod's location might be termed average, having the usual number
of impedimenta in the form of light lines, neighboring houses, etc.
W6YX's location (at least for the north and south directions) is
better than average; the station is located atop a small hill one
or two hundred feet above the floor of the valley containing San
Fig. 4. - Forward and back-reflected meteor
echoes at 14 megacycles. When these records were made (late
at night), no layer propagation of any kind could be shown to
While Rod, wakened out of a sound sleep, good-naturedly went
down into his basement to turn on the rig, we at Palo Alto thoroughly
crossed our fingers and patrolled back and forth across an absolutely
dead band. Suddenly, a signal! Could that drowsy-sounding voice
be Rod's? In our excitement, we placed another 'phone call to verify
it. There could be no doubt. Again we checked the amateur scatter-sounder.
No sign of any echoes. No sporadic-E at all, and F-reflections had
died out hours earlier. Yet there was W7FXI: at times unreadable
on voice - at others, easily readable and well above the noise.
During the dips, his carrier could always be copied by switching
on the b.f.o. C. w. reception was quite satisfactory without the
crystal filter, and much improved, of course, with it.
These tests were repeated as often as suitable conditions could
be found, with similar results on each occasion. The signal was
definitely always there, when by all rights nothing should be heard.
Its characteristics at once suggested the meteor-scatter explanation,
and instantaneous field-intensity recordings strengthened this impression.
In addition to bursts, nose whistles and "body Dopplers" could easily
be seen superimposed on the continually-fading, but almost-always-present
background. As is to be expected, the duration of the big bursts
over this long path was, on the average, far greater than anything
we had experienced during the course of local tests. Fig. 4 illustrates
this effect by showing the comparison between a recording of backward-reflected
meteor echoes obtained locally, and a similar recording of forward-reflected
meteor echoes over a 750-mile path. Echo overlapping in the latter
case prevents accurate determination of individual echo durations
but the increased average duration is clear.
In the thought that there might be something magic about the
path to Spokane, similar tests were carried out with W7PZ in Tucson,
Arizona - about 750 miles away in a south-easterly direction. Ben
has a three-element beam, about 300 watts, and a location outside
Tucson on flat land not far from the airport. His signals were heard
just as consistently as W7FXI's in Palo Alto.
In addition, W6HJT in San Marino - only 300 miles away and nearly
south from Palo Alto - also put in a very strong signal with a steady
background underlying the meteor bursts.
Attempts to increase the frequency or the distance met with less
success, however. Transmissions to and from Tucson on 10 meters
resulted in a signal audible only during well separated bursts,
with no sign of a background between.
On one occasion, W0PRZ in Aberdeen, South Dakota, was asked to
listen for the 20-meter W6YX signal. His distance is near the maximum
for one-hop E-layer reflection: about 1400 miles. During the course
of a 15-minute transmission, only one or two distinct bursts were
heard. His antenna, location and equipment are top-flight, as his
DX record shows, so the conclusion seems to be that at extreme range
the number of meteors which can produce a signal over the path (they
have to be just about exactly over the midpoint) becomes so small
that a continuous background is not supported. Also, the angle of
take-off becomes so low (down around one degree) that antennas of
practicable height are quite inefficient. The effect of varying
transmitter-receiver distance, with frequency and power constant,
is shown in Fig. 5.
Fig. 5 - Effect of distance on meteor echo behavior,
for a given frequency and power.
Relationship to 50-Mc. Scattering
The theoretical investigations which followed these ham experiments
confirm the expectation that meteors alone can support the entire
signal.5 ,6 However, the possibility that other factors
may be involved can by no means be ruled out. There has recently
been published an account of another new form of propagation, in
many respects resembling that discussed in this article, which is
effective at frequencies of the order of 50 megacycles and at very
high power levels.7 It is suggested that this propagation
may be explained as forward-scattering from irregularities such
as might be caused by turbulence in the E region of the ionosphere.
Meteors are cited as playing an important part. The observed signal,
however, has certain characteristics for which meteors would almost
certainly not be responsible.
These characteristics, unhappily, are not easy to study at 15
megacycles. It is not yet known to what extent, if any, the 15-
and 50- megacycle signals arc caused by the .same agency. The situation
as of December, 1952, may be summarized in the following way. At
the lower frequency, theory indicates that meteors alone should
easily account for the observed signal. Nothing in the experimental
evidence thus far disagrees with this conclusion. At 50 megacycles,
however, the theory -- based on present knowledge of meteor echo
behavior-predicts that they alone will not be sufficient to account
for what is observed. It appears that other factors must be sought.
The unscrambling of the several factors which may contribute
to the signal observed at the two frequencies will be an exciting
and challenging job. One of the first tasks will be to gain as much
experience with these new types of propagation as possible. Here
the amateurs, with their wide geographical distribution, and their
willingness to experiment at all hours of the day and night, are
in a position to make a real contribution. It is obvious that any
means for making the 20-meter band work around the clock (at least
for 800-mile QSOs!) is going to be important as crowding on the
lower frequencies increases.
Furthermore, the invulnerability of meteors to ionospheric storms
is another important point: a weak, but really reliable circuit
may, during emergencies be worth much more than one which could
fade out at the crucial moment.
The strength of the meteor-scatter signal, and hence its usefulness
in ham communication, will depend on the efficiency of the stations
involved. The antenna system is very important, and should be designed
to concentrate power where the most meteor scatter is taking place
- namely, in the E region over the midpoint of the great circle
path. For an 800-mile path, the main lobe of the pattern in the
vertical plane should ideally be at 6 degrees above the horizontal.
At 20 meters a dipole should be 165 feet over perfectly-conducting
earth, for the lowest lobe to be at 6 degrees! In practice, whatever
arrangement affords the highest gain consistent with a low vertical
angle will be best.
Almost any good station will be able to take advantage of meteor-scatter
transmission at 20 meters. At 15 meters, however, it is probable
that only the kilowatt boys will be able to transmit a usable background
signal over the path. Stations having good locations and rotary
beams (or preferably rhombics), and willing to use maximum receiver
crystal selectivity, will no doubt be able to make a go of it. (As
frequency goes up, echo strengths and durations go down, but since
the echoes are exponential, the net loss can be overcome by an increase
in power or receiver sensitivity.) In any case, a c.w. clipper or
limiter will be very worthwhile. Otherwise, when gain is advanced
enough to copy weak passages, meteor bursts tend to be deafening.
Note that the preceding remarks on signal strength apply to those
times of day when meteor scatter is the only form of transmission
taking place. Actually, for much of any given day the signal will
be well above the purely meteor level. Any sporadic-E activity,
for example, will enormously increase the strength of the received
field. (During one memorable test with W7PZ, sporadic-E set in and
within a minute or so transformed his randomly-fading S1 meteor-scatter
transmission into a rock-solid S9 signal with a very slow, almost
perfectly sinusoidal amplitude variation.) Whenever any F-layer
transmission is in at all, of course, there will be a strong ground
back-scatter component present along with the meteor-scatter.
Thus the timetable for 14-Mc. transmission over a New York-Chicago
path, during the winter months of the year, might run something
like the following:
8 P.M. - 7 A.M. meteor scatter alone weak signal
7 A.M. - 9 A.M. meteor plus F-layer ground scatter medium signal
9 A.M. - 5 P.M. direct F-layer transmission very strong signal
5 P.M. - 8 P.M. meteor plus F-layer ground scatter medium signal
(Sporadic E, which might come in at any hour of the day or night,
would provide a strong signal directly, or a weaker signal via ground
The reader is probably wondering, at this point, why meteor-scatter
propagation has not previously been noticed on transmission from
commercial stations. The answer is that it probably has, but simply
was not identified as such. Most broadcast or commercial stations
are in the habit of signing off after F-layer transmission fails,
so listeners seldom get much of an opportunity to hear meteor scatter.
Once in a while a station, transmitting according to a prearranged
schedule, will stay on the air after its frequency has "gone dead."
This has happened, for example, in the case of a 17-megacycle short-wave
broadcasting station roughly two hundred miles south of Palo Alto.
Their beam points right at Stanford, on its way to the Orient, and
what is believed to be meteor scatter has been heard on many occasions.
WWV's transmissions on 15 and 20 megacycles, of course, provide
a wonderful opportunity to check for meteor scatter, and hams living
within a radius of 1000 miles of Beltsville, Maryland, are urged
to tune in on WWV and satisfy themselves that the 20-meter band
really doesn't go entirely dead, at night, after all!
The authors are indebted to W6VUW, W6UGL, W6LLK, W6AOF and other
members of the Stanford Radio Club for assistance during the tests.
The help of Larry and Clayte at W7TMK is also appreciated. The loan
of recording equipment belonging to a joint-Service-sponsored research
project is gratefully acknowledged. The photograph of meteors during
a shower was taken by L. A. Manning, W6QHJ.
* Trustee, W6YX; Dept. of Electrical Engineering, Stanford University,
** Radio Propagation Laboratory, Stanford University, Stanford,
1 O. G. Villard, jr., and A. M. Peterson, "Instantaneous Prediction
of Radio Transmission Paths," QST, Vol. 36, No.3, pp. 11-20, March,
2 Von R. Eshleman, "The Mechanism of Radio Reflections from Meteoric
Ionization," Technical Report No. 49. Electronics Research Laboratory,
Stanford University, Stanford, Calif., July 15, 1952.
3 L. A. Manning, O. G. Villard, jr., and A. M. Peterson, "Radio
Doppler Investigation of Meteoric Heights and Velocities," Journal
of Applied Physics, Vol. 20, No.5, pp. 475-479, May, 1949.
4 O. G. Villard, jr., "Meteor Detection by Amateur Radio," QST,
Vol. 31, No.7, pp. 13-18, July, 1947.
5 O.G. Villard, jr., A. M. Peterson, et al., "Extended-Range
Radio Transmission by Oblique Reflection from Meteric Meteoric Ionization,"
Journal of Geophysical Research, March, 1953 (in press).
6 Von R. Eshleman and L. A. Manning, "Radio Communication by
Scattering from Meteoric Ionization," Technical Report No. 57, Electronics
Research Laboratory, Stanford University, Stanford, Calif., December
7 D. K. Bailey, et al., "A New Kind of Radio Propagation at Very
High Frequencies Observable over Long Distances," Physical Review,
Vol. 86, pp. 141-145, April 15, 1952.
Posted April 11, 2016