October 18, 1965 Electronics
[Table of Contents]
Wax nostalgic about and learn from the history of early electronics.
See articles from Electronics,
published 1930 - 1988. All copyrights hereby acknowledged.
Meteor scatter (aka
burst) communications is today largely the domain of amateur radio operators in their
ongoing attempts to set records for making long distance (DX) contacts with a minimum
amount of transmit power. When this article was written by U. California's Victor Latorre,
transcontinental fiber optic cables did not interconnect the world with high speed, phase
stable media that meets the exacting needs of precise time synchronization. Radio astronomy,
quantum physics experiments, and even stock market trading (see
Arbitrage via Microwaves)
depends on microsecond or finer timing. Mr. Latorre mentions here about using meteor
scatter communications' unique phase-stable characteristic to send synchronization signals
between scientific and navigation facilities. Of course meteor scatter has the severe
disadvantages of being unpredictable in time and place, short-lived, and varying in levels
of ionization of the upper atmosphere with attendant frequency and bandwidth accommodation.
That very unpredictability, however, in opportunity was exploited by the military to
send secure, encrypted messages across the globe.
Messages by Meteor
Meteor burst communications systems transmit secure
data over the horizon; excellent phase stability provides time synchronization with only
By Victor R. Latorre,
University of California, Davis
With a meteor trail and simple, inexpensive equipment, very high frequency signals
can be transmitted over the horizon to a point as far distant as 1,200 miles. The technique,
known as the meteor scatter mode, cannot be used to transmit real-time data because the
meteor scatter mode is not a continuous medium. The meteor trails that reflect signals
occur at discrete intervals of time, rather than continuously, and would not be suitable,
for example, in a command data link where real-time data must be transmitted without
However, for those situations where delays between data transmission can be tolerated,
a meteor scatter system is far less expensive than tropospheric and ionospheric scatter
One of the advantages of the meteor scatter mode is excellent phase stability, which
can be applied in a time distribution system that could synchronize clocks at distant
locations within about 200 nanoseconds. Such a system would be simple and yet have five
times the accuracy of the best currently available time distribution system.
Statistical distribution of signal amplitudes reflected from meteor
trails, as measured on the experimental meteor scatter link between Seattle and Bozeman,
Mont. Chart is a plot of the measured probability of reflected signal amplitudes that
will be greater than some arbitrary reference. Underdense bursts are characterized by
that part of the distribution curve whose slope varies from 0 to -1; overdense bursts
are characterized by slope from -1 to -4. The curve becomes discontinuous falling off
to a constant slope = -5.7, which indicates additional ionospheric scattering, and multiple
trails in the burst.
The meteor scatter mode depends upon signal reflection from meteor trails, a phenomenon
that has been fairly well analyzed in the past few years. It is interesting that early
investigators attributed the enhancement of vhf signals beyond the horizon to holes created
in the ionosphere by meteor particles, although it is now known that the trail created
by the particles causes the reflections.
In this article the scattering mechanism itself is analyzed, and its important features
are discussed for the system designer. The basic considerations are evaluated for a meteor
burst system design and the results are presented from an experimental system that has
been in operation for the past two years between Montana State University, in Bozeman,
and the Boeing Co., in Seattle.
Shower and Sporadic Meteors
To analyze the properties of the meteor burst propagation medium, a logical starting
point is the meteor particle itself, since it is responsible for the existence of the
scattering surface or volume of the medium. Individual meteor particles vary in radius
from about 40 microns to about 8 centimeters, and their mass varies from 10-7
gram to about a kilogram. The velocity of the particles varies between 11.3 and 72 kilometers
Millions of meteor particles enter the earth's atmosphere each day. Normally, they
are placed into two distinct categories - shower meteors, which are predictable and occasionally
quite spectacular, and sporadic meteors.
Shower meteors are concentrated in streams of well-defined orbits about the sun; they
travel in an ecliptic plane in much the same direction as the earth moves about the sun.
But only a small percentage of the total number of meteors are shower meteors. Since
the sporadic meteors occur much more frequently, they are far more important for radio
communications. Both their location and frequency of occurrence seem to be random.
The actual mechanism by which the trail of the meteor is formed is not well defined,
but a reasonable explanation of it can be offered. A fast-moving particle approaching
the earth enters a region in which there is a relatively rapid change in atmospheric
density. This region extends from about 80 to 120 kilometers above the earth's surface
and is characterized by a diffusion constant that varies from about 1 to 140 square meters
per second. (Diffusion constant, which is a function of the air density, describes the
rate at which the electrons in the meteor trail tend to disperse.)
Statistical distribution of burst durations as measured on the Seattle-Bozeman
link. Curve is a plot of the measured probability of meteor bursts occurring whose duration
is greater than an arbitrary duration.
Above this region, a meteor trail can't form because the air is too thin; below this
region, a meteor trail can't exist because the meteor is pretty much burned up due to
the heavy air density. The collision between the high-velocity particle and the air molecules
in this region produces ionization, heat, and light. Because the mass of the particle
is quite large relative to the air molecule, the velocity of the particle remains fairly
constant until it vaporizes. When the particle vaporizes it produces a thin meteor trail
that can be as long as 50 kilometers and that varies in radius between 0.5 and 4.35 meters.
Some investigators say that the trail has an outer sheath, which is indicated by the
presence of intense ultraviolet light. This sheath has a different electron density from
that of the rest of the trail. At frequencies higher than about 50 megacycles, the sheath
causes some reflection in addition to that caused by the trail itself; at lower frequencies,
the sheath is essentially transparent to incident electromagnetic radiation.
Most investigators have categorized the meteor trails into four groups: underdense,
underdense-distorted, overdense, and overdense-distorted trails. The first two categories
are characteristic of low-density trails (less than 1014 electrons/meter),
whose electrons act as individual in-phase scatterers, each one affecting the signal
equally. The underdense and underdense-distorted trails are also distinguished from the
others because signals reflected from them have a fast rise time. The difference between
the underdense and under dense-distorted trails is the irregular shape of the latter,
which is caused by wind shear. Because of its irregular shape, the underdense-distorted
trail causes modulations during the decay interval of the reflected signals.
Overdense trails have a higher concentration of electrons (i.e., greater than 1014
electrons/ meter). Signals reflected from these trails are characterized by a relatively
slow rise time and a fairly constant amplitude. Because it's more dense, the overdense-distorted
trail is broken into several distinct blobs, or segments, when wind shear is sufficient.
Thus, the amplitude of a signal reflected from such a trail will fluctuate somewhat.
For the case where long signal wavelengths (low frequencies) are to be considered,
the trail is assumed to be a long, thin cylinder, since the wavelength is longer than
the radius of the trail, and the duration of the trail is much greater than its formation
time. For short wavelengths, however, the wavelength is equal to or smaller than the
radius of the trail. Therefore, the trail is essentially always in a transient condition,
and must be considered as having the shape of a paraboloid.
The pertinent mathematical expressions for the various burst modes will not be derived
here. Instead, the physical phenomena will be explained qualitatively.
Measured statistical distribution of period between bursts.
Perhaps the most important point to realize is that the received power in a meteor
burst system is a direct function of the wavelength raised to the nth power, where n
varies between 3 and 6, depending on many factors, including frequency and the shape
of the trail. Because of this, meteor scatter systems operate in the lower portions of
the vhf frequency band, where the wavelengths are longer. Research is presently under
way at the University of California to determine experimentally the practical upper frequency
Another consideration is that reflections from the nondistorted underdense and overdense
trails are specular. That is, the angle of incidence at which the signals arrive at the
trail is equal to the angle of reflection. This implies that meteor scatter links are
somewhat directional in nature, and therefore can provide some degree of privacy from
unauthorized or unintended interception of messages.
Since the meteor burst channel is not continuous, it is necessary to describe it statistically.
In general, the statistical fluctuations are divided into two distinct parts - short-term
and long-term variations. Representative distributions obtained last year on the meteor
burst communications link between Seattle and Bozeman are shown in charts. The chart
on the preceding page shows the measured statistical distribution of reflected signal
amplitudes greater than any given arbitrary reflected amplitude. From this chart, it
can be seen that all of the reflected signals will have an amplitude greater than approximately
0.6 A0 while only about 10% will be greater than about 3.0 A0,
where A0 is an arbitrary reference level.
The chart at the top of this page shows the measured statistical distribution of the
duration of meteor bursts as a function of time. Of the burst durations measured, 100%
lasted more than about 0.15 seconds, while only 2% lasted for as long as 1.5 seconds.
Burst durations theoretically have a Poisson distribution, which characterizes purely
random events. However, the measured curve is slightly different from the expected distribution
for short burst durations; this is due primarily to the presence of distorted overdense
The measured statistical distribution of time between bursts is shown in the other
chart on this page. Here, it can be seen that the minimum time between bursts was one
second, and that only about 5% of the intervals between bursts were greater than 100
seconds. Although meteor bursts occur randomly, the measured data again deviates from
theory, due to distorted overdense bursts.
The majority of meteor burst channels operate in the vhf range of the spectrum (30
to 300 megacycles), where signals are subject to absorption in the D-layer in the same
manner as signals that depend on normal ionospheric reflections. At night, this absorption
is generally negligible for vhf frequencies. At about midday, however, signals in this
frequency range may suffer up to 10 decibels of attenuation. And absorption increases
during ionospheric disturbances, such as solar flares or auroral activity caused by magnetic
storms, affecting meteor scatter signals up to 100 megacycles.
In addition to susceptibility to absorption in the ionosphere, other variations in
signal can be caused by: geographical location of both the transmitter and receiver;
the actual path length between the transmitter, the meteor trail and the receiver; and
the antenna patterns employed. The optimum antenna pattern for the burst channel appears
to be a split-beam pattern. Research is in progress, however, on self-adaptive antennas
whose patterns can be varied in accordance with diurnal variations in the ionosphere.
Other types of diurnal and seasonal variations must also be considered. For example,
there are diurnal variations in meteor arrival rate (the maximum occur at around sunrise
and the minimum at sunset), meteor velocity, and effective radiants (position in the
sky of the meteor trails); all of which affect system performance. The major seasonal
variation seems to be in the meteor arrival rate. The maximum number of bursts occur
in August; the minimum in February.
Typical Meteor Scatter System
Block diagram of system used to measure phase stability of the meteor
In a meteor scatter communications network, one station is a master, or base, station
and the others are slave, or remote, stations. The most obvious requirement of the typical
meteor scatter system is some method to inform a slave station that a usable meteor trail
is available. A slave station will remain silent until it receives an individual and
distinct interrogation, or pilot tone, from the master station. When the pilot tone exceeds
a preset threshold, the slave station transmits any information it may have at that time.
When the pilot tone falls below the threshold, this signifies that the trail has decayed,
and transmission ceases. In a system with two or more stations capable of transmitting
information to each other, each station transmits a pilot tone, which, when received
by another, initi-ates information transmission.
There are several possible methods for alerting the system to the presence of meteors,
but all have the same basic purpose - to inform other stations in the network that satisfactory
communication is possible. This closed-loop feature is characteristic of all meteor scatter
The preceding discussion implies the existence of another characteristic peculiar
to meteor burst systems; namely, the ability to make decisions.
Meteor scatter systems are limited by the kind of information that can be transferred.
In the case of data transmission, for example, only non-real-time data can be transmitted,
since the channel is not continuously available. Thus, this propagation mode would be
impractical for a command-control system because it sometimes takes as long as 30 minutes
for a suitable meteor trail to form. Such a long delay obviously could be most disastrous
for the quick-response requirements of modern military systems.
Although the meteor burst system between the Boeing Co. in Seattle and the Electronics
Research Laboratory at Montana State University in Bozeman is experimental, a discussion
of it nevertheless illustrates the techniques and the practical problems encountered
with operational systems.
The Boeing-ERL meteor scatter link, which was established in the early part of 1960,
spans a linear distance of some 550 miles. Most of the initial effort with this channel
was devoted to determining the basic propagation path loss, the channel's duty cycle
(ratio of available transmit time to dead time) as a function of time of day and as a
function of receiver threshold, the cumulative burstwidth distributions, and the channel's
reciprocity conditions (offset between the master and slave stations' transmit frequencies).
Subsequent tests were performed using frequency modulation and correlation detection
Phase Stability and Time Synchronization
Waveform envelopes of signals received from the various types of meteor
trails are shown in recordings presented at the Navy Research and Development Clinic,
Bozeman, Mont., July, 1964.
In 1962, a series of experiments produced statistical information concerning the phase
stability of signals reflected from the meteor trails. The results of these phase stability
tests were very encouraging and formed the basis for the design of an experimental instantaneous
time-synchronization system between Bozeman and Seattle.
In such a system, a pulse is transmitted from one site to the other at an accurately
known time according to the clock. The operator at the receiving station is informed
via telephone as to the precise time the pulse will be transmitted, and he sets his clock
accordingly. The error between the two clocks is only that caused by the delay time in
the equipment, since the delay time due to the data-transmission path can be measured
and taken into consideration when the clocks are synchronized. Even though it was rather
crude, initially, the system was still capable of synchronizing clocks at the two locations
within 15 microseconds.
A block diagram of the equipment used in the phase stability experiments is shown
At the Seattle terminal, a 46.548-megacycle signal was transmitted. When a suitable
meteor trail occurred, the signal was received at Bozeman. By examining the waveform
envelope of the received signal, it was possible to identify the specific propagation
mechanism; that is, whether the propagation was indeed by meteor (and the specific type
of meteor trail, or whether it was by sporadic-E, a phenomenon characterized by occasional
lowering of the E-layer of the ionosphere, or by other ionospheric effects. Only those
signals reflected from meteor trails were used in the phase stability analysis. In addition
to the envelope of the demodulated signal, the quadrature signals, sin 4Φ(t) and
cos 4Φ(t), which describe the phase character-istics of the signal, were recorded
on a multiple channel recorder.
The test data was analyzed on an IBM 1620 computer. From an analysis of the phase
information for both the underdense and overdense trails, it was determined that phase
shift in meteor burst propagation is very nearly a linear function of time, and is so
small that a time distribution system using the meteor scatter mode would be capable
of operating with timing errors as small as 20 nanoseconds. This becomes clear from the
data for a typical trail of 300 milliseconds duration, during which the phase shift varied
at a rate of 20 radians per second. This results in a total change in time delay of about
20 nanoseconds, which is the ultimate timing potential of the medium.
It is interesting to observe that the degree of expected accuracy using this mode
is considerably greater than that obtained with conventional high-frequency systems,
such as the National Bureau of Standards' WWV time and frequency distribution system,
which transmits standard frequencies at 10 and 20 Mc, and pulses at accurately measured
intervals according to the clock. But since the WWV system relies on ionospheric reflection
of h-f signals, where it is difficult to precisely determine the path length, it is able
to provide timing information within only a millisecond.
Meteor scatter time-synchronization systems are potentially equal to or greater than
the best currently available system - the loran-C, which is capable of achieving time
synchronization to within about a microsecond.
Pulses received via meteor scatter over the Bozeman-Seattle link.
Top pulse was reflected by an underdense burst, and pulse at bottom by an overdense burst.
Phase of received pulses indicates relatively stable path lengths.
The application of correlation techniques to the detection of signals transmitted
via the meteor scatter mode is another important tool for the communications system designer.
The results of an experiment establish that the usable duration of meteor bursts can
be extended with correlation detection techniques and a delay line matched filter.
Besides effectively increasing the signal-to-noise ratio and increasing usable burst
time, correlation techniques may be applied in systems that require protection from intentional
jamming or from unwanted interception of messages.
G.W. Pichard, "A Note on the Relation of Meteor Showers and Radio Reception," Proc.
IRE, Vol. 19, No.7, July, 1931.
Von R. Eschleman, "The Mechanism of Radio Reflections for Meteoric Ionization," Tech.
Report No. 49, Electronics Research Laboratory, Stanford University, July 15, 1952.
D.M. Reyonds, "Antennas for Meteor-Burst Communication Systems," Tech. Report No.2,
Electronics Research Laboratory, Montana State University, January, 1959.
J.D. Belenski, "Meteor Burst Communication Research Program," D2-20788, The Boeing
Co., Seattle, Wash.
J.D. Belenski, "The Application of Correlation Techniques to Meteor Burst Communications,"
1962 IRE Wescon Proceedings.
D.K. Weaver, P.C. Edwards, A.E. Bradley, and D.N. March, "Final Report, Meteor Burst
Time Synchronization Experiments," ERL Tech. Report, Montana State University, August,
George Sugar, "Radio Propagation by Reflection from Meteor Trails," Proc. of IEEE,
Vol. 52, No.2, pp. 116-136, February, 1964.
V.R. Latorre and G.L. Johnson, "Time Synchronization Techniques," IEEE International
Convention Proceedings, March, 1964.
Hewlett-Packard Co. Application Note No. 52, "Frequency and Time Standards," Hewlett-Packard
Co., Palo Alto, Calif., 1962.
V.R. Latorre, "The Phase Stability of uhf Signals Reflected From Meteor Trails," IEEE
Transactions on Antennas and Propagation, July, 1965.
Victor R. Latorre is an assistant professor at the University of California, Davis.
His current research project involves remotely measuring the temperature changes in a
Posted November 6, 2018