International Ursigram
andWorld Days Service
I.U.W.D.S.

Synoptic Codesfor
Solar and Geophysical Data
Second Revised Edition
1969

Published by the IUWDSSecretariat,Boulder, Colorado

with the financialassistance of UNESCO

International

Ursigram

and
World

Days

Service

I.U.W.D.S.

Synoptic Codesfor
Solar and GeophysicalSecondRevised

Data

Edition1969

Additional copies may be obtained from one of the following addresses:
P. Simon, Ursigrammes

Observatoire, 92 Meudon, France

Miss J. V. Lincoln, Deputy Secretary, IUWDS Steering Committee
Environmental Science Services Administration
Boulder, Colorado, 80302 U.S.A.
Published for the International Council of Scientific Unions with thefinancial assistance of Unesco (Unesco subvention‑‑1968‑DC/2.1/414/26'

INDEX
Page
PART A GENERALINFORMATION

I. Introduction A.
H. Shapley 5
II. Some Commentson the Forecastingof
Solar Activity P.
Simon 7
III. Scientific
Information
Neededfor Radio B. Beckmann 17
Propagation
Forecasting
PART B ALERTS

AND COMBINEDMESSAGES

I. Alert Messagesfor IUWDS by RegionalWarningCenters 22
1.1 AdvanceAlerts:
ADALERT 22
II. Alert Messagesfor WorldwideDissemination 24
II.1 Worldwide Alerts:
GEOALERT 24
WMO distribution 25
Broadcastsby WWV/H 25
Other Broadcasts:
France 27
F. R. of Germany 2
India 27
Japan
U.S.S.R27 27

7III. Advice from RWC to World WarningAgency 28
III.l Advice Message:
ADV― 28
IV. Combined Solar‑GeophysicalData and Forecasts 30(for remoteregionsor generalusers)
IV.1 General Data and Forecast
Message:
GE0S0L 30
PART C DATA

CODES

I. Solar Optical,X‑ray and particleObservations 38
1.1 Sunspots
Code 1 :Code 32 ::Code

USSPS 38USSPR
USSPI 3845

1.2 Solar Flares
Code 1 :Code
Code 23 ::UFLAH 5UPATPUPATV 557
99

1.3 Calcium Plages and Centers of
Act ivity
Code 1 :UPLAK

1.4 Solar Corona
Code 1 :UCORE

1.5 Solar X‑rays
Code 1 :USOXO

1.6 Solar Particle Events
Code 1 :UPART

1.7 Solar Wind Parameters
Code 1 :USOLWII. Solar

Radio Observations

11.1 Flux Measurements on
Discrete Frequencies
Code 1 :URANO

11.2 Spectrographic Observations
Code 1 :URANZ

11.3 Interferometric Observations
Code 1 :Code 2 :

URALE
URALS

III. Ionospheric Observations
III.l Critical Frequencies
Code 1
Code 2
Code 3

UFOFI
UFOFO
UFOFU

III.2 Sudden Ionospheric Disturbances
Code 1
III.3 Ionospheric Absorption
Code 1
IV. Geomagnetic and Auroral Activity
IV. 1 Geomagnetic Activity
Code 1
IV.2 Auroral Observations
Code 1
V. Cosmic

Rays
V.l Daily Cosmic Ray Data
Code 1

UCOSE

96

Pagt
VI. Specialized networkcodes
VI.I Radio propagationforecasts
Code I :Code
Code 23 ::FORDA 100FORWE
102
AD ‑‑ 104

VI.2 Radio propagationindices
Code 21 ::Code

PROPO 10105
PQA‑‑

VI.3 Detailed ionospheric
data
Code 1 :ION‑ 108

VI.4 SPARMO balloonmeasurements
Code 1 :UCOSD 111

PART D LISTS

7OF STATIONINDICATORS 113

I. Observing stationsin numericalorder 113
II. Observing stationsin alphabeticalorder 119
PART E DETAILSOF PLAN FOR RAPID COMMUNICATIONS

I. Description of Arrangements
for Rapid Interchange 121
II. Details of Regionaland AssociateRegional
WarningCenters 124
11.1 RWC ‑ Boulder(WWA) 124
11.2 RWC ‑ Paris 126
11.3 RWC ‑ Darmstadt 128
11.4 RWC ‑ NERA 130
11.5 RWC ‑ Moscow 132
11.6 RWC ‑ Kokubunji 134
11.7 RWC ‑ Sydney 136
11.8 ARWC ‑ Stockholm 138
11.9 ARWC ‑ Prague 13
11.10
Delhi141140
11.11 ARWC
ARWC‑‑ New
Irkutsk

9

III. National WarningContactsand Addresses 142(in alphabeticalorder by country)
PART F IUWDSPART G ALPHABETICAL

AND ITS PROGRAMS 149
INDEX OF CODES 15

7

I'AR!'A

GENERAL INFORMATION

I. Introduction
This booklet gives all information needed in the rapid collection,interchange and distribution of solar and geophysical data, alerts andforecasts. It is intended for use by observing stations, by warning or
forecast centers and by institutions or individual scientists making useof the services of the centers. This interchange activity is carriedout under the auspices of the International Ursigram and World Days
Service (IUWDS); Part F of this booklet gives a description of the fullIUWDS program.
The data are communicated by telegrams (or in some cases by radio
broadcast) which are sometimes referred to as Ursigrams (after URSI ‑‑Union Radio Scientifique Internationale). For clarity and economy, thedata reports are usually cast into 5‑character codes. The alerts andforecasts are expressed in plain English language in standard formats.
The main function of this booklet is to give a full explanation of thesecodes and standard formats to enable observing stations to describe theirobservations and others to interpret the messages.
The plan for rapid solar‑geophysical services, described in moredetail in Part E, is briefly as follows: Many observatories cooperate
in providing promptly the results of their observations. These observa‑
tories are listed in Part D, together with the 5‑digit code numbers
assigned to each as "station indicators." (Note that the scheme ofstation indicators has now been completely changed from that used since
IGY.) The observatory prepares a data message according to the appro‑
priate data code given in Part C. The message is sent as promptly as
possible to one of the IUWDS Regional Warning Centers (RWC; see Part E);
it is sent to the RWC which is most convenient and most efficient as
regards communications possibilities. There is a regular interchange
once or twice each day among the RWC, as well as special messages(ADALERTs) when necessary. The RWCs use these data for issuing regularand special alerts and forecasts for their region, as well as for for‑warding messages with selected or summary data (see Part B) to individual
institutions or scientists which have requested these services. One of
the RWCs (the Western Hemisphere RWC at Boulder, USA (SOLTERWARN)) serves
as the IUWDS World Warning Agency and, on the advice of all RWCs, issues
worldwide alerts and forecasts (GEOALERT ― see Part B) which are distrib‑
uted through the RWCs, through the WMO meteorological telecommunications
networks and by radio broadcast (see Part E). The communications channels
used for this solar‑geophysical interchange are those which are available,
efficient and economical, including commercial, government or in some cases
the meteorological data channels. The RWCs and the National Warning Contacts
for each country (see Part E) make the necessary arrangements for each com‑munication circuit; in general, the originator of the messages assumes any
special costs.

Two of the important uses of the solar‑geophysical interchange
are for forecasting of ionospheric radio propagation conditions and fore‑
casting of solar activity. There have been important developments ineach of these subjects in recent years because of progress in scientificunderstanding and the introduction of new techniques of observation.
These developments in turn have had an effect on the plan for rapid solar‑
geophysical interchange and the selection of the important data parameters
to be included in the messages, and hence on the construction of the codes.
The two articles which follow this general introduction discuss some ofthe present philosophy as to the data most needed for forecasting. It isevident that participants in the rapid solar‑geophysical interchange aremaking possible the use of the most modern techniques by forecasting
services as well as providing important current information to the scien‑tific community.
This present (1969) IUWDS code booklet takes the place of the 1965
revised edition. The new codes should be introduced by observing stations
as soon as possible; they will begin to be used by RWC in May 1969. Almost
all of the previous codes have been changed, but since the changed codes
are identified by a new code word, there can be no confusion between the
new codes and the old ones (see Part G) .
Though the material presented in this booklet has been checked
several times, there no doubt have remained inaccuracies and ambiguities.
The user is invited to call any such errors to the attention of the IUWDS
Deputy Secretary (Miss J. V. Lincoln, E.S.S.A., Boulder, Colorado, USA,80302). Any substantial errors will be corrected through the series of"RWC Circulars" issued from time to time to RWCs and National Warning
Contacts.
The leader of the huge task of preparing this revised edition has
been the IUWDS Deputy Secretary, Miss J. Virginia Lincoln, in very close
association with the IUWDS Secretary, Dr. P. Simon, and with some assist‑ance from the undersigned. Many individual participants have made sug‑gestions, and valuable assistance has come from the RWCs who reviewed
drafts of the new codes. Acknowledgment is made to P. Simon and B. Beckmam
for the introductory articles on forecasting and to UNESCO for providing thenecessary support for printing, in the subvention received by IUWDS throughthe ICSU Federation of Astronomical and Geophysical Services.

A. H. Shapley, Chairman
International Ursigram andWorld Days Service(Boulder, Colorado, U.S.A.)
February 1969

A. II. Some

Comments on the Forecasting of Solar Activity
P. Simon ‑IUWDSSecretary

The indices of solar activity
Several indices may be used in order to forecast the solar acti‑
vity: the Wolf number, the 10 cm flux, the flare index and so on...
They are given in the form of numbers easy to use for an estimate of acorrelative function or any other computation. They appear like a very
simple expression of the activity, something like "high temperature incase of illness".
But after thorough observation of their physical content it isobvious that they combine several elements together, which are very
different on the grounds of solar activity. In the Wolf number several
tiny spots may possibly have the same weight as one very complex groupof spots whereas that one group may possibly be the one to produce anoutstanding flare. (M. J. MARTRES et al. 1966). The 10 cm flux comesfrom several active centers with definite different spectra in thecentimetric range, but the slope of that spectrum is connected withthe outstanding events in a specific sort of way. (H. TANAKA et al.
1964). The same kind of criticism may be raised against any global
index of solar activity: none of these indices can be of significant
use for the forecast of specific events.
Distribution of the flare activity amongst the solar centers
For many years now solar observers have had the feeling that some
active centers are very eruptive when others are very quiet. This isa point easy to check: trying to summarize the Quarterly Bulletin on
Solar Activity, with the help of some catalogues such as the Meudon
catalogue about active centers, it is easy to notice that 207aof them
give 807,of the flares. We conclude that we have to identify the erup‑
tive centers in order to forecast the solar activity.
The eruptive centers
It has been known for many years now that the Mt. Wilson magneticclassification of the spot groups is an index of the flare activity,(R. G. GIOVANELLI, 1939): the Gamma class with both polarities irregu‑
larly distributed amongst the spots is the most active class. But,
beside the spots, there is a noticeable surrounding magnetic field, and
it is not possible to describe the complexity of a group only according
to the polarity of its spots. (S. F. SMITH et al. 1968).
Our knowledge regarding the solar activity has been definitely
improved thanks to the study of the active centers magnetic field. On
this ground the first decisive results have been obtained at the Crimean
observatory and at the Meudon observatory. Their scientists could pointout the part played by the neutral line of the longitudinal component inthe life of a flare. (M. J. MARTRES et al. 1966 ‑ G. E. MORETON
et al. 1968). First of all no flare at all occurs without a neutral
line. Second, using good resolving power it is possible to specify
that most of the time the first bright tiny spots appear very near
the neutral line, on both of its sides. The third point is that inmany cases the flare grows into two bright ribbons which move a little
during their evolution to avoid the neutral line; they move at various
speeds in a way which makes the flare look like a Y after a few tenthsof a minute. (Z. SVESTKA, 1962 ‑ M. B. OGIR, 1967). According tothese data it is clear that there must necessarily be a strong connec‑
tion between the flare and the features of a neutral line.
A new step has been taken when Meudon observers emphasized thatthe more complicated the neutral line is, the more chance one has toobserve a flare at the same time. (M. J. MARTRES et al. 1966). At
the Lockheed Observatory a more extensive study about the most complex
state of that neutral line during the life of an active center came tothe same conclusions. (S. F. SMITH et al. 1968).
Optical data
As a consequence of these results the first material to be obtainedin order to forecast solar activity is the report of the neutral linefeatures of any active center coming out on the surface of the solar
disk. Now, the only problem is to obtain these data in due time andform.
First of all very few observatories can provide this material
rapidly and with adequate resolving power: any part of an active centerwith a tiny area of opposite polarity is an important datum for thisforecast. From the point of view of the practical realization, anotherdifficulty comes from the difference between the techniques used to
study an active center. It is necessary to build a composite drawingof the center in order to interpret the magnetic data correctly. Itmeans that one has to superpose the chromospheric data obtained in thecenter of Ha and in the wings of the K line as well as the estimate of
the magnetic field (given through a process related to the Zeeman effect)
upon the sunspot data obtained in white light. Some chromosphericfeatures such as the dark filaments and the edge of the plages havetheir counterpart in the magnetic field features: this remark may be
used for the setting up of this composite.
Another difficulty comes from the value of the data for the groups
situated near the solar limb at a meridian distance more than 60‑70°:
the angular slope of the line of sight with the solar radius makes theresults of the longitudinal component uncertain.
The last problem consists in reporting these features in a written
me ssage.

Radio and other data
Other data happen to confirm these optical reports. The firstone is related to the size, brightness and spectrum of the centimetric"spots". It has been pointed out first (M. R, KUNDU, 1959) that avery narrow and bright spot is a good source for centimetric outbursts
also associated with outstanding flares. Later, Japanese astronomers(H. TANAKA et al., 1964) studied the centimetric spectrum of these"spots": a flat spectrum in the range 7 cm to 3 cm is a good index ofthis important flare activity. The use of the brightness, spectrum
and flux obtained with a good interferometer can all together contri‑bute very valuably to the solar activity forecast.
Another interesting report is the X‑ray data: in the band 40 to
60 A an increase of the flux is related to the eruption of complex
active centers on the surface of the solar disk, and the increase of
the flux in the 1 to 8 A is related to the eruption of an outstanding
flare ere long. (R. MICHARD et al. 1968). There are practical prob‑
lems about that point, too. Most of the flares are able to produce
a short enhancement of the X‑rays flux during their eruption. These
data are obtained by a satellite which does not report the opticalflares, and up to now the X‑ray data have only been registered during
the ten minutes pass of that satellite: one must determine the actual
origin of any reported enhancement.
According to the Pioneer experiment carried out by the Chicago
group (R. Y. FAN et al. 1968) a continuous proton flux in the energy
range 0.6‑13 MeV is reported from a few active centers. These lastcenters produce flares with high energy protons and fill an inter‑
planetary magnetic sector which may possibly have a 180°aperture.
On neutron monitors a small decrease (J. P. LEGRAND, 1960) coincides
with this flow of low energy protons. The report of low energy flux
from space probe experiments and measurements and from neutron moni‑
tors may be used to identify the active centers that might produce
proton flares.
The estimate of the flare activity of the active centers
Using all these data simultaneously it is possible to make anestimate of the probability for flares occurrence for each of thesolar disk active centers. The X‑rays and proton data are global
data and the centimetric report is only related to a scanning of thesolar disk, but according to the solar and optical,data, one canmost of the time assign this estimate to each of the active centers
without ambiguity. According to this detailed prediction, it ispossible to expect a reasonable forecast of the global solar activity.
Flare forecasting
The best thing would be to have a possibility of forecasting theexact position, time of occurrence and size of the flares, at leastof the most important of them. In view of such a forecast, it would

be necessary to have in hand the very specific circumstances whichhave all contributed to the eruption of the flare. At the present
time the knowledge is still incomplete on that ground and the pub‑lished works only concern definite kinds of events: proton flares,
radio burst flares, weak flares and so on... Still, the observers
wonder whether the source is the same for all these manifestations.
Some flare appearancesThis first point was noticed long ago (R, G. GIOVANELLI, 1939).
If one considers the whole area of the sunspots, one may state veryclearly that the faster the evolution goes, the stronger the prob‑
ability for a flare's appearance. It has also been pointed out thatthe largest part of the spectacular solar activity seems to happen
close to a few solar longitudes (M. W. HAURWITZ, 1968). These lastpoints give a general impression but they cannot actually be used forthe forecast of specific events.
At the Crimean observatory 51 major flares were carefully studied(class 2 and greater). All of them were related to the report of astrong gradient of the magnetic field longitudinal component. Protons
have been reported (by balloon or by polar absorption) for the flares
related to the largest gradients and the figure of 0.1 Gauss/km seems
to be the step between the class 3 and class 2 flares. Noticeablechanges in the spot configuration were pointed out following proton
flares (S. I. GOPASIUK et al. 1963).
At Meudon some centers have been studied in relation with proton
events reported by polar absorption and related to metric noise storm
and classical type IV (Y. AVIGNON et al. 1964 ‑ C. CAROUBALOS, 1964).
The first one happens in an A or A1 configuration. There is a kind ofbalance between the two spots of opposite polarity which constitute that
configuration, and it may be an index of the next eruption of a flare.
The other flares related to radio events without particles appear ona B configuration with only one big spot. The importance of the mag‑netic field gradient has been acknowledged under the form of the ratioof the distance between the spots to the spot's diameters. But wemust notice that if on one hand most of the proton events and type IV
bursts occur on A, A1 or B configurations, on another hand many otherflares which are reported on these configurations are not proton events
nor type IV bursts. These last events are related to the biggest flares,
At Boulder it has been noticed that a Delta configuration plays animportant part in the proton flare's appearance. This configurationis the report of two spots of opposite polarity in the same penumbra(C. S. WARWICK, 1966).
Another study has been carried out at Meudon with the material
collected during the Cooperative Study of Solar Active Regions (M. J.
MARTRES et al. 1968, a and b). It is related to the eruption of any
flare during the life of several active centers. In fact, most of

these events are only subflares. For that work use has been madeof the sunspot data with identification of their magnetic polarities,
in order to specify the most important variations of the magnetic
field. According to that work any flare can occur when two spots of
opposite polarity are very near each other, and each one evolves the
opposite way, that is, the one increasing, the other decreasing interms of total flux or field intensity. This relation between theeruption of a flare and this evolution has been checked in both ways:
starting from the eruption of the flare or from the evolution of themagnetic features. Now it has been confirmed from magnetic measure‑ments related to an active center (E. RIBES, 1968).
Philosophy of this forecast
These last results allow one to accept two conclusions. First,
only a small number (one or two pairs) of the magnetic units or fea‑tures of an active center (or of two active centers close to eachother) may be concerned with a flare. The second point is that the
conjunction of two circumstances is necessary for a flare to be ob‑served. These are that magnetic features of opposite polarity exist
close to each other, and then the flare only occurs when they evolvethe opposite way. The first conclusion emphasizes the need for de‑tailed reports of the complex magnetic features. Global reports suchas the Zurich or the Mt. Wilson classifications are useful but not
sufficient for this kind of task. In order to forecast the place ofthe flare and its importance the reported material must describe any
active configuration as well as its size and distance to allow an
estimate of the gradient value and magnetic flux balance. In the sam
way the forecast must try to include the birth and evolution of anyof these small areas which are, in fact, the most important places.
Happily the outstanding events are most of the time related to large
active configurations easy to report.
The second conclusion emphasizes the most difficult point of any
forecast: the way the evolution goes.

The evolution forecast
Several data may be taken into account. The first consists inthe same flare activity. If a flare is connected with the evolutionof the magnetic features, the eruption of that flare is the best signof the right evolution of these features. The radio bursts, X‑ray
bursts, as well as any indirect report concerning a flare (such as
its ionospheric effect) are useful, but it is necessary to have theoptical data at one's disposal to know the associated active centers,
and these last data are quite difficult to obtain on a continuous
basis. To obtain them implies a network of observatories all cooper‑
ating together with good connections and good observers. Using theoccurrence rate of the flares, it is possible to forecast the coming

activity (V. BUMBA et al. 1968). But, in fact, it is necessary touse other signs showing the flare activity at the same time because
the survey of a flare can only be used after the eruption of several
flares and it is of no use for the forecast of those first flares.
Another possible means consists in studying the evolution of theactive centers. This is a very hard problem. There are plenty ofstatistics concerned with the evolution of the active centers accord‑
ing to the Zurich classification, but this does not help much. A
first step has been taken at Meudon related to the birth of a bipolar
active center beside or inside a previous active center. (M. J. MARTRES,
1968). Depending on the stage of evolution of the first center andthe position of the new one some rules can be established, which givean opportunity to forecast the evolution of both groups. The funda‑
mental aspect is that the remnant magnetic structures existing at a
center's birth‑place or nearby are an important factor in the evolutionof the new center. The largest production of flares is related to thesimultaneous birth of several centers very near one another. This is
only a preliminary approach, but it looks full of promise. Still, there
is a problem about the circulation of the solar data in a form thatmight be suitable for that kind of forecast. There is a satisfactory
start and improvements are expected before long.
Proton events, geomagnetic storms, etc.
All these geophysical events are concerned with solar activity,
and as reported above, the flares and active centers have been studiedin connection with these geophysical events. In some ways the fore‑
cast of a flare might be a preliminary warning of a geophysical event.
The report of an A configuration as well as the forecast of the rightevolution results in the forecast of proton events. It is the only
valuable forecast concerning that event. SID can be forecast in thesame way.
About geomagnetic storms there is still another possibility related
to the travel time of the shock wave between the sun and the earth.
According to the reported radio emission of the flare, and to the pre‑vious geomagnetic activity, one can evaluate the speed of propagationand predict the time of the arrival (C. CAROUBALOS, 1964 ‑ T. OBAYASHI,
1962).
There is also a delay between the occurrence of the proton eventon the sun and its arrival on the earth. It may be shorter than 20
minutes, but it can last a few hours or more. According to the centi‑
metric flux (M. PICK, 1961), it is possible to forecast the arrivalof the protons, but it is hard because of the short delay and the prob‑
lem of the reception of the data on a real time basis.

Limitations of the forecasts
The limitations come from many different circumstances. Firstof all the value of the available material may change from day today, and it unfortunately happens that on some days no material orreports are available. Another point is related to the same solar
activity. Many of its aspects escape any form of available fore‑cast. For instance we have not been able to predict the birth‑
place and date of appearance of any new center up to now. Some
events are unusual, such as the proton events of January 28, 1967.
They also escape being forecast. How long in advance could a fore‑
cast be issued? One point is the rotation of the sun. But the mostcritical point is the speed of the evolution of the active centers.
The quicker they grow, the more flares they produce. As a conse‑
quence the longest reasonable delay is about two days. This limi‑
tation comes from the possible unexpected birth of new centers.
The new codes
It is impossible to obtain the data which are required for theforecast within the limits of one observatory only. From the mere
point of view of the group's evolution a lot of information is re‑quired, (such as flare appearances and so on...) from different ob‑
servatories situated at different longitudes. At the present timesome data can only be obtained by a single observatory in the wholeworld (radio location at different frequencies).
Still, bad weather sometimes prevents one from making observa‑
tions. Then an exchange of data through encoded messages is required
and sometimes difficult. But all things considered, it is the easiest
way since it eliminates the difficulty of the difference of languages,
and is the most secure as far as it states very clearly the natureof the data to be given. Further, each group of observers only sends
one or two different classes of data, and the codes rapidly growfamiliar. On the other hand, changes introduced in the codes arealways difficult, because it is hard to change habits. However, as
far as the codes are concerned the scientific progress must be taken
into account to make the data really useful. These are the reasons
which induced us to discuss the problem. We especially tried to con‑stitute a bibliography as complete as possible to allow the observers
to improve their documentation, and to justify the eventual changes
and introduction of new elements in the codes.
Conelusion
The first aim of the forecast of solar activity and geophysicaldisturbances was to improve the effectiveness of radio telecommunica‑
tions by way of the ionosphere, and despite the introduction of relay
satellites and the perfecting of alternative techniques of telecom‑
munications on the earth, the problem has not much changed. As amatter of fact the traffic grows more rapidly than the facilities;andthe new techniques allow wider and consequently more difficult trans‑missions and connections. But since the birth of the space researchand the new technical possibilities placed at the experimenter's
disposal, these forecasts became an essential element for many ofthe very ticklish space experiments. Finally, the manned satellites
and space probes, as well as the commercial supersonic flights, raise
the problem of the preservation of the human life or health acutely.
This does explain the increasing interest taken in the study of solar
activity and in all the techniques which allow a prompt reduction of
the data in view of immediate use. Of course, all this implies new
hard problems for the observatories where the systematic observations
and research programs exist competitively. It also states the prob‑
lem to those involved in forecasting and related work: must theforecast activity be the job of technicians or must it be part of thework of a research group? From the scientific point of view the prob‑
lem concerning solar activity is not yet on a level where the defini‑tive question consists in determining a quantity or a temperature.
It is a matter of evolutive phenomena, and the rules governing suchan evolution are still to be learned. They are the key for the fore‑cast.
To dedicate a few moments daily to participating in some part of
the total forecasting activity is tantamount to collating the previous
knowledge with the concrete reality. Clearly, this is a aood stimulus
for research on the basis of increasing knowledge as well as obtainingof a few more bits of data. On another hand some experimenters statevery difficult questions to the forecasting centers. They are glad tosubmit them to scientists well informed on these problems.
Finally, we must admit that the forecast of solar activity morethan any other activity must be the result of international cooperation:
cooperation on the grounds of obtaining the data, of the elaborationof the methods, and for the best profit of the users. This emphasizes
the part which may be played in view of such a cooperation by the Inter‑national Ursigram and World Days Service, as far as it is the necessary
basis for the cooperation and makes it possible and easy. The 1966
Proton Flare Project was an occasion to make its efficacy on a world‑
wide scale quite apparent. Let us hope that this service will confirm
these possibilities on the grounds of the various projects accepted by
the Inter‑Union Commission on Solar‑Terrestrial Physics for the coming
years.

P. SIMON
Meudon, November 28, 1968

BIBLIOGRAPHY

AVIGNON, Y., MARTRES, M. J., and M. PICK, Identification de classesd'eruptions chromospheriques associees aux Emissions de rayons
cosmiques et a l'activite radiofelectrique,Ann. Astro. 2̲7,23‑28,
1964.
BUMBA, V., KRIVSKY, L., MARTRES, M. J., and I. SORU‑ISCOVICI, Flareactivity and spot groups development, n' 35 IAU Symposium, 311‑317,
1968.
CAROUBALOS, C., Contribution a l'etude de l'activite solaire en relation
avec ses effets geophy siques,Ann. Astro. 2]̲,333‑338, 1964.
FAN, C. Y., PICK, M., PYLE, R., SIMPSON, J. A., and D. R. SMITH, Protons
associated with centers of solar activity and their propagation ininterplanetary magnetic field regions co‑rotating with the sun,
J.G.R. 73.,1555‑1582, 1968.
GIOVANELLI, R, G., The relations between eruptions and sunspots, Ap. J.
89, 555‑567, 1939.
GOPASIUK, S. I., 0G1R, M. B., SEVERNY, A. B., and E. F. SHAPOSHNIKOVA,
The structure of magnetic fields and its variation in flare regions,Izv. Krym. Astrofiz. Obs. 2̲9,15‑67, 1963.
HAURWITZ, M. W., Solar longitude distributions of proton flares, meterbursts and sunspots, Ap. J. 151, 351‑364, 1968.
KUNDU, M. R., Structures et proprietes des sources d'activite solaire surondes centimetriques, Ann. Astr. 22, 1‑100, 1959.
LEGRAND, J. P., Les prebaisses de rayons cosmiques en periode de maximum
de l'activite solaire, Ann. Geoph. 16̲,140‑142, 1960.
MARTRES, M. J., MICHARD, R., and I. SORU‑ISCOVICI, Etude morphologiquede la structure magnetique des regions actives en relation avec lesphenomenes chromospheriques et les Eruptions solaires, Ann. Astr. 2̲9245‑253, 1966.
MARTRES, M. J., Origine des regions solaires actives "anormales", nJ 35
IAU Symposium 25‑32, 1968.
MARTRES, M. J., MICHARD, R., SORU‑ISCOVICI, I. and T. TSAP, A study ofthe localization of the flares in selected active regions, n' 35
IAU Symposium 318‑325, 1968a.

MARTRES, M. J., MICHARD, R., SORU‑ISCOVICI, I., and T. TSAP, Structure
evolutive magnetique des regions actives solaires, Solar Physics ̲5,
187‑206, 1968b.
MICHARD, R., and E. RIBES, La composante lentement variable des rayons X
solaires en relation avec la structure des centres d'activite, n'
35 IAU Symposium, 420‑430, 1968.
MORETON, G. E. and A. B. SEVERNY, Magnetic fields and flares in theregion CMP 20 September 1963, Solar Physics 3, 282‑297, 1968.
OBAYASHI, T.j Propagation of solar corpuscules and interplanetary magnetic
fields, J.G.R. 67, 1717‑1729, 1962.
OGIR, M. B., Some peculiarities of the origin and motion of the flaresaccompanied by type IV bursts, Izv. Krim. Astrofiz. Obs. 37̲,94‑104,
1967.
PICK, M., Evolution des emissions radioelectriques solaires de type IV etleur relation avec d'autres phenomenes solaires et geophysiques, Ann.
Astr. 24, 183‑210, 1961.
RIBES, E., Private communication, 1968.
SMITH, S. F., and R. HOWARD, Magnetic classification of active regions,n" 35 IAU Symposium 33‑42, 1968.
SVESTKA, Z., Motions in chromospheric flares, Bull. Astr. Inst. Czekoslovaki
190‑198, 1962.
TANAKA, H. and T. KAKINUMA, The relation between the spectrum of slowly
component of solar radio emission and solar proton event, Rep. Ion.
Space Res. Japan ̲18.,
32‑41, 1964.
WARWICK, C. S., Sunspot configurations and proton flares, Ap. J. 145,
215‑223, 1966.

A. III. ^c^ientj.ficInformation deeded for Radio Propagation Forecasting
B. Beckmann ‑RWC‑Darmstadt

The ionospheric transmission frequency range is represented by thevariation of field strength as a function of time and frequency. Its
Limits are affected by the standard‑MUF, operational MUF, LUF, signal‑
to‑noise ratio (atmospheric and man‑made noise or interference) and thefading‑character, i.e., the distortions of the signals caused by thelatter vary as a function of the type of service. The objective of
the forecasting activity should be the prediction of the transmission
frequency range expressed in median values for a relatively long time(e.g., monthly median predictions) together with additional information
about short‑term variations exceeding the normal statistical deviations(disturbances, e.g., daily forecasts). For the description of theseshort‑term variations use is made of current, if possible real time
critical frequency values of ionospheric sounding stations (e.g., foF2
and f‑min) [ see UFOFI, UFOFO, (JFOFU,ION '. If these data are notavailable to a sufficient extent, current observations of field strength:of azimuthally distributed long distance transmission areas are used asa function of frequency and time [ published by ESSA Research Laboratorie:
in the series "Solar‑Geophysical Data" as Transmission Frequency Ranges‑
North Atlantic Path, Observations by Deutsche BundespostJ. These ohser‑
vational results can be combined in a so‑called 'band character figure"(these are the product of the usable transmission frequency range times
the mean logarithmic field strength). Values are normalized with respecl
toG = 0.0 torunningaverageand adapted
scale from
9.8a insteps of0.2 (normal
valuetoG a= prediction
6.0) [see PROPO].
These character
figures show the times of quiet conditions (G >6, broad transmission
frequency ranges with high field strengths) and of disturbances (G <6,narrower frequency ranges with lower field strengths), as well as theirregional differences. Assessed quality figures as provided by radio
operators from different stations can also be used.
The above mentioned ionospheric parameters define the propagation
conditions as a basis for the forecast. Its extrapolation in time (ifpossible by autocorrelation) is also an important basis for the fore‑
cast, especially in comparison with the previous solar rotation period.
The extrapolation in time of operational parameters is studied in de‑tail by CCIR (CCIR Doc. Vl/160, Boulder 1968)." The same applies tothe precursors indicative of short‑term variations caused by solar‑
terrestrial relations (CCIR Rep. 247‑1, St. Pr. 10 A).* The following
is involved in the behavior of ionospheric propagation:
1. the solar activity centers
2. the state of the interplanetary space (solar wind, inter‑
planetary magnetic field, its sector structure, etc.)
3. the magnetosphere
4. the ionosphere"These documents are usually available from national administrations
for ITU; the IUWDS Deputy Secretary can supply copies upon request.

Flares of all importance classes 1 UFLAH, UPATP, UPATV■can produce
an SID fUSIDO] and, after 1 to 2 days, ionospheric storms FUABSE accom‑
panied by geomagnetic storms [UMAGE1 may occasionally take place. SIDs
(SWF, etc.) occur, if the X‑ray flux ! USOXOl is greater than 2xl0 3
erg/cm sec in the range below 8 A. Besides larger flares other solar
phenomena such as active prominences, surges and limb flares may be theradiation centers. The general tendency of SWT, SES, SPA, etc. 1 USIDO1
can be forecast in steps of different probability.
Ionospheric or geomagnetic storms not related to specific outstand‑ing flares can be related to special centers of activity, the so‑called
M‑regions (Bartels).
The probability of occurrence of ionospheric storms is increased:a) in case the activity centers or flares occur in CMP + 30' withspecial emphasis to the west side ＼most of the solar codes1b) in case there are bright and large plages or rapidly developing
sunspot groups TUSSPR, USSPS, UPLAK, UPART], increased corona‑line emissions PUCORE'andactive prominences.
c) the magnetic (3yand Y configuration of spot groups enhances theprobability of flares about 5 times TuSSPl],d) in case major‑plus bursts occur at decameter waves in the pre‑maximum phase of the flare r URANO, URALE],e) in case a type IV occurs with a well‑developed continuum in the
cm‑ and m‑wavelength range rURANZ￨ initiated by an increasing
SHF radiation [URANO],f) in case the tendency of a proton flare is indicated by magnetic
6 configuration I'uSSPI,UPART: , by increasing of the 3 cm flux
density, and by the fact that the spectral ratio of emission at
3 cm to emission of 10 cm is greater than the mean and is of
the order of unity.
g) in case that after emission of energetic protons from type IV
centers a PCA occurs within about 6 hours observed by riometeras cosmic ray associated [UABSE, type III] or as phase ‑ andamplitude variations observed on VLF circuits via the polar‑cap.
h) in case successive type IV outbursts occur in "repetition cen‑ters", grouped in privileged areas of the sun‑i) in case energetic protons (30‑100 MeV) are detected over thepolar region or a GLE (>1 GeV) is observed in cosmic rays
[UCOSB, UCOSE].
j) in case the precipitation of electrons is indicated by aurora[UAUREj and the existence of soft X‑ray radiation by black‑outs[UABSE, type IIj.
k) in case pre‑decreases or anisotropic effects in the amplitude
and phase of the daily variation of the cosmic rays are detected[UCOSE] in connection with characteristicvariations of worldwide
positive phases (G >6) and local break‑downs in the night‑criticalfrequencies foF2 (see above).

1) in case these variations are about parallel with thosein the previous solar‑rotation corresponding to the sector‑
structure of the solar‑interplanetary magnetic field and adevelopment tendency of a disturbance is indicated by thiscomparison. Critical time intervals are local break‑downsof critical frequencies foF2, geomagnetic disturbances,
ionospheric positive phases as well as the disturbances in
the previous solar rotation.
The above mentioned criteria are derived from the interpretationof a number of geomagnetic or ionospheric events. They are not always
applicable and their importance changes within the sunspot cycle. The
physical relations are only known in part. Therefore, forecasts arestill difficult. The forecasters are very grateful to get flare fore‑casts from the solar observatories in the GEOSOL, SDF, SFD‑Reports.
The same applies to solar and geomagnetic development tendencies indi‑cated therein. Successful propagation forecasts require the latest
information to be passed on as soon as possible. Some radio propagation
forecasts are included in the Ursigrams for scientific purposes [FORDA,
FORWE] .

B. Beckmann
RWC‑Darmstadt
December, 1968

19

PART B. ALERTS

AND COMBINED MESSAGES

I.1 Alert Messages for IUWDS by RWC
Code 1: ADALERTII.1 Alert Messages for Worldwide Dissemination
Code 1: GEOALERT
III.1 Advice from Regional or Associate Regional
Warning Centers to World Warning Agency
Code 1: ADV‑‑
IV.1 Combined Solar‑Geophysical Data and Forecasts
for Remote Regions or General Users
Code 1. GEOSOLPART RALERTS AND COMBINED MESSAGES

B. 1.1 Alert

Messages for IUWDS by RWC

Code 1. ADALERT
1. Content.
Report of major events to the other RWC and to the local orregional customers, and as advice to include in the GEOALERT
2. General form.
ADALERT observatory

JJHHmmreport3. Definitions.
ADALERT = key word for advance reporting of major events
observatory = name of reporting observatory in clear text
JJHHmm = Greenwich date and time of issue of message inhours and minutes UTreport = one or more of statements as below
For GEOMAGNETIC ACTIVITYMAGSTORM BEGINS JJHHmmZ
STRONG MAGSTORM IN PROGRESS JJHHmmZ
Note: One may add plain language comments related toauroral reports or Forbush effect expected
For MAJOR FLARESSOFLARE ‑ importance class ‑ coordinates (i.e. N20 E78) ‑ JJHHmmZ(date ana time) ‑ "duration in minutes given" or statement "in pro^resd"
Note: One may add plain language comments like "Y‑shaped" or"covering spots" or "suspected proton flare"
For TENFLARETENFLARE (solar
radio
outburst
10 cm) in minutes, or‑ XX units‑ emission
JJHHmmZ for
onset at‑ duration
statement "in progress" at the time of ADALERT, or statement"observed until hours and minutes UT"
Note: Units
givelevel
the increaseof the flux
density^over
the 1)
pre‑burst
in conventionalunits(10 22Wm 2Hzby two significant digits and words such as 1700 units

B. 1.1 Code1 (continued)

For PROTON EVENTCOSMIC RAY INCREASE ‑ JJHHmmZ ‑ percent increase above normal basedon neutron monitor
POLCAP ABSORPTION ‑ JJHHmmZ ‑ dB of absorption by riometer or iono‑
spheric forward scatter technique
PROTON EVENT ‑ JJHHmmZ ‑ specify energy range from a spacecraft report
1. ADALERTS should be circulated as soon as the event has beenrecognized.
2. The ADALERTS will only report events and no forecasts. Any
unexpected change of a forecast would be sent to the interested
customers as an advice or a CORRECTED ADVICE.
3. If the observatories follow this scheme, it is not necessary
to report the kind of experiment
SOFLARE signifies a chromospheric report
TENFLARE signifies a centimetric outburst
COSMIC RAY INCREASE signifies a neutron monitor count increas<
POLCAPsignifiesa groundbasedonly
polar cap report
PROTON ABSORPTIONEVENT signifies
spacecraft
reports

B. II.1 Alert

Messagesfor Worldwide

Dissemination

Code 1. GEOALERT
1. Content.
Major
2. General
IUWDS

eventsand forecasts

for worldwide

JJNNN

type

statement

Ursigramand World

distribution

form.

GEOALERT

3. Definitions.
IUWDSGEOALERT= International= worldwide

Days

JJ = Greenwich date of issue ― at 0400
NNN = serial number of GEOALERT message
Statement

Service

Alert
UT= one or more of following types
For no alert‑ NIL
For flares
SOFLARE FLARES EXPECTED ONE * (coordinates
SOFLARE FLARES EXPECTED TWO ""(coordinates)
SOFLARE PROTON FLARE EXPECTED (coordinates)
SOFLARE PROTONFLARE
JJ/HHmmZ (coordinates)
SOFLARE ENDS OR SOFLARE ALERT ENDS

i.e. N10E20)

Note: Whenappropriate, add elaboration,i.e., EAST LIMB, DELTA SUNSPOT, RADIO
For geomagnetic storms
MAGSTORM EXPECTEDMAGSTORM BEGINS JJ/HHmmZMAGSTORM EXISTSMAGSTORM ENDS OR MAGSTORM

ALERT

BURST

ENDS

Note: Whenappropriate, add elaboration,i.e., MAJOR (if Ap>50),
GREAT (if Ap >100)or AURORA (if unusual aurora expected)
For cosmic events
COSMIC EVENT BEGINSCOSMIC EVENT EXISTSCOSMIC EVENT ENDS

JJ/HHjimZ

Note: Whenappropriate,
add elaboration,i.e., COSRAY INCREASE, POLCAP ABSORPTION,FORBUSK DECREASE.

* Importance class one or two

B. II.1 Code1 (continued)

For stratospheric warmings
STRATWARM (Day of week) STARTS GEOGRAPHIC AREA
STRATWARM (Day of week) EXISTS GEOGRAPHIC AREA
STRATWARM ENDS
Note: Whenappropriate,elaboration
will beadded,
i.e., STATIONARY
or SPRINGCIRCULATION CHANGE PROGRESSING, etc.
Notes: 1.

If two or more alerts are issued on one GEOALERT message,
each receives a serial number

2. STRATWARMS are not numbered.
3. No

serial number is used if GEOALERT is NIL.
WMO Distribution of Geoalerts

The GEOALERT is given very extensive and worldwide distribution
through the cooperation of the World Meteorological Organization's (WMO)
telecommunications network. The GEOALERT is issued once daily by the IUWDSWorld Warning Agency ― the Regional Warning Center at Boulder, Colorado,
U.S.A. The GEOALERT for observational purposes, begins upon receipt of
the telegram at the station, hopefully well before 1200 UT, and lasts
until the next GEOALERT message is received which may continue, changeor end the Alert.
To identify these messages on the WMO network the introductory words"IUWDS KWWA" preceed the GEOALERT statement. The message is delivered to
the Washington outlet of the network every day at 0400 UT and is given
worldwide distribution in the hours following. Meteorological stations
and solar or geophysical stations on the network are thus served automat‑
ically. Other solar and geophysical stations can often make local arrange‑ments with the director of their meteorological service or with a nearby
meteorological station for regular delivery of the IUWDS GEOALERT message.
In case the use of WMO channels is impractical arrangements can be madewith the RWC, each of which receives the message promptly directly from the
WWA. A National Warning Contact (see Part E‑III) is designated for eachparticipating country to assist with these arrangements.
Broadcasts of the GEOALERTS by WWV and WWVH
The GEOALERT for a given day is first broadcast at 0418 UT on station
WWV‑, Fort Collins, Colorado, then at 0448 UT on station WWVH**, Maui,
Hawaii, and at hourly intervals until the next alert is issued. In case ofdelay in receipt of the daily message, WWV or WWVH will be silent at 18 or
48 minutes after the hour UT, respectively, until the new message is received.
* WWV frequencies: 2.5, 5, 10, 15, 20, 25 MHz** WWVH frequencies: 2.5, 5, 10, 15 MHz

Each message begins with letters GEO in Morse Code and the coded
information follows. This coding permits three types of information ateach broadcast ― each in the form of letters repeated three times in slow
International Morse Code. The first set concerns the forecast of solar or
geophysical events or the observation of a stratospheric warming (or theobservation of a stratospheric warming together with a forecast of either
solar or geophysical event). The letters which may occur in the first set
and their meaning are as follows:

The second and third sets of letters refer to the occurrence of observed
solar and geophysical events. The time of onset of, or the existence ofthe phenomenon is included by the letter broadcast. The coding for thetime and type of event is shown in the table given below:

The letters have no significance; however, in general the older the evenl
is at the hour the message is issued, the longer is the broadcast time oJ
the coded symbol.
Sample messages (in International Morse Code):
GEO SSS EEE DDD
signifies: GEO= solar geophysical message

SSS = PROTON FLARE expected
EEE = no PROTON EVENT between 0000 UT yesterday and0400 UT today
DDD = GEOMAGNETIC STORM occurred (began) between
1800‑2400 UT yesterdayGEO III GGG NNN
signifies:

GEO= solargeophysicalIII = FLARES

expected

GGG = PROTON

EVENT

NNN = GEOMAGNETIC

in progress
STORM

Other

See

By Federal

RepublicSee

By Japan:See

By U.S.S.R.:

began

Broadcasts

By France:

By India:

messagepage

12

UT today

7.

140‑

page

134‑

page

0000‑0400

of GEOALERTS

of Germany:

page

See

between

133

See

page

129.

B. III.l Advice from Regional or Associate Regional Warning Centers toWorld Warning Agency
Code 1. ADV―

1. Content.
Advice concerning solar or geophysical activity to include in theworldwide GEOALERTADV = ApVice to World Warning Agency
aa = RWC or ARWC issuing message
BO = Boulder (SOLTERWARN)DA = Darmstadt
IR = Irkutsk
KO = Kokubunji
MO = Moscow

JJHHmmforecast)= Greenwich

date

and time

ND
NE
PA
PU
ST
SY

=
=
=
=
=
=

of message,

New Delhi
Nederhorstdenberg
Paris
PragueStockholm
Sydneyhours

and minutes

UT= ALNIL = recommend no alert
SOLNIL = recommend no solar alert
MAGNIL = recommend no geophysicalalert
FLARE EXPECTED (include coordinates,
i.e. N20 E78) signifies
recommend alert for many flares class one in one orseveral active centers
MAJOR FLARES EXPECTED (include coordinates)
signifies recommend
alert for flares class two or more
PROTON FLARE EXPECTED (include coordinates)
signifies recommend
alert for a flare with high energy protons
MAGSTORM EXPECTED signifies recommend alert for a geomagneticstorm
c = available
1 = a
2 = a
5 = a
6 = a

optical material
few data reported to
lot of data reported
few data observed at
lot of data observed

RWC and few data
to RWC and a lot
RWC and a lot ofat RWC and a few

observed at RWC
of data observed at RWC
data reported to RWC
data reported to RWC

B. III.l Code1 (continued)

available solar magnetic data
1 = Mt Wilson‑type classifications reported to RWC
2 = more sophisticated data report to RWC
5 = minimal magnetic data observed at RWC
6 = detailed magnetic data observed at RWC
available radio data
1 = a few total flux data reports
2 = several total flux data reports
5 = localization of radio sources at a few wavelengths
6 = localization of radio sources at several wavelengths
Greenwich date for the next advice message
Note: FORTE = strong, or PIANO = weak, may be
added, if desired, for strength ofopinion for each individual forecast.

29

B. IV.1 Combined Solar‑Geophysical Data and Forecasts for Remote
Regions or General Users
Code 1. GEOSOL
1. Content.
For sending combined data to remote regions, or for general data

B. IV.1 Code1 (continued)

JJ = Greenwich day of month
HHmmZ = hours and minutes UT of the beginning of the flare
Q = quadrant (heliographic coordinates) of the flare
1 = NE (north‑east) 3= SW (south‑west)
2 = SE (south‑east) 4= NW (north‑west)
XX = distance to central meridian in degrees
YY = heliographic latitude in degrees
Note: In case of indirect detection, the group
QXXYY will be omitted.
MAGSTORM = key to indicate beginning of magnetic storm to follow
JJ = Greenwich day of month
HHmmZ = hours and minutes UT of the beginning of the storm
Notes; 1.

When no outstanding events to be reported,
this part of the message will not be given.

2. If an event does not exactly correspond to
the above conventional classifications, itwill be described in clear text.
3. Events mentioned here can have formed thesubject of a special message: in this case,they will
alwaysinformation
also be reported
heresincetoincludefurther
received
the time of issue of the special message.

DETAILED FORECASTS (DATA AVAILABLE INDICATED)
A. SOLAROBSERVATIONS AVAILABLE
888 = key numbers to indicate the part of the message dealing withsolar observations available, description of activity of thesolar centers and forecasts
JJ = Greenwich day of the description (normally same as day of themessage)
7777 = key to indicate the more or less complete character of theavailable local observations (external observations assumed
to be available in all cases)
c = definition of available observations
0 = no local observations
1 = no local optical solar observations but solar radio
observation exists
2 = part of local optical solar observations available
3 = all of local solar observations available
4 = local solar observations include measurement ofsolar magnetic fields

B. IV.1 Code1 (continued)

DETAILED FORECASTS
For each active center two groups as follows:
Q = quadrant (heliographic coordinates) of the active center
1 = NE (north‑east) 3= SW (south‑west)
2 = SE (south‑east) A= NW (north‑west)
XX = distance to central meridian in degrees
YY = heliographic latitude in degrees
Note: The position QXXYY is given for the day JJ
at time of the message.
Descriptive words for groups with spots:
Quiet = less than one Chromospheric Event a day is expectedin this center.
Eruptive = at least one Radio Event or several Chromospheric
Events expected.
Active = at least one Geophysical Event or several Radio
Events expected.
Proton = at least one High Energy Event expected.
Notes: 1. Eventsare classified as below:a) Chromospheric Events: some flares are just
Chromospheric Events without Centimetric
Bursts or Ionospheric Effects. (SID).
b) Radio Event: flares with Centimetric Bursts
and/or definite Ionospheric Event. (SID).
c) Geophysical Event: flare (class two or more)with Centimetric Outbursts (maximum of theflux higher than the Quiet Sun flux, duration
longerthan
10 minutes)
and/orstrongSometimes
theseflares arefollowedby SID.
Geomagnetic
Storms or small PCA.
d) High Energy Event: flare (class two or more)with outstanding Centimetric Bursts and SID.
High Energy Protons are reported at the Earthin the case of most of these events occurringon the western part of the solar disk.
2. Some quiet groups being of very little importance,these can be reported only by their number.
3. If insert word CAUTION between QXXYY group anddescription word, it signifies one cannot forecast
real evolution of the group at time of the message.
4. If insert word DOUBTFUL between QXXYY group anddescription
word, it signifies
it isofimpossible
determine definitely
the true classactivity to
fromthe available information.

B. IV.1 Code1 (continued)

C. ALERTS
The Alerts are forecasts related to specific scientific programs. The
Alert messages are difficult to diagram, the different possibilities arepresented here.
SOLNIL =there is no alert
SOLALERT = the beginning or continuing of a logistical alert,
there is no observational alert but the solar activity
increase could evolve into greater activity that would
initiate an observational alert.
PROTONALERT JJ/KK)

XRAYALERTJJ/KKMAGALERT JJ/KK)) =type
an observational
thestatedfor the daysalert
JJ to of
KK,
inclusive

Protonalert = a High Energy Event is expected in this center
during a period which is very hard to estimate,(from one to three days). We cannot give any
estimate of the speed of evolution of the group,
nor forecast the time the flare will occur.
Xrays alert = High Energy Event is expected on the easternpart of the disk of the Sun.
Magalert =a Geomagnetic Storm is expected.
PROTONIL )XRAYNIL )MAGNIL )= end or cancellation of an observational alert

Alerts corresponding to different programs can be sent simultaneously.
They are repeated as long as they are justified.

35

B. IV.1 Code1 (continued)

D. FORECASTS
When the situation is favorable, general forecasts for several days
can be sent in clear text. These will not be repeated on succeeding days

FIN = end of message

EXAMPLES
1. Indirect detection of a flare and forecasts
GEOSOL MEU07 201550Z
99919 1//// 21280 30280
MAJOR FLARE 190247Z

40190 0010/

88820
12817 77773
13817 47020
18020 42317
QUIET 22015
SOLNIL 12123
SPOT GROUP NOW 17N38E WILL BE ACTIVE
AFTER FEW DAYS FIN
2. Observation alert ‑ includes calm regions grouped
GEOSOL MEU09 221657Z
99921 11050 2///1 30120 40110 00///
MAGFLARE 220025Z 16223
88823 77772 FIVE GROUPS QUIET 16023 ACTIVEMAGALERT 23/24 FIN
3. Logistic alert ‑ a non‑classical flare
GEOSOLMEU14 21791
301630Z
99929 12164
30080 00254
MAJ0RFLARE 300851Z 44322 MAGSTORM 300139Z
88830
41517
15426
16516
17723
QUIET
21620 77772
ERUPTIVE
45223
43821
ACTIVESOLALERTFINC DATA

CODES

I. 1 Sunspots
Code 1. USSPS
Code 2.
Code
3. USSPR
USSPI
1.2 Solar Flares
Code 1. UFLAH
Code 3.
2. UPATV
UPATP
Code
1.3 Calcium Plagesand Centersof Activity
Code 1. UPLAK
1.4 Solar Corona
Code 1. UCORE
1.5 Solar X‑rays
Code 1. USOXO
Solar ParticleEvents
Code 1. UPART
1.7 Solar Wind Parameters
Code 1. USOLWPART CC.I SOLARDATA CODESOPTICAL, X‑RAY AND PARTICLE OBSERVATIONS

C.I.I SUNSPOTS
Code 1. USSPS
or
Code 2. USSPR
1. Content.
Description of sunspot groups, if key word is USSPS
Description of sunspot groups and their associated Ka structure,
if key word is USSPR

This code identical with USSPS, with the addition of groups "OXXYY jjklm".

1.1 Code1 or Code 2 (continued)

Definition of symbols.
USSPS = key word, SunSPotSorUSSPR = key word, SunSPot Regions
IIIII = station indicator (See lists in Part D.)
JJ = Greenwich date of observation
HHH = hours and tenths of hours UT of observationaaa = relative sunspot numberb = seeing quality
1 = very poor
2 = poor
3 = fair
4 = good
5 = exceptionalc = solar disk size used for measurement
1 = diameter of the solar disk less than 15 cm
2 = diameter of the solar disk between 15 and 30 cm
3 = diameter of the solar disk more than 30 cm
4 = individual sunspot groups at very high resolution
dd = serial number of sunspot groupeee = area of sunspot group in tens of millionths of the solar
hemisphereQ = quadrant (heliographic coordinates) in which geometriccenter of sunspot group is located
1 = NE (north‑east) 3= SW (south‑west)
2 = SE (south‑east) 4= NW (north‑west)
XX = distance to central meridian in degrees
YY = heliographic latitude in degrees
f = type of penumbra in the largest spot in group (see diagram)
0 = no penumbra (Zurich class A or B)
1 = rudimentary (r)2 = small symmetric (s) (diameter less than 2.5°)
3 = small asymmetric (a) (diameter less than 2.5°)
4 = large symmetric (h) (diameter greater than 2.5°)5 = large asymmetric (k) (diameter greater than 2.5°)
g = relative importance of the leading spot and density of thesunspot population (see diagram)
1 = leading spot largest and sunspot population density open
2 = following spot largest and sunspot population density op<
3 = leading and following spots nearly same size and sunspot
population density open
4 = leading spot largest and sunspot population density
intermediate
5 = following spot largest and sunspot population density
intermediate
6 = leading and following spot nearly same size and sunspot
population density intermediateC. 1.1 Code1 or Code 2 (continued)

7 ‑ leading spot largest and sunspot population density
compact
8 = following spot largest and sunspot population density
compact
9 = leading and following spot nearly same size and sunspot
population density compact
Note: g= / (slant line) for unipolar spots of Zurichclass A, H or J

h = Zurich sunspot class (see illustration)

Note: Normally G will be encoded as an open E or F and J
will be encoded as a small H.
ii = number of spots in the group
Q = quadrant (heliographic coordinates) in which the geometric centerof Ha plage associated with the preceding spot is located
1 = NE (north‑east) 3= SW (south‑west)
2 = SE (south‑east) 4= NW (north‑west)
XX = distance to central meridian in degrees
YY = heliographic latitude in degrees
jj = longitudinal extent of the Ha plagek = Ha brightness on a scale of 5 steps
1 = faint to 5 = very near to flare brightness
1 = description of the bright H‑alpha structure (see illustration)
1 = sc; scattered bright points
2 = sp; separated areas of bright plage; interior of theregion not bright3 = cn; connected areas of bright plage filling the interiorof the region, but with corridors among them
4 = cm; compact plage with little or no space among emittingareas
5 = cx; complex structure embedded in large, compact plagem = dark filament in relation to the photospheric spots (see illustration)
1 = no associated filament
2 = filament between the two main spots and basically parallel
to a solar meridian
3 = filament between the two main spots and basically parallelto the solar equator
4 = filament surrounds a large spot, as an eyebrow at a distanceof less than half the diameter of the spot
5 = filament points between two spots that are very near to each other
Note: Ifregion,
more describe
than one filament
associatedwiththe one which
encodesby thethe spothighest code number thus implying the most importantfilament feature.

14 JUNE 1968 BOULDER
BRIGHT H‑a STRUCTURE

29 OCTOBER 1968 BOULDER
BRIGHT H‑a STRUCTURE

C .I. 1

SUNSPOTS

Code 3. USSPI
Introduction to the code USSPIThe gradient of the active centers magnetic field is really an important
point as far as the forecast of the flare activity is concerned: unfortunately
only a few observatories can make an estimate of the value of this gradient.
The purpose of this new code is to circulate a magnetic description of the
spotted active centers with a qualitative estimate of this gradient.
1. Classification of the spotted active centers
The classification which is used follows the philosophy of the Mt. Wilsonclassification, but it contains some slight improvements.
The a group is simply named "unipolar spots".
The Beta group has been divided into two classes: the "open bipolar spots
and the "closed bipolar spots". Some gradients of the latter class are higher
than the gradients of the former class.
These two last classes do not coincide exactly with the Mt. Wilsonclassification: some regions have the common feature of having more than
two main spots of opposite polarities and are named the multipolar regions.
Some of them can be reported as made up by the juxtaposition of several
unipolar and bipolar groups: sometimes this description follows exactly
the history of this region, sometimes it can be a purely arbitrary arrange‑
ment, but in any case the possibility exists for a description of the main
spots. This point is important. The last class is related to the complex
regions (bipolar or multipolar) which escape any reasonable analysis of themain spots, but the configurations can be reported daily.
2. Estimate of the higher gradients
These places have been reported as active configurations: two spots ormore of opposite polarities very close to each other (i. e. the distance
between the interior edges of the main spots is less than or equal to thediameter of the biggest spot). The most general situation consists of two
spots of unequal areas: the A configuration includes two spots of equal area,
and the B one is a limit situation with a large spot surrounded by several
tiny spots very close to its edge, these tiny spots being of opposite polarity(this configuration has been first recognized on chromospheric data as alarge round spot surrounded by a dark filament like an eyebrow and often
the spot companions do not exist). The Delta configuration appears whenboth spots are in the same penumbra and in this case the interest is mostly
related to the feature of the umbra.
The existence and place of these configurations must be reported inorder to specify and to achieve the magnetic description of the spotted
active centers.

Conclusion
It is known that the sunspot data are not sufficient in order todescribe exactly the magnetic features of an active center or of a region
but two comments can be given: the highest gradients always exist between
spots and the drawing of inversion lines between just sunspots is a usefulapproach to the real inversion line features.
The observers using this code must point out that this classification
is mainly a practical one. Sometimes one solar feature can be reported
through several classes or descriptions: it does not matter since theonly purpose is to issue a description which can help a solar astronomer
to follow the evolution of that region.
Please note that only spots with real measurement of the longitudinalcomponent will be reported (i.e. with a longitude less than 60°or 70° orwith a sufficient area).

SUNSPOTS
C. 1.1 Code3 (continued)

Code 3. USSPI
1. Content.
Sunspots classified by magnetic characteristics

3. Definitionof symbols.

USSPI = key word, SunSPots, code I
IIIII = station indicator (See lists in Part D.)
JJ = Greenwich date of observation
HH = hour UT of observation
G = quality of the seeing
1 = very good 4= good2 = poor 5= exceptional
3 = fairIf basically UNIPOLAR:
Q = quadrant (heliographic coordinates) in which geometriccenter of sunspot group is located
1 = NE (north‑east) 3= SW (south‑west)
2 = SE (south‑east) A= NW (north‑west)
XX = distance to central meridian in degrees
YY = heliographic latitude in degrees
K = key number
5 = isolated unipolar spot or large spot surrounded by small
companions of opposite polarity (B configuration).
a = Zurich sunspot class
18 == HA
9 = J
b = diameter of the main spot in degrees
c = magnetic polarity of the main spot
1 = north2 = south
3 = doubtful (related to its heliographic longitude)d = configuration
0 = not any configuration, i.e. single spot or all tiny spots
1 = several tiny spots of opposite polarity at a distance(configuration B)
2 = configuration B suspected according to chromospheric data
(dark filament surrounding the spot like an eyebrow).

C. 1.1 Code 3 (continued)
Q = quadrant (heliographic coordinates) of geometric centerof bipolar group
1 = NE (north‑east) 3= SW (south‑west)
2 = SE (south‑east) 4= NW (north‑west)
XX = distance to central meridian in degrees
YY = heliographic latitude in degrees
K = key number
6 = open bipolar ― that is the shortest distance
between the edges of the main
spots is equal to or greater thanthe diameter of the largest spot
7 = closed bipolar ― simple classical bipolar groupand the shortest distance between
the closest main spots is lessthan the diameter of the largest
spot in the groupa = Zurich sunspot class
2 = B 5= E
3 = C 6= F
4 = D 7= G
bb = longitude difference in degrees between exterior edgesof the main spots
c = number of five digit blocks used to describe configuration,
if any configuration exists, or X when this bipolar groupis a part of a multipolar region (see K = 8).
dd = shortest distance in degrees between the interior edgesof the closest spots of opposite polaritiese = diameter in degrees of the largest spot
f = orientation of the inversion line
1 = the inversion line is roughly parallel (<30°)to a
solar meridian and the two main spots are equivalent(Beta) or the leading spot is the larger (Beta P)
2 = the inversion line is roughly parallel (<30°)to a
solar meridian but the following main spot is thelarger (Beta F).
3 = the inversion line is tilted between 30° and 60°
to the solar equator and the two main spots areequivalent, or the leading spot is the larger(Beta and Beta P).
4 = the inversion line is tilted between 30° and 60°to
the solar equator but the following main spot is thelarger (Beta F).
5 = the inversion line is roughly parallel (^30°)to thesolar equator and the two main spots are equivalentor the leading spot is the larger (Beta and Beta P).
6 = the inversion line is roughly parallel (<30°)to thesolar equator but the following main spot is thelarger (Beta F).

1.1 Code 3 (continued)
g = description of the polarities
1 = the polarities are normal in relation to thehemisphere and solar cycle
2 = the polarities are normal but with many tiny spots
3 = the polarities are reversed in relation to thehemisphere and solar cycle
4 = the polarities are reversed but with many tiny spots
5 = the two polarities are nearly at the same longitude(see f = 5 or 6)
a CONFIGURATION exists
Q = quadrant (heliographic coordinates) of the geometriccenter of an active configuration ― that is two spots(or many more) of opposite polarities very near together(i.e. the distance between the interior edges of themain spots is less than or equal to the diameter of thebiggest spot) ― the best known is the Delta configuration
where two umbra of opposite polarities are in the same
penumbra (these are used to estimate the position of thehighest gradients of the longitudinal magnetic component)
XX = distance to central meridian in degrees
YY = heliographic latitude in degrees
K = key number
0 = description of active configurationh = type of configuration and orientation of the inversion line.
1 = a spotted configuration and the inversion line isroughly parallel G;30 °)to a solar meridian.
2 = a spotted configuration and the inversion line istilted between 30°and 60° to the solar equator.
3 = a spotted configuration and the inversion line isroughly parallel (<30 °)to the solar equator.
4 = a Delta configuration and the inversion line is roughly
parallel (<30 °)to a solar meridian.
5 = a Delta configuration and the inversion line is tilted
between 30°and 60 °to the solar equator.
6 = a Delta configuration and the inversion line is roughly(<30 °)parallel to the solar equator.
i = diameter in degrees of the west spot (the west umbra in a
Delta configuration)j = diameter in degrees of the east spot (the east umbra in a
Delta configuration)k = distance in degrees between the interior edges of the twopolarities (the two umbrae in a Delta configuration)
N. B. For two polarities nearly at the same longitude there
is no special order to report the spot or umbra diameters.

C. 1.1 Code 3 (continued)
If MULTIPOLAR region made up of SEVERAL UNIPOLAR OR BIPOLAR GROUPS:K = key number
8 = multipolar region which can be reported as composing
a set and configuration of unipolar and/or bipolargroupsaa = longitude difference in degrees between exterior edgesof the main spots
bb = number of five digit blocks used to report the groups andthe configurations
QXXYY Kabcd for
QXXYY Kabbc ddefg for
QXXYY Khijk foreach unipolar component as above
each bipolar component as above
each active configuration as above

If COMPLEX REGION:
Q = quadrant (heliographic coordinates) of geometric centerof multipolar group
1 = NE (north‑east) 3= SW (south‑west)
2 = SE (south‑east) 4= NW (north‑west)
XX = distance to central meridian in degrees
YY = heliographic latitude in degrees

K = key number
9 = complex multipolar region which cannot bereasonably reported as a set of groups
aa = longitude difference between the exterior edge of main spots
b = latitude difference between the exterior edge of main spots
c = number of five digit blocks used to report active configurations
QXXYY Khijk for each active configuration as above.

C. 1.1 Code 3 (continued)
SAMPLE OF REPORTS OF GROUPS, REGIONS AND CONFIGURATIONSJuly 7,1967 Isolated Unipolar Spot10720 58220
October 20,1958 Typical
30405 58321

B Configuration with a spotted eyebrow

May 29,1966 Classical Open Bipolar Group
40924 64120 07211
April 26,1966 Closed
43118 74062 02231

Bipolar Group with one active Configuration

February 24,1967 Complex Multipolar Region with at least four
active configurations
It is difficult to report the configurations in these data:
the biggest spot is a bipolar one and according to the inversion line
only part of this spot contributes to some active configuration or
the same place contributes simultaneously to two configurations
13624 91758 13823 03571 (a part of the biggest spot)
14224 04311 (a Delta configuration)
14522 02111 (a part of the biggest spot)
13124 02421
June 12, 1966 Closed Bipolar Group, being by itself a configuration
11322 74032 00255 11322 03220
March 30, 1960 Multipolar Region made up of two bipolar groups, beingby themselves two configurations
11512 81010 11714 7406X 00331 11411 7408X 03411
11714 02330 11411 01423
July 29, 1966 Closed Bipolar Group, being by itself a configuration
14724 74032 00211 14724 01210
September 17, 1966 a B Configuration which can alternately be reported
as a closed bipolar
13107 58421 or 13107 73052 00431 13106 02410
March 6,1967 Complex Region with a Delta configuration
24218 90952 24218 05217
July 6,1966 Complex Region with a Delta configuration
44235 91062 44335 06221
September 10, 1966 a Multipolar Region made up of two bipolar groups
with one configuration
34321 81208 34721 6407X 06111 34121 6405X 04111 34321 OHIOC. 1.1 Code 3 (continued)
September 20, 1966 Multipolar Region made up of one bipolar and one
unipolar group with one configuration
40906 80707 40907 58420 41004 6407X 04221 40806 02420
May 27, 1967 A

very impressive and exceptional Multipolar Region which infact can be reported with a reasonable accuracy
42726 82620 44025 58120 43322 6408X 06111 42826 6514X 08311
41827 7407X 01311 41830 7407X 02211 43224 03312 42017 04120
41727 01211

C. 1.2

SOLAR

FLARES

Code 1. UFLAH
1. Content.
Position, importanceand duration of solar flares as reported by asingle observatory(importancein conformance with the recommendationsof IAU Commission 10 as of January 1, 1966)

3. Definitionof symbols.

UFLAH = key word, solar FLAres, code H
IIIII = station indicator (See lists in Part D.)
JJ = Greenwich date of observationa = quality of observation
1 = very poor 4= good2 = poor 5= exceptional
3 = fairb = number of flares reported: 0 = ten or more, 1 = one to 9 = nine
K = last digit of check sum of all the following digits
Q = quadrant (heliographic coordinates) in which the flare is observed
1 = NE (north‑east) 3= SW (south‑west)
2 = SE (south‑east) 4= NW (north‑west)
XX = distance to central meridian in degrees
YY = heliographic latitude in degrees

.2 Code1 (continued)

c = indicator that time which follows is:
1 = beginning of flare, end of flare was observed
2 = beginning of flare, end of flare not observed
3 = first observation of a flare in progress, endof flare observed
A = first observation of a flare in progress, endof flare not observed
5 = time of last observation of flare (if used encode"fff" by slant lines
6 = time of maximum of flare
7 = time of secondary maximum of flare
8 = time of end of flare (if used encode "fff" by slant
lines)
9 = nominal time of beginning of a subflare
HHmm = time in hours and minutes (UT)
d = importance based upon "corrected" area in square degrees
0 = subflare (S); area <2.0 square degrees
1 = importance 1; area 2.1‑5.1 square degrees
2 = importance 2: area 5.2‑12.4 square degrees
3 = importance 3; area 12.5‑24.7 square degrees
4 = importance 4; area >24.7 square degrees
e = importance based upon relative intensity evaluation
7 = faint
8 = normal
9 = brilliant
fff = duration or period of observation of the flare, in minutes
depending on whether the indicator c in previous group is
1 or 2, 3, 4.
Note: As many times (cHHmm) as are significant may
be given to describe a flare, in order ofincreasing value of the time indicator c.
Also, a second (and third, etc.) flare in
the same region may be fully reported with‑out ambiguity without repeating the groups
UFLAH III1I JJabK QXXYY.

C. 1.2

SOLAR

FLARES

Code 2. UPATP
orCode 3. UPATV
1. Content.
Solar flare survey intervals
or visual only (V)3. Definition

for Ha patrols,

cinematographic

only

(P)

of symbols

UPATP = key word, flare PATrol hours, Photographic
or UPATV = key word, flare PATrol hours, Visual
IIIII = station indicator (See lists in Part D.)
JJ = Greenwich date of observation
U = overall quality of observations
0 = no data 2= poor 4
1 = very poor 3= fair 5
aa = check sum of all following digits= good= exceptional

bbb = UT of beginning of patrol period in hours and tenths of hours
cc = UT of end of patrol period, in hours and tenths of hours, withtens digit suppressed
Notes: 1. Repeat "UPATP (or UPATV) IIIII JJUaa" when‑ever observing period covers two (universaltime) dates.
ambiguity
possibleupon de‑codinginsertIfan extra
group"bbbcc".
2. UPATPUPATV
onlyand
if thetions orhave
beensent
reducedare flare
being observa‑
reportedin the same message.
3. The message is sent, of course, even if no flares
have been observed during the patrol period.

C.

1.3 CALCIUM

Code

1.

PLAGESAND

CENTERSOF

ACTIVITY

UPLAK

1. Content.
Area,

importance3. Definition

andintensityofcalcium

plagesof symbols.

UPLAK = key word, PLAges. code 1&
IIIII = station indicator (See Lists in Part D.)
JJ = Greenwich day of observation
HHH = time of observation in hours and tenths of hours UT
q = quality of observation on a scale from 1 to 5;
1 = very poor 4= good2 = poor 5= exceptional
3 = faird = number of days since last message from this stationx = always x (or slant bar in teletype aessages)
nn = number of plages (three five‑digit groups each)for which information will follow

C. 1.3 Code 1 (continued)
eee = serial number, assigned by observatory
f = importance of plage region on a scale of 1 to 3 combinedwith information on the stage of evolution

9 = eighth disk transit
X = no evaluation given
Q = quadrant (heliographic coordinates) containing the plage
1 = NE (north‑east) 3= SW (south‑west)
2 = SE (south‑east) 4= NW (north‑west)
XX = distance to the central meridian in degrees
YY = heliographic latitude in degrees
iii = area in millionths of the solar hemisphere, divided by
j = intensity
1 = (faint) 4= 2.5 7= 4
2 = 1.5 5=3 8= 4.5
3=2 6=3.5
9=5(very bright)
k = check, units digit of sum of preceding 14 digits

C. 1.4

SOLAR CORONA

Code 1. UCORE
1. Content.
Intensity
latitude

3. Definitionof coronalline

emissionas a functionof heliographicof symbols.

UCORE = key word, CORona, code E
IIIII = station indicator (See lists in Part D.)
JJ = Greenwich date of observation
HHH = time of observation in hours and tenths of hours UT
a = line observed (See key word COLOR below)
1 = green (A5303A) 3= red (A6702A)
2 = red (A6374A) 0= yellow (A5694A)
b = scattered light intensity (measure of observation quality)
1 = strong (>60 millionttis)or observation low quality
2 = moderate (30‑60 millionths) or observation moderate quality
3 = weak (<30 millionths) or observation high quality
qqq = quadrants of limb for which values are given in message
1 = NE (north‑east) 3= SW (south‑west)
2 = SE (south‑east) 4= NW (north‑west)‑ if all four quadrants insert 999; if fewer than three
quadrants, complete group with O's

C. 1.4 Code 1 (continued)
c = latitude (divided by 10) of intensity reported in dd
dd = intensity measured at latitude indicated by c (millionths divided
by ten)ee = intensity measured at next succeeding 5 °position angle ‑ proceed‑ing N‑E‑S‑W‑(millionths divided by ten) (See Note 1)
COLOR = more than one line reported, word signifies change of line being
reported
Notes: 1. Always give observations in order of increas‑ing position angle, i.e. N‑E‑S‑W. A groupgiving intensities at equator and poles isusually necessary to avoid ambiguity.
2. Usually enough measurements will be given tooutline the intensity peaks and usually onlyfor East limb, green and yellow line.
3. Intensity is measured as millionths of an
angstrom of the continuum of the center ofthe solar disk (at same wavelength as the line).

63c. 1.5 SOLAR

X‑RAYS

Code 1. USOXO
1. Content.
Background (or event) of solar x‑ray radiation measured by satellites.

3. Definitionof symbols.

USOXO = key word, SOlar X‑ray events, code 0^.
IIIII = station indicator (See lists in Part D.)
JJ = Greenwich date of observationa = satellite
0 = new satellite identified by plain language at end of message
together with number to specify satellite thereafter
4 = 1967‑73A (NRL data from 0G0‑4)
5 = 1967‑100A (data from 0S0‑4)
6 = 1968‑17A (SOLRAD 9)b = type of satellite readout
0 = real‑time
1 = from stored datac = last digit of check sum of all the following digits

C. 1.5 Code 1 (continued)
d = general aspect of the record
0 = no detectable radiation
1 = stable
2 = fluctuation: "hhi" gives mean level
3 = beginning of an increase: "hhi" gives level before increase
4 = definite increase in progress: "hhi" gives mean level
5 = definite decrease in progress: "hhi" gives mean level
6 = maximum: "hhi" gives maximum level
HHmm = UT hours and minutes of beginning of period reported by "d"(usually this will be beginning of satellite readout)e = number of groups to follow
HHmm = UT hours and minutes of end of period reported
f = band of adjusted (or actual) flux measurements
0 = 0.5‑3 Angstroms (sensor actually 0.5‑3 Angstroms)
1 = 1‑8 Angstroms (sensor actually 1‑8 Angstroms)
2 = 1‑20 Angstroms (sensor actually 1‑20 Angstroms)
3 = 8‑20 Angstroms (sensor actually 8‑16 Angstroms)
4 = 44‑60 Angstroms (sensor actually 44‑60 Angstroms)
Note: The above bands are for the existing and planned
SOLRAD sensors. For other satellites in the
future additional bands will be specified and theadjusted flux may equal the actual flux.
g = qualifier to "hh"0 = value on scale as given in "hh"8 = less than value given in "hh"9 = greater than value given in "hh"hh = flux in ergs cm‑2sec 1x10"1in units and tenths of units
i = exponent of 10 in group "hh"
1 = 1
2etc.
= 2

C. 1.6 Code 1 (continued)
3. Definitionof symbols.

UPART = key word, solar PARTicles
IIIII = station indicator (See lists in Part D.)
JJ = Greenwich date of observation
HH = hour UT of message
a = type of apparatus on which event observed
1 = neutron monitor
2 = detector carried by balloon
3 = riometer in auroral zone
4 = VHF ionospheric forward scatter in auroral zone
5 = earth satellite (i.e. 0G0, etc.)
6 = space probe (i.e.
Pioneer, etc.)
b = indicator describing time which follows
1 = beginning of event (the enhancement of the fluxof particles)
2 = event in progress at time of beginning of theperiod of readout
4 = following data sent during pre‑maximum of event,time corresponds to highest levels as yet recorded
6 = time of maximum of the event
9 = time of end of the event
HHmm = UT time in hours and minutes
If "a" was 3 or 4 (riometer or VHF ionospheric forward scatter observations)
ccc = absorption in tenths of dB (the greatest value of the available reports)
d = kind of solar particles
1 = protons
2 = relativistic electrons
3 = type of particles unknowne = extent of the event or number of reports involved
1 = local or just one report available
2 = small extent or a few reports available
3 = definite event or several reports available
If "a" was 1 (neutron monitor)
5 = always a five as key number
cccc = percent of increase of flux at the maximum
If "a" was 2 or 5 (balloon or satellite)
5 = always a five as key number
cccc = percent of increase of flux at the maximum
d = band of energy
7 = above the energy "eee"
8 = about the energy "eee"
9 = below the energy "eee"C. 1.6 Code 1 (continued)
eee = energy of reference expressed in Mev/ = always a slant line
If "a" was 6 (space probe)
5 = always a five as key number
cccc = percent of increase of flux at maximum
d = band of energy
7 = above the energy "eee"
8 = about the energy "eee"
9 = below the energy "eee"eee = energy of reference expressed in Mev/ = always a slant line
4 = always a four as key number
fff = corotation delay in tenths of days
g = sign of corotation delay
0 = + (westward around sun)
1 = ‑ (eastward around sun)Note: Message may repeat at "bHHmm ...." to give details of developmentof the event. If b = 1, 2 or 9, only group "bHHmm" given;
if b = 4 or 6, groups following "bHHmm" depend upon encodingof "a".

C. 1.7 SOLAR
Code

1.

WIND

PARAMETERS

USOLW

1. Content.
Solar

wind

3. Definition

velocity,

density,temperature,

corotationdelay

of symbols.

USOLW = key word, SOLar Wind
JJ = Greenwich date of observation
III = Space probe
006
007 == Pioneer
Pioneer 67 008
009== Pioneer
Pioneer 89
HHmm/ = time of readout, hours and minutes UT
1 = identifies solar wind velocity (km/sec)
aaaa = velocity in km/sec
2 = identifies density (cm‑3)
bbb = density in 3 significant figures, to be multiplied by 10̲cc = negative exponent of 10
3 = identifies temperature (106 °K)
ddd = temperature in 3 significant figures, to be multiplied by 10"
e = negative exponent of 10
4 = identifies corotation delay (days)
fff = number of days in tenths
g = sign of corotation delay
0 = + (westward around sun)
1 = ‑ (eastward around sun)PageII SOLAR

RADIO OBSERVATIONS

11.1 Flux Measurements
on DiscreteFrequencies
Code 1. URANO 72
11.2 Spectrographic
Observations
Code 1. URANZ 75
11.3 InterferometricObservations
Code 1. URALE 77
Code 2. URALS 79

C. II. SOLAR

RADIO OBSERVATIONS

C. II.1 FLUXMEASUREMENTS ON DISCRETE FREQUENCIES

Code 1. URANO
1. Content.
Solar radio outstanding events (and median flux, if desired) at any
fixed frequency

3. Definitionof symbols.

URANO = key word, RAdio Noise, code 0.
IIIII = station indicator (See lists in Part D.)

C. II.1 Code 1 (continued)
JJ = Greenwich date of beginning of period of observation
FF = radio frequency of observation to two significant figures inunits and tenths of units
G = power of ten to convert FF to MHz
i.e., 283 = 2800 MHz
281 = 28MHz
aa = UT hour nearest beginning of period of observations reported
bb = UT hour nearest end of period of observations reported
c = 0 to 9 for number of outstanding events reported
ddd = background flux (adjusted for burst) for period of observationin 10‑22Wm‑2Hz‑1
ee = nearest UT hour of background flux measurement
f = 9 to signify beginning of an event report
HHmm = UT hour and minutes of beginning of outstanding eventg = key to type of outstanding event
0 = minor burst (meter wave)
1 = simple (microwave burst)
2 = post burst increase (microwave burst)
3 = complex (microwave burst)
4 = group or fluctuation (microwave)
5 = major burst (meter wave)
6 = major plus (meter wave)
7 = onset of noise storm (or noise storm in progress) (meter wave]
8 = rise in base level
HHmm = UT hour and minutes of end of eventh = key to measurement of maximum flux of event in 10‑22Wm 2Hz‑1
5 = actual measurement
6 = saturated record
iii = actual peak flux of the event to three significant figures(expressed in hundredths of units) (if noise storm, use median flux)
j = power of ten to express iii in 10 'iZWm zHz 1
i.e. 3343 = 3340 units
3342 = 334 units
3341 = 33.4
units
3340 = 3.34
units
/ = always slant line
HHmm = UT hour and minutes of time of maximum
Note; Secondary maxima may be reported by additional"hiiij /HHmm" groups.

C. II.1 Code 1 (continued)
Groups "hiiij /HHmm" may be replaced without ambiguity by following
two groups.
k = key to measurement of maximum flux in terms of percent increase
7 = actual measurement
8 = saturated record
1111 = peak flux reported as percent of pre‑burst leveli.e., 0240 = 240% of pre‑burst level (preburst level = 100%)
1280 = 1280% of pre‑burst level/ = always slant line
HHmm = UT hour and minutes of time of maximum
Note: Secondary maxima may be reported by additional"kllll /HHmm" groups.

C. II.2 SPECTROGRAPHIC
Code

1.

OBSERVATIONS

URANZ

1. Content.
Eventobserved

3. Definition

on

sweep

frequency

recordsof symbols.

URANZ = key word, solar RAdio Noise, code Z
IIIII = station indicator (See lists in Part D.)
JJ = Greenwich date of observationa = number of phenomena reported
bb = power of ten to express "cc" and "ddd" in MHz
cc = lowest frequency to two significant figures of activity
ddd = highest frequency to three significant figures of activity
e = type of spectral activity
1 = noise storm = type I storm
2 = slow‑drift burst = type II
3 = fast‑drift burst = type III or decimeter fast drift burst
4 = broadband continuum = type IV
5 = brief period of continuum associatedwith fast‑drift burst = type V
6 = dekameter continuum associated with
type III burst storms
7 = storm of fast drift bursts = storm of type III bursts
8 = microwave burst = short (minutes) microwave continuum
usually of impulsive start
9 = slow drift feature = decimeter slow drift burst or type I
chain or gradual change in type III starting frequencies
RHmm = UT hour and minutes of beginning of activity

C. II.2 Code 1 (continued)
f = relative importance on scale of 1, 2 or 3 except
7 = importance 1+
8 = importance 2+
9 = importance 3+
HHmm = UT hour and minutes of end of activity

c.

II.3 INTERFEROMETRIC

Code

1.

OBSERVATIONS

URALE

1. Content.
Position,

3. Definition

maximum

intensity

and

flux

of

solar

radio

source.

of symbols.

URALE = key word, solar RAdio noise Location, Code E
IIIII = station indicator (See lists in Part D.)
JJ = Greenwich date of observation
HHH = time of observation in hours and tenths of hours UT
FF = radio frequency of observation to two significant figuresin units and tenths of units
G = power of 10 to express FF in MHz
a = type of observation reported
1 = single group for description (defff), which may be repeated
2 = two groups for description (QXXYY bbbcc), which may berepeated
K = last digit of check sum of following groups (or slant line)II.3 Code 1 (continued)
Q = quadrant (heliographic co‑ordinates) containing the noise source
1 = NE (north‑east) 3= SW (south‑west)
2 = SE (south‑east) 4= NW (north‑west)
XX = distance to the central meridian, in degrees
YY = heliographic latitude, in degrees
bbb = maximum intensity in tens of thousands of degrees Kelvin
cc = flux of region in 10‑22Wm‑2Hz‑i
d = importance on scale 0, 1, 2, 3 where 3 has the greatest importancee = angular location with respect to North‑South diameter at meridiantransit
1 = North, east 5= Central, east
2 = South, east 6= Central, west
3 = South, west 7= ‑ ‑ ‑ , east
4 = North, west 8= ‑ ‑ ‑ , west
fff = distance to N‑S diameter at meridian transit, in percent of the solar
optical radius (e.g. 075 = 75%, 125 = 125% of the radius).

C.

II.3

Code

2.

Code

2

URALS

1. Content.
Position,

3. Definition

3‑cm

flux,

flux

ratio

3‑cm

to

8‑cm

of

solar

radio

noise

source.

of symbols

URALS = key word, solar RAdio noise Location and Spectrum
IIIII = station indicator (See lists in Part D.)
JJ = Greenwich date of observation
FFF = total flux of sun on 8 cm in 10‑22Wm̲2Hz̲1a = angular location with respect to North‑South diameterat meridian transit
1 = north‑east 5= central‑east
2 = south‑east 6= central‑west
3 = south‑west 7=― ‑east4 = north‑west 8=― ‑westbb = distance to the North‑South diameter at meridian transit
in percent of radius
cc = distance to the East‑West diameter at meridian transit
in percent of radius
dd = 3‑cm flux of the region in 10 22Wm̲2Hz‑1
e = flux ratio 3‑cm to 8‑cm in 10 percent steps
1 = 10%or 0.10to9 = 90%or 0.900 = ^100% or 1.00
f = activity of the region
0 = no special comment 3= growing rapidly
1 = stable 4= eruptive
2 = variableg = description of the region on the record
0 = no special comment 4= high degree of polarization
1 = broad 5= not well isolated
2 = small size 6= during burst
3 = double shapedPn‑<
C. Ill IONOSPHERICOBSERVATIONS

III. I Critical Frequencies
Code 1. UFOFI 82
Code
11FOFO 8282
Code 2.
3・UFOFU111.2 SuddenIonosphericDisturbances
Codu 1. USIDO 85
111.3 IonosphericAbsorption
Code 1. UABSE 87

C. III.
C. III.l CRITICALIONOSPHERIC OBSERVATIONSFREQUENCIES

Code 1. UFOFI
Code 2. UFOFO
Code 3. UFOFU
1. Content.
Critical frequencies of F2 region (foF2) as a function of Standard
Meridian time (if code UFOFI) or Universal time (if code UFOFO or UFOFU)
Maximum and minimum values of foF2 and hour of occurrence
f‑min frequencies as a function of same times as given for foF2

C. III.l Code 1, 2 or 3 (continued)
3. Definitionof symbols.

JJ = local date of beginning of 24‑hour period reported if UFOFI or
Greenwich date of beginning of 24‑hour period reported if UFOFQ
or UFOFU
T = time indicator for approximate time of beginning of 24‑hour period
0 = 0000 4= 1200
1 = 0300 5= 15002 = 0600 6= 18003 = 0900 7= 2100
HH = hour of message
f = even hour indicator, give data for 0000, 0600, 1200 and 1800,
beginning with the appropriate hour after the date0 = 0000 hours 6= 12003 = 0600 9= 1800Note: Code UFOFU is the same as UFOFO except values will he given
for every two hours, Universal time, instead of every six
hours. The definition of "f" is extended as follows:f = even hour indicator, giving data for 0000, 0200,
0400, etc., beginning with the appropriate hour
after the date

ggg = value of foF2 (in tenths of MHz; report as 000 if symbols only
are applicable)
h = descriptive letter symbol (see Piggott and Rawer, URSI Handbookof Ionogram Interpretation and Reduction, 1961, for full infor‑
mation)
X = none (use slant line in teletype messages)
1 = A, blanketing sporadic E
2 = B, complete absorption
3 = C, equipment trouble
4 = D, frequency higher than equipment limit
5 = E, frequency lower than equipment limit
6 = F, spread echoes
7 = G, foF2 <foFl (report foFl in group "ggg" above)
8 = I or T, interpolated or smoothed value
9 = R, measurement influenced by, or impossible because of attenuationin the vicinity of a critical frequency
0 = any otherC. III.l Code 1, 2 or 3 (continued)
MAXMI = key word, indicating the following groups give MAXimuraand Minimum
foF2 during 24‑hour period reported
HH = nearest hour of maximum value
ppp = maximum value of foF2 in 24 hour period reported, in tenths of MHz
HH = nearest hour of minimum value
qqq = minimum value of foF2 in 24‑hour period reported, in tenths of MHz
EFMIN = key word, indicating f‑MIN data to follow
ii = f‑min in tenths of MHz for time of first "fgggh" group above
jj = f‑min in tenths of MHz for 6 hours later than "ii"kk = f‑min in tenths of MHz for 12 hours later than "ii"
11 = f‑min in tenths of MHz for 18 hours later than "ii"XX = always "XX" or slant lines in teletype
Notes: 1. In "iijjk kllXX" groups, "99" will signify
f‑min >9.9 MHz
2. If

symbol to be used for f‑min, encode as follows:
XI = A X3= C
X2 = B X5= E(The X's should be slant lines in teletype messages)

C. III.2 SUDDENIONOSPHERIC DISTURBANCES

Code 1. USIDO
1. Content.
Type of phenomenon (SWF, SEA, SCNA, SPA, SES, SFD>, time of beginning,
duration and importance.

3. Definitionof symbols.

USIDO = key word, Sudden Ionospheric Disturbance, Code 0
IIIII = station indicator (See lists in Part D.)
JJ = Greenwich date of observation
N = number of phenomena reported
HH = UT hours of message
a = type of phenomenon
0 = sudden frequency deviation, SFD
1 = typical S‑SWF (short wave fade out: sudden dropout)
2 = slow S‑SWF (short wave fade‑out: dropout taking 5 to
15 min and gradual recovery).
3 = G‑SWF (short wave fade out: fade irregular in both
dropout and recovery)
4 = SEA (sudden enhancement of atmospherics)
5 = SPA, phase advance (sudden phase anomaly)
6 = SCNA (sudden cosmic noise absorption)
7 = SES (sudden enhancement of signal at about 15 kHz)
8 = SPA, phase retardation (sudden phase anomaly)
Note: To"subjective
report SPA
by "degrees"thanimportance"
userathercode UABSE.
HHmm = hours and minutes (UT) of beginning of phenomenon

C. III.2 Code 1 (continued)
b = 9 signifies time of maximum
HHmm ■ hours and minutes UT of maximum of phenomenonc = importance of phenomenon
0 = importance 1‑ 7
= importance 1+
1 = importance 1 8= importance 2+
2 = importance 2 9= importance 3+3 ■ importance 3
dd = duration of phenomenon in minutes
if 99: duration equal to or greater than 99 minutese ≫ reliability of time
5 = beginning of phenomenon itself is not clear
6 = nominal time
7 ■ first observation
8 = beginning time less certain than 2 min.
9 ≫ beginning time accurate to nearest 2 min. or lessf = definiteness of phenomenon on recording
0 = questionable 3= reasonable
1 = possible 4= reasonably definite
2 = fair 5= definite

C. III.3

IONOSPHERIC

ABSORPTION

Code 1. UABSE
1. Content.
Ionosphericionospheric

3. Definition

absorption measurement
by riometer techniqueforward scatter or by VLF recordings

or byof symbols.

UABSE = key word, ionospheric ABSorption, code ￡.
IIIII = station indicator (See lists in Part D.)
JJ = Greenwich date of observation
T = type of measurement
1 = riometer
2 = forward scatter
3 = VLF phase advance (rarely retardation) ―requires use of group "dddHH" instead of group "ccXHH"
HH = hour of message UT

C. III.3 Code 1 (continued)
a = type of phenomenon
1 = SCNA (sudden cosmic noise absorption ‑ solar flareassociated normally reported by code USIDO)
2 = SPA (sudden phase anomaly ‑ solar flare associatedmay be reported by code USIDO)
3 = Aurora ‑ associated absorption
4 = PCA (polar cap absorption event) due to protons
5 = PCA (polar cap absorption event) due to relativistic
electrons
6 = noise storm of solar radio emission superposed on absorption
7 = slowly varying ionospheric absorption ‑ defines onset timeof magnetospheric sub‑storm at auroral zone stations near
the midnight meridian. (Eather and Jacka, Australian J.
Physics 19, 215, 1966).
HHmm = hours and minutes UT of beginning of phenomenonb = key number
9 = time of maximum to follow
HHmm = hours and minutes UT of maximum of event
Note: Group "bHHmm" used only when maximum time known.
cc = number of decibels of maximum absorption before hour indicatedby next HH (use this group if T = 1 or 2)
X = always an X (or slant line in teletype message)
HH = UT hour of the ending time of the event. If event still inprogress at time of message replace by slant lines.
ddd = phase advance (rarely retardation) in degrees (use this group
if T = 3)
HH = UT hour of the ending time of the event. If event still inprogress at time of message replace by slant lines.

Page
GEOMAGNETIC AND AURORAL ACTIVITY
IV. 1 Geomagnetic Activity
Code 1. IMAGE
IV. 2 Auroral Observations
Code 1. UAURE 92

C. IVGEOMAGNETIC AND AURORAL ACTIVITY

C. IV.1 GEOMAGNETIC

ACTIVITY

Code 1. UMAGE
1. Content.
Geomagnetic Ak index
Geomagnetic K‑indices for the period reported
Geomagnetic disturbances with time of occurrenceTime and value of minimum H‑component (optional)

3. Definitionof symbols.

UMAGE = key word, MAGnetic activity, code E
IIIII = station indicator (See lists in Part D.)
JJ = Greenwich date of beginning of 24‑hour period reported
TT = UT hour of beginning of 24‑hour period reported
a = last digit of check sum of following 10 digits
bb = Ak‑index for Greenwich date JJ (hundreds digit omitted).
(Note
not the at
24‑hourperiod put
reported,
T is 0.
If Akthisnot isavailable
observatory,
XX or unlessslant barin teletype message.)kkkkkkkk = K indices for the 24‑hour period reported

C. IV.1 Code 1 (continued)
c = indicator telling the time reported in HHmm is
1 = storm end 6= gradual storm beginning
2 = bay (psc) 7= sudden storm commencement (ssc)
3 = typical crochet 8≫ very marked sudden storm
4 = provisional figures commencement(ssc)
HHmm = UT hour and minute of phenomenon indicated by c. (If c = 4,
HHmm used for reporting up to four additional 3‑hour periods
following the 24‑hour interval reported by the "k's".)
Optional groups
d = 5 signifies time to follow refers to absolute value of minimum
reached on horizontal component
HHmm = time of minimum in hours and minutes UTeeeee = intensity of minimum expressed in gammas
Note: Use groups "dHHmm" and "eeeee" only for stations
where such a measurement is a good approximationof Dst, i.e. Fredericksburg.

C. IV.2

AURORALOBSERVATIONS

Code 1. UAURE
1. Content.
Occurrence, principal forms, activity, brightness and color
aurora as functions of time and place of observations
Quality of observations
and cloudiness3. Definitionofof symbols.

UAURE = key word, AURoral observations, code ̲E
IIIII = station indicator (See lists in Part D.)
JJ = Greenwich date of message
a = type of message
1 = warning
2 = survey
HH = hour of end of observation in UT
bb = Greenwich date of warning or beginning of observations
HH = UT hour of warning or of beginning of observations
d = tens of minutes after HH for warning or number of five digit
groups "efghi" to follow if survey message

C. IV.2 Code 1 (continued)
e = type of aurora during the first hour0 = no observation
1 = no aurora
2 = veil
3 = pulsating patches
4 = homogeneous bands in the north
5 R homogeneous bands near zenith
6 = homogeneous bands in the south
7 = forms with typical ray structure
8 = combination of bands and rays without pro‑nounced motion
9 = combination of bands and rays with rapid
motion over a great part of the sky
f = brightness and color of aurora during the first hour0 = no observation
1 = color uncertain (because of other lights,
moonlight, dawn, etc.)
2 = faint yellowish green
3 = moderate yellowish green
4 = bright yellowish green
5 = faint yellowish green with red
6 = moderate yellowish green with red
7 = bright yellowish green with red
8 = faint red only
9 = bright red onlyg = quality of observations and cloudiness during thetwo hours covered by "ef" and "hi"0 = cloudy
1 = occasional observation and semi‑cloudy
2 = occasional observation and almost clear
3 = occasional observation and clear
4 = periodical observation and semi‑cloudy
5 = periodical observation and almost clear
6 = periodical observation and clear
7 = continuous observation and semi‑cloudy
8 = continuous observation and almost clear
9 = continuous observation and clear
h = type of aurora as in "e" above, during the secondhour or "0" if warningi = brightness and color of aurora as in "f" above
during the second hour or "0" if warning

C. IV.2

Code

1 (continued)

Notes:

1.

In
the first "efghi" group "ef" refers to time in‑terval HH to HH+1 and "hi" refers to the timeinterval HH+1 to HH+2. In
the second "efghi"
group, "ef" refers to the time interval HH+2 to
HH+3 and "hi" to the time interval HH+3 to HH+4
and so on to the last "efghi" group.

2.

The observer should be able
formation is most importantinterval.

to judgefor eachwhich in‑one hourPage
COSMIC RAYS
Daily Cosmic Ray Data
Code 1. UCOSE

c. V.

COSMIC RAYS

C. V.l DAILYCOSMIC RAY DATA

Code 1. UCOSE
1. Content.
Bi‑hourly flux values of cosmic rays, daily variations, special
events (based on code RAYCO)

3. Definitionof symbols.

UCOSE = key word, COSmic rays, code E
IIIII = station indicator (See lists in Part D.)
JJ = Greenwich date of first period for which flux values are given
T = type of apparatus
0 = neutron monitor (IGY Simpson type)1 ≫ high counting rate neutron monitor (IQSY type)
2 = meson monitor (IGY‑type)
3 = meson monitor (IQSY‑type)
4 = telescope, no shielding
5 = ionization chamber
HH = UT hour of message (normally in Greenwich day following thedate of "JJ")C. V. 1 Code 1 (continued)
a = type of variation during the day
0 = normal daily variation
1 = beginning of a pre‑decrease (pre‑baisse)
2 = pre‑decrease (pre‑baisse)
3 = commencement of a Forbush decrease
4 = Forbush decrease
5 = recurrent activity
6 = increase
7 = after‑effect of increase
8 = daily variation of large amplitude
9 = daily variation of anomalous phaseb = sign of daily variation
7 = negative
8 = zero
9 = positive
ccc = average deviation expressed in steps of thousandths of anarbitrary mean level

2. Ground level increases should be reported by
Code C.I.6. UPART.
HH = hour indicator; deviation of flux from the normal value follow‑
ing with "ddd" refers to the interval HH‑1 to HH+1 hours; if thedeviation is positive 30 is added to the hour to obtain HH.
ddd = deviation of cosmic ray flux from level expressed by steps ofthousandths of an arbitrary mean count.

SPECIALIZED NETWORKS
VI.I Radio Propagation Forecasts
Code 1. FORDA
Code 2. FORWE
Code 3. AD‑‑‑
VI.2 Radio Propagation Indices
Code 1. PROPO
Code 2. PQA‑‑
VI.3 Detailed Ionospheric Data
Code 1. ION‑‑
VI.4 SPARMO Balloon Measurements
Code 1. UCOSD

C. VISPECIALIZED NETWORKS

C. VI. 1 RADIO

PROPAGATION FORECASTS

Code 1. FORDA
1. Content.
Daily radio propagation forecast for different radio circuits between
Germany and certain areas of the world

3. Definitionof symbols.

FORDA = key word, FORecast Daily, code A
IIIII = station indicator
31503 = RWC Darmstadt
JJ = Greenwich date of issue of forecast
T = time of issue in tenths of day
FF = Greenwich date of begin of the 24 hour period to which
the forecast refersa = circuit
1 = North America
2 = South America
3 = East Asiab = expected quality figure for beginning of next night periodc = MUF for corresponding night period
1 = normal
2 = higher than normal and increasing
3 = higher than normal and decreasing
4 = lower than normal and increasing
5 = lower than normal and decreasingd = LUF for corresponding night period
1 = normal
2 = higher than normal and increasing
3 = higher than normal and decreasing
4 = lower than normal and increasing
5 = lower than normal and decreasinge = expected quality figure for end of night period

C. VI.1

Code

I (continued)

f = expected quality figure for beginning of nextg = MUF for corresponding
day period
1 = normal
2 = higher than normal and increasing
3 = higher than normal and decreasing
4 = lower than normal and increasing
5 = lower than normal and decreasing
h = LUF for corresponding
day period
1 = normal
2 = higher than normal and increasing
3 = higher than normal and decreasing
4 = lower than normal and increasing
5 = lower than normal and decreasingi = expected quality figure for end of day periodj = always a slant line in teletype message
Notes: 1.

The

day period

scale of quality figures is from 1 to 9, where
1 = useless
5 = fair
2 = very poor
6 = good (normal)
3 = poor
7 = very good
4 = poor‑to‑fair
8 = superior
9 = excellent

2. Thequalityconditions,forecasts.

figures give deviations from normal
which are predicted in the monthly

3. As day period is considered the period in whichusually the day frequencies can be used; asnight period is considered the period in whichusually the night frequencies are to be used.
4. Forevery forecast period two quality figures
are given in order to indicate the expecteddevelopment of conditions during the forecast
period.

c. VI.1

RADIO

PROPAGATIONFORECASTS

Code 2. FORWE
1. Content.
Weekly radio propagation forecast for different radio circuits between
Germany and certain areas of the world for the following ten days

3. Definitionof symbols.

FORWE = key word, FORecast Weekly, code E
IIIII = station indicator
31503 = RWC Darmstadt
JJ = Greenwich date of issue of forecast
T = time of issue in tenths of day
FF = Greenwich date of beginning of the first 24 hour period
to which the forecast refers
CC = circuit (or group of circuits) to which the following 5 digit
groups refer
NA = North America EA= East Asia
SA = South America EU= Europe
III = always slant lines in teletype messagea = expected quality figure for the day period starting with date FF
b = corresponding day period MUF
1 = normal
2 = higher than normal
3 = lower than normalc = corresponding day LUF
1 = normal
2 = higher than normal
3 = lower than normal

C. VI.1 Code 2 (continued)

expected quality figure for the night period starting with date FF+1
corresponding night period MUF
1 = normal
2 = higher than normal
3 = lower than normal
Similar"abcde"groups inrepeatedfor each of the following
nine days,
ten groups
all.

Notes: 1.

The quality figures give deviations from normal
conditions, which are predicted in the monthly
forecasts. (See FORDA.)

2. As day period is considered the period in whichusually the day frequencies can be used; asnight period is considered the period in whichusually the night frequencies are to be used.
3. Each night‑time period is reckoned to follow
the respective day‑time period. For circuits
to the West from Germany, it may therefore
start on next Greenwich date.

c.

VI.1 RADIO

Code
I.

3.

AD

PROPAGATIONFORECASTS―‑

Content.
Forecastfor

3. Definition

coming7

day

periodof symbols.

AD = ADvance forecast
a = circuit, or combination of circuits
H = high northern latitude
J = combination of circuits
JJ = date of beginning of seven‑day period to which forecast applies
bb = date of ending of seven‑day period to which forecast applies
ccccccc = forecast quality figures for each of the seven days of the periodd = check, units digit of sum of preceding 11 digits
ee = date of beginning of disturbed period
ff = date of end of disturbed periodg = check, units digit of sum of preceding 4 digits

C. VI.2

RADIO

PROPAGATION

INDICESfor certain

radio

Code 1. PROPO
1. Content.
Radio propagation
indices
at the observatory

3. Definition

circuits,

monitoredof symbols.

PROPO ‑ key word, PROPagation conditions, code Q̲
IIIII = station indicator
31514 = station Luchow
JJ = Greenwich date of begin of the 24 hour period to which the
propagation indices apply
X = always an X (or slant line in teletype message)zz = last two digits of check sum of all the following digits
a = circuit
monitored
1 = U.S.A.
(Eastern part)2 = South America
3 = East Asia
4 = Canada
5 = India
6 = South Africa
bb = propagation index referring to day‑time, in steps of 0.2 ona scale from 0.0 ‑ 9.8 where 6.0 = normal
cc = propagation index referring to night‑time, according to thesame scale as "bt"Notes: 1.

The definition of day and night periods isthe same as given in the FORDA code.

2. The scale of the propagation index corresponds
to that of the quality figures as used in fore‑casts (FORDA code). The indices are evaluatedto the nearest fifth of a unit. Conditions are"normal" (index = 6.0) if they correspond to theaverage of the preceding 27 days (1 solar rota‑tion) .
Ref. A. Ochs and B. Beckmann: On the 27 days'recurrence tendency of radio propagation dis‑turbances in the period of high solar activity
in: The Effect of Disturbances of Solar Origin
on Communications (ed. G. J. Gassmann), pp.
235‑244, AGARDograph 59, Pergamon Press 1963.

C. VI.2 RADIO

PROPAGATION INDICES

Code 2. PQA‑‑
I. Content.
Preliminary daily propagation quality figures

3. Definitionof symbols.

PQ = key for Preliminary daily Quality figure reporta = circuit
A = Atlantic circuits
JJ = Greenwich date of beginning of 24 hour periodbcde = preliminary quality for each of the periods of the day, whereb refers to 1800 ‑ 2400
c refers to 0000 ‑ 0600
d refers to 0600 ‑ 1200
e refers to 1200 ‑ 1800
f = check, units digit of preceding 6 digits

C. VI.3 DETAILED
Code

1.

1. Content
All

ION

IONOSPHERIC

DATA

―
■

purpose

3. Definition

ionosphericcodeof symbols.

ION = key word IONosphereaa = station indicator (two letter identification from IQSY Notes No. 11)
PO = South Pole MW= MawsonMI = Mirny HB= Halley Bay
EL = Ellsworth VO= Vostok
WL = Wilkes DU= Terre Adelie
BD = Byrd QM= Sanae Basebbbbb = ionospheric characteristic reported
FOFTO = foF2 HIFTO= h'F2
FOFON = foFl HIFFF= h'F
FOEEE = foE HIEEE= h'E
FOESS = foEs HIESS= h'EsEFBES = fbEs EFMIN= f‑minMUFTO = M (3000)F2
MUFON = M (3000)F1
cc = beginning date of observations reported (individual hourly values)or= month; 01 = Jan., 02 = Feb., etc. (monthly median values)

C. VI.3 Code 1 (continued)
d = types of values
0 = hourly values within a 24‑hour period (Standard MeridianTime)
9 = monthly median values (Standard Meridian Time)
8 = values at 6‑hour intervals for a period of more than 24hours starting on date "cc"Note: In reporting a week's data, start with 00
hours on Monday (Standard Meridian Time)
7 = values at 6‑hour intervals, from scheduled ionograms
taken on hour nearest to Local Mean Time
Note: By arrangement, Universal Time may be usedinstead of Standard Meridian Time.
ee = number of groups of data of characteristic "bbbbb" which follow
f = even hour indicator: (See Table 1, below)

ggg = value in usual units, e.g. tenths of MHz (report as 000 if symbol
only applicable)

C. VI.3 Code 1 (continued)
h = symbol (list A, below)

i = odd hour indicator (Table 1, above)
jjj = valuek = symbol (See list A, above)
11111 = sum of all "ggg" and "jjj" values in preceding groups

C. VI.4

SPARMOBALLOON

MEASUREMENTS[Cosmic rays and x‑rays by balloon measurements‑‑ used bySolar Particles and Radiation Monitoring Organization(SPARMO)]
Code 1. UCOSD
1. Content.
Special events, detectedby particle
by stratosphericballoons

3. Definition

and radiation

detectorsof symbols.

UCOSD = key word, COSmic ray balloon observation, code D.
IIIII = station indicator (See lists in Part C.)
JJ = Greenwich date of observation
M = type of monitor flown
1 = SPARMO standard detector with 1 GM counter
2 = SPARMO standard detector with 2 GM counters
3 = SPARMO standard detector with 3 GM counters
4 = SPARMO scintillation detector
5 = other kinds of detectors// = always two slant lines

carriedC. VI.4

Code

1 (continued)

A = type of alert
1 = PROTONALERT
4 = AURORALERT (local auroral alert)
2 = MAGALERT
5 = ROUTINE
3 = RECURALERT
HHmm = launching time UT (hours and minutes)
type of event
7 = solar x‑rays
8 = proton events (see also C.I.6 ‑ UPART)HHmm = beginning time of event UT (hours and minutes)
i = intensity at maximum of event measured on the most sensitive
channel0 = 0.1 to 1
times the normal level (10% to 100%)
1=1
to
10
times the normal level (100% to 1000%)
2 = 10 to 100 times the normal level (1000% to 10,000%)
3 = 100 to 1000 times the normal level (10,000% to 100,000%)
4 = greater than 1000 times (>100,000%)
HHmm = time of maximum intensity UT (hours and minutes)
DDD = duration of event in hours and tenths of hours
dd = duration of reception in hours
Notes: 1.

If no event or phenomenon occurs, write thecorresponding group with XXXXX (or slant
lines on teletype).

2. If several events occur during a flight,
groups THHiran,
iHHmm, DDDdd will be repeatedas often as events, but, in this case, "dd"will be written as "XX". "dd" will be written
in hours after the last event at the end ofreception.
3. Theamplitude
event
will always
becalculated
on of
the themostsensitive
channel.
Special Note: The above code is identical with UCOSB of
Circular Letter RWC‑92 except the groups "UCOSB JJMII"
have been replaced by "UCOSD IIIII JJM//". If UCOSB isused, the station indicator is "II" encoded as follows:
14 = Sodankyla
20 = Buenos Aires
30 = Kiruna
43 = Reykjavik
46 = Roi Baudouin
53 = Utrecht

71 = Lindau
74 = Potchefstroom
75 = Aires/Adour
76 = Port aux Francais
94 = Dakar

PART D LISTSOF STATION

The indicatorgroupa = octant"IIIII"

INDICATORS

is constructed

as follows

in order"abcde"of world

100°west, northern hemisphere 180°west, northern hemisphere 100°east, northern hemisphere 180°east, northern hemisphere 100° west, southern hemisphere 180° west, southern hemisphere 100° east, southern hemisphere 180° east, southern hemisphereb ≪ tens

positionof longitude

if a = 1, 3, 5 or 7

if a = 2, 4, 6 or 8c = tens

positionof latitude

dd ‑ station number within position "abc" (arbitrarily
assigned by IUWDS)

i.e. Boulder,
N40 W105
becomes
Boulder,Colo.
Colo. ESSA
Universityof Colo.
N4020401
W105becomes20402

PART D. I. STATIONS
Indicator

10401 10402
10501 10502
10503 12101
12601
12301

AND INDICATORS IN NUMERICAL ORDER

Ge o gr aph ic a1 Loc

Bordeaux
Aires/Adour
Abinger
He r stmonc eux
Jodrell Bank
Dakar
Reykjavik
Canary Is.

at ionFranceFranceUK
UK
UK
SenegalIceland17201

Narssarsuak Greenland
Paramaribo Surinam
St. John's Nfld Canada
TrinidadWest Indies
Ramey AFB
Puerto Rico

17202 17401
17801

Arecibo
Puerto Rico
Sagamore Hill Mass. USA
Thule Greenland

14601 15101
15501 16101

18401 18402
18403 18404
18405 18406
18407 18408
18501 18502
19501 19601
19701 20301
20302 20401

Coordinates

Codes

N45 W01 N44
WOO N54
W02 N51WOO N53
W02 N15W17 N64
W21 N28
W16

URAN
UCOS
UMAG
UFLA,UPAT,USSP
URAN
UCOS, UFOF
UCOS
UFLA, UPAT, URAN, US
ID
UFOF
URAN, US ID, UFOF UFOF

N61 W55
W45 N47
N06
W52 NIO
W61 N18W67
N18 W67 N42
W70 N76
W68

Washington NASA D.C. USA
N38 W77
Washington NRL D.C. USA
W77
Fredericksburg
Va. USA
W77
McMath‑Hulbert
Pontiac,Mich.USA Ottawa W83
Dominion Obs. Canada
Ottawa NRC Canada
Ottawa CRC Canada
Penn State U. Pa.
USAor Univ. Park
Deep River Ontario
CanadaGreat Whale Canada
Aberdeen S.
DakotaChurchill Canada
Resolute Bay Canada
Ft. Davis Texas
USA
Houston Texas
USA
ESSA, Boulder Colo.
USA

N45 W76 N45
W76 N45
W76 N41W78
N46 W77 N55
W77 N46
W98 N58
W94 N74
W94 N31
W104 N30
W105 N40
W105

20402 21301

U. of Colo. Boulder,Colo.USA Sacramento
N40 W105
Peak N. Mex. USA
W105

21302 21401

White Sands N.
Climax Colo.

21501

Saskatoon

Mex. USA
USA
Canada

N38
N38
N42

N32

N32 W107 N39
W106
N52 W106US ID
UFLA,UPAT,
UPLA,USSP
URAN
URAN, URAL
UABS,UCOS,
UMAG, UFOF
US ID
USOX
UMAG
UFLA,UPAT,UPLA
USSP,USID
UFLA, UPAT, UMAG URAN
UFOF
URAN

UCOS
UABS
USOX
UABS
UABS,UFOF
URAN
UFLA, UPAT, URAN UFLA
UPAT, URAN, USS

URAN.USID
UFLA,UPAT,USSP.UCORUS ID, UFOF
UFLA,UPAT,
UCOR,UCOSUAUR

D. I. (continued)
Indicator
22301
22302
22303
22304
22401

Geographical

Location

CoronaCalif.

Lockheed

Burbank

Cal.

Los

Angeles

Calif.

Mt.

WilsonCalif.

Palo

Alto

22501
23601
25601
25602
26201
26202
26203
26204
26701
28701
30201
30401
30402
30501
30502
30503
30504
30505
30506
30507
30508
30509
30510

USA
USA

USA Calif.
USA B.C.

Penticton

Cana d a A l a s k a

Sitka

USA Alaska

Anchorage

CollegeUSA

AlaskaHonolulu

HawaiiUSA

Haleakala

Hawaii

USA

Maui

NBS

HawaiiUSA

HawaiiUSA

AlaskaUSA

Barrow
Cape

Schmidt

USSR

Tamanrasset

Algeria

Pic‑du‑Midi

FranceTortosa

Spain

Bagneux

FranceBretigny

FranceChambon‑la‑ForetFrance

DeBiltNetherlands

Dourbes

Belgium

GarchyFranceKootwijk

Netherlands

MeudonFranceNan^ayFranceNera

Netherlands

Poitiers

30511
30512
31401
31402
31403

Uccle
Anacapri‑G

Italy

Anacapri‑S

Italy

Arcetri

Italy

Bologna

Italy

Catania

Italy

Rome

Italy

31406
31501

Arosa

Switzerland

31502

Berlin‑Adlershof

GDR

31404
31405

Breisach GFR

31503
31504

Darmstadt GFR

Codes

N34 W118
N34
N33 W118
W118

US ID,URAN
UFLA, UPAT
UFLA,UPATUSSP, URAL
USSP
URAL
URAN
UMAG

N31 W118
N37 W122
N49 W120
N57 W135
N61 W150
N64 W147

USA

Maui

Oahu

Coordinates
USA

N21 W158
N20 W157
N20 W157
N21 W158
N71 W157
N69 W179
N22 E05
N43 E00
N41 EOO
N49 E02
N48 E02
N52 E05
N50 EOSN47 E03
N52 E06
N49 E02
N47
N52 E02
E05

N46 EOO
N50 E04
N40 E14N40
N43 E14Ell
N44 Ell
N37 E15
N42
N46 E12E09
N53 E14
N48
N50 E07
E09

USID,UABS,
UMAG, UPART
UABS,UFOF,UMAG
UAUR.USID
US ID
UFLA,UPAT,USSP
UABS,USID,UFOF
UFLA,UPATUMAGUFOF
USID,UMAG,UFOF
UCOR.UCOS
UFLA,UPAT,USSP.
UFOF, UMAG
US ID
US OX
UMAG
UFOF
UMAG
UMAG
UFOF
UFLA, UPAT,UPLA U
URAL
UFLA,UMAG,UPAT,
URAN, USSP,URAL,

US ID,UFOF
UFLA, UPAT
UFLA,UPAT
UFLA,UPAT
UFLA,UPAT,USSP,USOXUC OS,URAN
UFLA, UPAT,USSP U
ID
UFLA,UPAT,USSP,UCORURAN
USID,UFOF
USID,ADV,FORD. I. (continued)
Indicator
31505
31506
31507

Geographical

Location

Furstenfeldbruck

GFR

Juliusruh/Ruegen
Kanzelhohe GFR

GDR

Coordinates

Codes

N48 Ell
N54 E13
N46 E14

UMAG
UFOF
UFLA, UPAT,USSP,UCOR
URAN, UCOS
UCOS
US ID
US ID, UFOF, UCOS
USSP
UFLA, UPAT, USSP
PROP
US ID
UFLA,UPAT,
URAN,USSP
US ID
UCOS
UMAG,UFOF
URAN
URAN
UFLA, UPAT,UC OR, USSP
UMAG
UMAG
UFLA, UPAT, USSP UABS

31508
31509
31510
31511
31512
31513
31514
31515
31516

N54 E10
N48 Ell
N54 E12
N51 E10N46
N46 E15
E09

31517
31518
31519
31520
31521
31522

N51
N47 E15E12N50 E14
N52 E13
N48 E10
N47 E12

31523
31524
31525
31801
32001
32401
32402
32403
32501
32502
32503
32601
32602
32603
32604
32605
32606
32701
32702
33301
33401
33402

N53 Ell
N53 E13
N50 E15

WingstWitteveeri

GFR
Netherlands

ZurichSpitzbergen
Bangui

Switzerland
N47 E08
Norway‑N78 E15
CentralAfrican Rep. Greece

N04 E19
N38 E23

AthensBelgrade
Thessalonika
Budapest

Yugoslavia
GreeceHungary

Lomnicki
Skalnate
Emmaboda
Enkoping

Czechoslovakia
Czechoslovakia
Sweden

St it
Pleso

Lycksele
Nurmijarvi
Stockholm

SwedenSwedenFinlandSwedenUppsalaAndenes

SwedenNorwayKirunaHe lwan
Bucharest

SwedenEgypt

Simferopol

N54 E09
N53 E07

RumaniaUSSR

N45 E20
N41 E23
N47
N49 E19E20
N49
N60 E20E17
N60 E17
N65 E19
N61 E25
N59 E18
N60 E18
N69 E16
N68 E20
N30 E31
N44 E26
N44 E34

UMAG
UFLA,UPAT,USSP,
USID,URAN
USSP
UFLA,UPATUFOF
UCOS, UAUR
USSP
UFOF
USID,UAUR
UFOF
UFOF,UMAG,UABS
UFLA,UPAT,
URAN,USIDUFOF
UCOSUABS,UFOF,UCOS
UMAG
UFLA,UPAT,USSP
UFLA,UPAT,USSP,
URAN,UMAG

D. I. (continued)
Coordinate:

Codes

33501
33601
33701
33702
33703
34101
34401

N50 E30
N60 E31N69E27
N68 E33

UFOF
UFOF
UCOS
UMAG, UFOFUAB S,UFOF, UMAG UFOF

34402
34501
34502

N43 E42
N50 E37
E36
N55

34601
35401
36401
3 7401
37701
38101

N65 E40
N36 E52
N37
N41 E58
E70
N66 E66
N10 E77

Indicator

Geographical

Location

N67 E27
N12 E43
N41 E43

N17 E78

38201
38301
38401
38701
40501

N28 E77
N43 E77
N74
N52 E81
E104

42101
42102

N14
N14 E121
E121

42201
42202
42301
43301
43401

N16 E120
N25 E121
N29 E128
El 16
N26

43501
43601
43701
44301
44401
44402
44403
44404

N48 E135
N62 E130
N71 E129
N35 E137
N36
N36 E141
E140

44405
44406
45601

N43 E132

N36 E140
E139
N36
Mt. Norikura
Tokyo
Magadan

Japan
Japan
USSR

N36 E138
N36 E140
N60 E151

UFLA,UPAT,USSP,URAN
URAN,USSP,UPLA
UFLA,UPAT
UFLA, UPAT, URAN, USI

UMAG
UFLA,UPATUFOF
UFLA,UPAT,USSP
UFOF
UFLA,UPAT,USSP,
USID,UFOF,UMAG
UFLA,UPAT
US ID
UFOF
UFOF
UFLA,UPAT,USSP,
URAN, UFOF, ADV
USSP
UFLA,UPAT,USSP,
US ID, URAN, UFOF USSP
UFOF
UFLA,UPAT
US ID, UFOF
UFLA,UPAT,USSP, URAN
UFOF
UMAG, UFOF
UCOS
URAN
URAN,USID
UMAG
UFOF,ADV
UFLA,UPAT,USSP,URAN
UC OR, UCOS
UCOS
UFOF

D. I. (continued)
Indicator

Geographical Location

Coordinates

Codes

56301
56302
56303
57101

Buenos Aires Argentina
San Miguel Argentina
Tucuman Argentina
Huancayo Peru

S35 W58
534 W58
526 W65
S12 W75

URAN, UCOS
UFLA,UPAT,USSP
UFOF
UFLA , UPAT, US ID, UMA
UFOF
UAUR,UABS
UFOF
UABS
UFLA,UPAT,UFOF
UABS
URAN, UFOF
UCOS
UFOF
UFOF
UCOS,US ID,
UFOF,UMAG
UFOF
UFLA,UPAT,
URAN.USID
UFOF
UMAG
UFOF
UFOF
US ID, UMAG, UFOF
UFOF
UFOF
UFOF
UFOF,USID,UMAG
UFLA,UPAT,URAN,
USID,USSP
URAN,URAL
US ID, UMAG, ADV, (URA
Planned)
UFOF
UFOF
UFLA,UPAT,USSP
UABS

70901
72301
72701
73001
73301
75201
76701
77501

S79 W120
518 W150
S90 E00
S3 4 E18
S70 E24502 E28527 E27
S20 E48
S68 E63
S49 E70

79101
81201

S12 E97
S25 E114

81701
82301
82302
84001
84701
85101
85201
85301
85302
85303

S66 E110
S32 El 16
S32 El 16
503 E141
S66 E141
S09 E147
519 E147
S27 E153
535 E149
S30 E149

62801
65201

85304
85305

Sydney (Fleurs) Australia
S34 E151
Sydney(IPSD Balmoral)Australia Hobart
S34 E151
Australia

85401
87301
87401
87801

Norfolk Island
Wellington N.Z.
McMurdo Antarctica

S43 E147
S29 E168
S41 E175
S77 E166

PART D. II. STATIONS
StationAND INDICATORS IN ALPHABETICAL ORDER
Indicator

Abastumani
34401
Aberdeen
19501
Abinger
10501
Aires/Adour
10402
38401
Alma Ata
31401
Anacapri‑G
Anacapri‑S
31402
Anchorage
25601
Andenes
32701
Arcetri
31403
Arecibo17202
34601
Arkhangelsk
Arosa
31501
Ashkhabad
36401
Athens
32401
42201
BaguioBagneux
30501
Bangui
32001
Barrow
26 701
Belgrade
32402
Berlin H. Hertz
31502
Bologna
31404
Bordeaux
10401
Boulder ESSA
20401
Boulder U. of Colo. Breisach
20402
31503
Bretigny
30502
Brisbane
85301
Bucharest
33401
Budapest
32501
56301
Buenos Aires
Burbank (Lockheed) Byrd
22301
62801
StationCanary Island
12301
Canberra
85302
28701
Cape Schmidt
Capetown
72301
Carnarvon
81201
Catania
31405
Chambon‑la‑Foret
30503
19601
Churchill
Climax21401
25602
College
Cocos Island
79101
Corona22301
Culgoora
85303

Station
Dakar
Darmstadt
DeBiltDeep RiverDixon
Dj ibouti
Dourbes
Emmaboda
Enkoping
Fredericksburg
Ft. Davis
Freiburg
Furstenfeldbruck
GarchyGnangara
Great Whale
Helwan
Herstmonceux
Hiraiso
HobartHonolulu
HoustonHuancayo
Hyderabad
Irkutsk
Ivalo
JodrellBank
Juliusruh/Ruegen
Kakioka
Kanzelhohe
Kerguelen
Khabarovsk
Kharkov
Kie 1
Kiev
Kiruna
Kislovodsk
Kodaikanal
Kokubunj i
Kootwijk
KranzbachKuhlungsborn
Leningrad
LindauLj ub 1jana
Loc arno

12 101
31504
30504
18501
38701
34101
30505
32601
32602
18403
20301
31504
31505
30506
82301
18502
33301
10502
44401
85401
26201
20302
57101
38201
40501
33 701
10503
31506
44402
31507
77501
43501
34501
31508
33501
32702
34402
38101
44403
30507
31509
31510
33601
31511
31512
31513

D. II.
Indicator
Lockheed (Burbank) Lomnicki
22302
32502
St it
Los Angeles
22303
Luchow
31514
Lulea
32602
Lwiro
73001
Lycksele
32603
McMurdo
87801
McMath18404
Magadan
45601
42101
Manila
Maui (Haleakala)
26202
26203
Maui (HBS)
Mawson
76701
Meudon30508
Mitaka44404
44405
Mt. Norikura
Mt. Wilson
22304
Moscow
34502
82302
Mundat ing
Murmansk
33 702
30509
Nan
Jay
Nanking
42301
Narssarsuak
14601
Nera
30510
31515
Neustrelitz
38301
New Delhi
87301
Norfolk Islani
32604
Nurmijarvi
Oahu
26204
43301
Okinawa
31516
Ondrejov
18405
Ottawa Domxn
Ottawa NBC
18406
18407
Ottawa CR0
22401
Palo Alto
31517
Panska Ves
Paramaribo
15101
18408
Penn State 1
22501
Penticton30401
pic‑du‑Midi
30511
Poitiers
85101
Port
Morest73301
Potchefstri
31513
Potsdam
31518
Predigtstu
31519
pruhoniceQuezon Git
42102
17201
Ramey AFB
12601
Reykjavik

StationIndicator

Resolute Bay
19701
Roi Baudouin
72701
Rome
31406
Sacramento Peak
21301
Sagamore Hill
17401
Salekhard
37701
San Miguel
56302
Saskatoon
21501
Simferopol
33402
Sitka
23601
Skalnate Pleso
32503
Sodankyl^
33 703
South Pole
70901
Spitzbergen
31801
St. John's
15501
Stockholm
32605
Sydney (Fleurs)
85304
Sydney (ipSI)
Balmoral) 85305
65201
TahitiTaipei
42202
Tamanrasset
30201
Tananarive
75201
Tashkent
37401
Tehran35401
Terre Adelie
84701
Thessalonika
32403
Thule
17801
Tiksi Bay
43701
Tokyo
44406
Tortosa
30402
Townsville
85201
Toyokawa
44301
Tremsdorf
31520
Trinidad
16101
Tucuman
56303
Tucson
21302
Uccle
30512
Univ. Park
18409
Uppsala32606
Vanimo
84001
Voroshilov (Ussurisk 43401
Washington
18401
NASA
Washington USNRL
18402
Weissenau
31521
Wellington
87401
Wendelstein
31522
White Sands
21302
Wilkes
81701
Wingst21523
Witteveen
31524
Yakutsk
43601
Zurich31525

PART E.

DETAILS OF PLAN FOR RAPID COMMUNICATIONS

E. I. Descriptionof Arrangements for Rapid Interchange

The basic concept of the rapid interchange arrangements is that observing
stations transmit data reports to a Regional Warning Center (RWC), that the
RWCs interchange data among themselves, that each RWC serves the needs ofinstitutions in its region for prompt data, and that in addition the RWCs
provide any necessary forecasts and alerts based on the comprehensive dataand information assembled through the whole data interchange activity. For
the worldwide alerts, all the RWCs provide their opinions to the RWC for theWestern Hemisphere which issues the worldwide GEOALERT, acting as the IUWDSWorld Warning Agency.
For purposes of this interchange, the IUWDS has identified five regionsof the world, each with a Regional Warning Center (for Western Europe thework is shared by three RWCs). The regions are:Western Europe
Western Hemisphere
Western PacificEurasia
Australasia and Antarctica
In addition, there are Associate RWCs in India, Sweden, Czechoslovakia and
USSR which perform part of the functions of an RWC. The regions are notstrictly geographical but are determined by the efficiency or economy ofcommunications.All details of the RWCs and Associate RWCs are given in
E. II below.
Participating observing stations are listed in Part D, above. Somesend reports regularly but many others have sent reports only when they
have observed a most unusual event. The stations send their reports to oneof the RWCs or Associate RWCs and thus the data gets into the rapid inter‑change system. The channels for communication are heterogeneous and change
from time to time, so it is not worthwhile to specify them in detail. How‑ever, in general the channels have been proven to be efficient and dependable
by repeated usage over a number of years.
Observing stations should dispatch their data reports as soon as prac‑
tical after the observations are made. The IUWDS codes should be used,with any further comments in plain language.
Speed is especially important when very unusual events are observed ‑‑such as outstanding flare events or proton events (see Part B (1.1) for fulllist); in these cases the observing station should send the message as an
ADALERT (advance alert) in plain language without taking time to prepare theusual data code. The full data report in the appropriate code should always
be sent afterwards.

E. I. (continued)
The RWC receives data from the observing stations with which it is in
direct contact. It has an habitual daily schedule for the interchange withother RWCs as given in the subsections of Part E. II. There are understand‑ings among the RWC so that essentially duplicating data reports are notinterchanged. Thus each RWC has an equivalent amount of solar and world‑
wide geophysical data on which to base the forecasts, regional alerts anddata distributions which are made in that region. The RWC also uses thisbody of data as the basis for sending each day its advice on the worldwide
GEOALERT to the IUWDS World Warning Agency. When very unusual events arereported as ADALERTs (whether from within its region or from outside), the
RWC has the responsibility to relay by expedited communications to the other
RWCs (if reported from within its region) and in all cases to any scientificinstitutions within its region which have requested this expedited service.
The objective is to distribute these ADALERTs to the relatively few numberof requesting institutions within one hour.
Several RWC compile a report for distribution to requesting scientificinstitutions which combines and to a certain extent interprets the large
number of individual data messages which it receives. This GEOSOL message(Part B (IV.1)) is partly in code and partly in key words. It provides aninformed summary of the state of the solar‑terrestrial environment andincludes the indices and details which are commonly needed by scientists.
The worldwide alert (GEOALERT, see Part B (II.1)) identifies or fore‑casts major solar or geophysical activity. Many observational programs are
influenced by the information in the GEOALERT message, which tends thus tocoordinate the worldwide observational effort. The GEOALERT is in plain
language in standard format. A message is issued each day at 0400 UT by
the IUWDS World Warning Agency; the message says GEOALERT NIL if there isno activity expected. It is distributed very widely, through RWC, by radio
broadcast and over the WMO meteorological telecommunications network (seefollowing Part B (II.1) for details of distribution). The content of the
GEOALERT is decided from the advice sent each day by the RWCs to the World
Warning Agency (see Part B (III.l)).
The success of the plans for all of these rapid interchange services
depends on there being effective arrangements for communications. Sincemany different communication channels are involved, the overall scheme has
to be the sum of many individual arrangements for communications between
observing stations and RWC and between RWC and the users of the services.
In practice all forms are used ‑‑ telephone, telex, special or commercial
or government teletype, radio links, meteorological networks. To help solvethese practical communication problems, it has been found convenient, beginningwith IGY, to have in each country participating in the program, an individual
who is designated as the "National Warning Contact" for that country (seePart E. Ill below for detailed list). This individual has knowledge of thepractical communication possibilities in his country and is requested towork with the RWC in making suitable and effective arrangements for commu‑
nications to or from stations or institutions in his country. It is hoped,

E. I. (continued)
moreover, that he can solve any problems of incidental cost which may
arise. The requirements for communications are both dependability andspeed, and the general objective is a maximum of two hours for thedelivery of a message over any single link, with the possibility of
expedited communications in a few tens of minutes to or from selected
stations or institutions involved in the Advance Alert (ADALERT) phaseof the program.

E. II. Details

of Regional and Associate Regional Warning Centers

The following detailed information was supplied to the IUWDSSecretaries in late 1968 or early 1969. No direct replies were received
from ARWC New Delhi or ARWC Irkutsk. The entries for these two centers
are taken from the latest information available.
It should be remembered that solar‑geophysical data interchange
is constantly expanding. New stations are established from time totime and communication routings for existing stations are modified forpractical reasons. Therefore, the arrangements for data collected
directly by each RWC will not remain static, and the information in thefollowing subsections should be regarded only as examples of data collected.

WORLD WARNING AGENCY (WWA)andRWC BOULDERSupervisory and
Immediate Charge

R‑ B. Doeker
D. B. Buckriam

Mail Address

Space Disturbance Forecast Center
ESSA, Boulder, Colorado, U.S.A. 80302

Telephone

303‑447‑1000 Extension 3171

Telex

45897 SOLTERWARN

TWX

303‑443 3653

U. S. MilitaryRUWTGPACable

SOLTERWARN, Boulder, Colorado

Operating Organization

Environmental Science Services Administration

Operating Hours

24 hours/day (but with somewhat limited
operation 0600‑1400 UT)Mes s age s(Data)(Forecast)

Data Solarcollected
WWA (RWC)
dataat(optical)Solar and Geophysical data for IUWDS
interchange issued daily, nominallyat 0200 and 1800 UT
1. GEOALERT at 0230 UT
2. Solar and Geophysical forecasts andsummary paragraphs for the past day,at 1700 and 2300 UT. Emphasis onflares, proton events, 10 cm radio
noise flux, geomagnetic activity.
Boulder, Sacramento Peak, McMath, Lockheed,
Los Angeles, Huancayo, Houston, CanaryIslands, Carnarvon, Culgoora, Maui, Manila,
Athens, Ramey, Tehran

Solar data (radio noise)

Ottawa, Penticton, Sagamore Hill, Penn. State,
Boulder, Fort Davis, Palo Alto, Los Angeles,
Manila, Athens, Houston, Canary Islands,
Carnarvon

Solar cosmic ray data

Anchorage,
BoulderFt. Churchill,

Thule,

Deep

River,

E. II. 1 (continued)

X‑ray data Washington(NRL),Aberdeen,Boulder

Ionospheric data (SID)

Boulder, McMath, Anchorage, CanaryIslands, Carnarvon, Manila, Maui,
AthensIonospheric data (UFOF)

Boulder, Resolute Bay, St. John's,
Wallops Island

Geomagnetic

Fre d e r i c k s b u r g ,data

Boulder,

Anchorage

Exchanges with RWC
Telegrams
0200 UT From
0230 " " (also
1800

Boulderto WMO net)

Broadcasts
WWV GEOALERTWWVH " " "every hour at 18 minutes pastat 48 minutes past

E.

II.2

RWC

PARIS

Supervisory and
Immediate Charge

Dr. P. S imon

Mail Address

Ursigrammes Observatoire
92 Meudon, France

Telephone

027 11 39

TWX
Telex

25312 CNETAGIMeudoa

Cab leTX25312 CNETAGI Meudon

Operating Organization

Jointly: CNET 96 Rue de Paris Bagneux
and
OBSERVATOIRE 92 Meudon

Operating Hours

0730 UT ‑ 1600 UT
Saturday 0900 ‑ 1400 UT(Closed on Sunday and holidays)

Messages(Data)GEOSOL ‑ Abbreviated solar and geophysicaldata issued daily close to 1400 UT(Sunday excepted)
URSIGRAM ‑ Solar and Geophysical data
issued daily (Sunday excepted)
close to 1000 UT and 1400 UT.
(Saturday the 1400 UT message
only.)(Forecast)

Solar activity and geophysical disturbancesin the GEOSOL and the 1400 UT URSIGRAM.

Data collected in its area
Solar data

Catania, Meudon, Nancay, Pic‑du‑Midi,Roma, Tortosa

Solar cosmic ray datalies Kerguelen, Pic‑du‑Midi

X‑ray data

SOLRAD through CNES BRETIGNY

Ionospheric data

Daily reports ‑ lies Kerguelen, Poitiers
Weekly reports ‑ Dakar, Djibouti,
Tahiti, Tananarive

E.

II.2

(continued)

G e omagnetic

Exchanges

with

0 7 00STE

data Chambon‑la‑Foret,RWC

LTT From

and

lies

WWA

Boulder

1 0 00 FromPraha

1 2 00 From

Darmstadt

1 4 00 To

Boulder,

1 5 00 ToTokyo

A S S ISE

KerguelenandandMoscow
To k y oan d(occasionallytoDarm s t a d t ,Frequency

Sign

(kHz)

Nera,

Moscow,(occasion a l l y

Call

from

Darmstadt,

to

Nera,

Praha

Sydney)Timesof

Emission

FTA91

UT

1208(1)

Solar‑geophysical1308(1)data

2008(2)GEOALERTS

2108(2)P O N T O I S E F TK77

10775

Al

13873

Al

1208(1)
2008

FTN87

Sydney)
Praha

Nera

(2)

1308(1)?.1 Qfi GO

1000

UT

Ursigram

at

times

denoted

(1)

1400

UT

Ursieram

at

times

denoted

(2)

amd

E.

II.3

RWC

DARMSTADTSupervisory and
Immediate Charge

Dr. B. Beckmann, Asst. A. Ochs
G. Richter

Mail Address

FTZ D 33
Am Kavalleriesand 3
61 Darmstadt
Federal Republic of Germany

TelephoneDarmstadt (0 61 51) 83‑25 30 (Beckmann)
25 49 (Ochs)
25 33 (Richter)

TWX

Telex

0419291IONO D

Telegraph

IONOSPHAERE Darmstadt

Operating Organization

Fernmeldetechnisches Zentralamt
61 Darmstadt

Operating Hours

0630 ‑ 1545 UT(Closed Saturday, Sunday and holidays)

Messages(Data ‑ Ursigram)Solar aridGeophysical Data issued
daily at 1200 UT (Saturdays, Sundays
and holidays excepted)(Forecast)

Ionospheric Propagation Conditionsin the Ursigram

Data collected

in its area

Solar data (optical)

Kanzelhohe, Wendelstein, Freiburg

Solar data (radio noise)

Kiel, Weissenau, Stockholm

Solar cosmic ray data

Lindau, Kiel, Predigtstuhl (Reichenhall)
Kranzbach (Mittenwald)

Ionospheric data

Breisach, Lindau, Darmstadt, Kiruna,
Enkoping

Geomagnetic data

furstenfeldbruck, Wingst, Sodankyla,
Nurmijarvi, Enkoping

Ionospheric propagation
condit ions

Luchow

E. II.3 (continued)
Exchanges with ARWC, RWC and WWA
Te lex

E.

RWC

II.4

NERA

Van Lohuizen
Van Burcken

Supervisory
andImmediate Charge

Dr. Neher Laboratory
St. Paulusstraat 4
Leidschendam, Netherlarid

Mail Address

Telephone
TWX
Te lex

12 308 NHORST DNL

Cable

IONRAST LEIDSCHENDAM

Operating Organization

Netherland Postal and
Telecommunication Services
Dr. Neher Laboratory

Operating Hours

0730 ‑ 1600 UT(Closed Saturdays, Sundays and holidays)Mes s age s

Alerts, Solar and Geophysical data
1300 UT daily(Saturdays, Sundays and holidays excepted)(Data)(Forecast)
Data collected

Solar and Geomagnetic activity
in its area

Solar data (optical)

NERA, Capri (through Stockholm)

Solar data (radio noise)
Solar cosmic ray data
X‑ray data
Ionospheric data

De Bilt (K.N.M.I.), Kootwyk (P. and T.)

Geomagnetic

Witteveen, NERA

data

Exchanges with RWC aridWWA
Telex 0700 UT From Boulder
1000 FromPraha, Meudon, (including Tokyo)
1300 To
Heudon1500 To
Boulder
No radio broadcast of the Ursigrams.

E.

II.5

RWC

Supervisory and
Immediate Charge

MOSCOW

Mme
Mme R.
L. A.
N. Zevakina
Ljakhova

Mail Address

P/0 Akademicheskii Gorodok
Moscow District, USSR

Cab leMoscow 754 IZMERAN

Operating Organization

Institute of Terrestrial
Magnetism, Ionosphere andRadiowave Propagation,
Academy of Sciences, USSR(IZMIRAN)

Operating Hours

24 hours/dayMe

s s age s(Data)

Ursigram:
Solar and Geophysical data issued
daily close to 1600 UT(Forecast)

Solar activity
geophysicaldisturbancesin andADVMO
at 1600 UT;
ionospheric disturbances in
URSIGRAM for National Centers

Data collected in its area
Solar data

Kislovodsk, Simferopol,
Voroshilov, Irkutsk,
Tashkent, Moscow, Kharkov,
Abastumani, Berlin H. Hertz

Ionospheric data

Daily reports ‑Juhliusruh, Budapest, Pruhortice
Hourly ‑Druzjriaja,Murmansk, Dixon,
Cape Schmidt, Leningrad,
Salekhard, Yakutsk, Magadan,
Khabarovsk, Moscow, Kiev,
Alma‑Ata, Ashkhabad
SID ‑Kuhlungsborn, Pruhonice, Juhliusruh

E. II.5(continued)

Exchanges

with

RWC and WWA

Telegrams
BeforeBefore

0900
1500

UT
UT

1600 UT

Ursigram

broadcasts

Time of transmission,
Call
Moscow legal time cies,

From Washington and Meudon
From Tokyo, Darmstadt, Praha(occasionallyfrom Sydney)
To Washington,
Tokyo, Meudon,
Sydney and National Centers,
to subcenter Irkutsk
Moscow ‑ three times a day,current data summaries andforecasts

letters

Frequen‑ Remarks
kHz
From 1/3 to 30/9
From 1/10 to 28/2
All yearAll yearAll yearAll yearAll yearAll yearAll yearAll yearAll yearAll yearAll yearTransmission
Moscow legal

time,
time

Frequency
kHz
C10344‑ 58607545
f 58601 3 740. 4490

E.

II.

6

Supervisory and
Immediate Charge

RWC

KOKUBUNJI

KasuyaTakiguchi

Mail AddressRadio Research Laboratories
Ministry of Post and Telecommunications
2‑1, Nukui‑Kitamachi 4‑chome
Koganei‑shi, Tokyo, 184 Japan

Telephone0423‑21‑1211

Telex

2832611 (DEMPA KKB)

Telegraph

TLX 2832611 DEMPA TOKYOCab leOperating Organization

Radio Research Laboratories

Operating Hours

24 hours/day

Messages(Forecast)Radio propagation advance weekly‑
forecast issued on Monday andThursdayE. II.6 (continued)
Data collectedin its area
Solardata Hiraiso,
Solar cosmicray data Mt.

Mitaka,Mt. Norikura,
Norikura,Tokyo

X‑ray data
Ionosphericdata

Hiraiso,Kokubunji(daily report)

Geomagnetic
data

Kakioka

Exchangeswith RWC and WWA

Broadcastssee Messages(Data)above.

E.

RWC

II.7

SYDNEY

Supervisory and
Immediate Chargec. G. McCue
F. E. Cook

Mail Address

IUWDS Regional Warning Centre
Ionospheric Prediction Service Division
Commonwealth Centre
Chifley Square
Sydney N.S.W.
2000
Australia

Telephone259 3366 (after hours 451 5848)

TWX
Telex

IPSO 20663

Telegrams

IPSO Sydney

Cable

IPSO Sydney

Operating Organization

Ionospheric Prediction Service Division
Bureau of Meteorology

Operating Hours

2230 ‑ 0700 UT (and later as required)(sometimes closed from 0300 UT ori
Saturdays, Sundays and holidays)(Data)

Ursigrams: Solar and Geophysical Data
issued daily at 0100 UT, occasionallyat 0630 UT, and following major events(Forecast)

Daily in 'Advice' message to WWA, andoccasionally as required to organizations
mostly in Australia, New Zealand andAntarctica

Data collected in region
Solar data (optical)

Culgoora, Carnarvon

Solar data (radio noise)

Sydney, Culgoora (occasionally), Carnarvon

Solar cosmic ray data
X‑ray data
Ionospheric data (SID)

Sydney, Canberra

E. II.7 (continued)(UFOF) Weekly reports‑ NorfolkIsland,Brisbane,
Townsville,
Canberra,Hobart,Port Moresby,
Vanimo,Mundaring,Wilkes,Cocos Islands,
MawsonGeomagnetic
data Canberra,

Sydney,Gnangara

Exchangeswith RWC and WWA
2300 UT From
Boulder,Moscow,and occasionallyParis0100 To
Boulder, Tokyo
To Moscow (Events)
0630 To
Boulder, Tokyo,Moscow,Paris (Events)
0800 FromTokyo (JJD Broadcast)ARWC

STOCKHOLM

Akerlind
Muth

Supervisory
andImmediate
ChargeMail Address

Central Administration of
Swedish Telecommunications
Development Department
S‑12386 Farsta, Sweden

Telephone
TWX
Te lex1208 Radgen S; 19734

Cab leGENRADIOTEC

Operating Organization

Central Administrationof
Swedish Telecommunications

Operating Hours

0700 ‑ 1540 UT
0700 ‑ 1500 UT May‑August(closed Saturdays, Sundays and holidays)

Me

Tgfstkm S

Stockholms s age s(Data)

Alerts, solar and geophysical data
issued temporarily(Forecast)Daily
propagationand disturbanceforecast
issued regionally

Data collected in its area
Solar data
SolarcosmicStockholm
ray data

X‑ray data
Ionospheric data

Stockholm, Enkoping, Uppsala, Lycksele,
Kiruna, Sodankyla, Nurmijarvi

Geomagnetic

Enkoping, Sodankyla, Nurmijarvi

data

Exchanges with RWC and WWA
0700 UT From
0900 From
0900 To
1300 From
1500 From

Boulder, via WMO
Darmstadt
Darmstadt, NERA
NERA
Paris

Supervisory and
Immediate Charge

P. TriskaAsst. K. Dobias, M. Jiskra

Mail Address

Geophysical InstituteBocni II
Praha 4 ‑ Sporilov
Czechoslovakia

Telephone

727 788,

Telex

Oil 346 ION PRUHONICE(016 350 ION PANVES)

Operating Organization

Geophysical Institute of the
Czechoslovak Academy of Sciences

Operating Hours

0530 ‑ 1330 UT(Closed Saturdays, Sundays and holidays)(Data ‑ Ursigram)Solar and Geophysical Data
issued daily at 1000 UT(Operating days)

792

204

Data collected in its area
Solar data (optical)

Ondreiov, Skalnate Pleso

Solar data (radio)

Berlin, Neustrelitz, Ondrejov

Ionospheric data

Pruhonice, Panska Ves, Juliusruh,
Kuehlungsborn, Neustrelitz

Geomagnetic data

PruhoniceExchanges with RWC
Telex

0700 UT From
0700 From
1000 From
1000 To
1200 From
1400 From

Darmstadt
MoscowParis, NERA
Darmstadt, Moscow, NERA,
Darmstadt
Paris

E.

11.10

ARWC

NEW

DELHI

Supervisory and
Immediate Charge

A. P. Mitra

Mail Address

National Physical Laboratory
New Delhi 12, India

Telephone55298,53051, 52045

Telegraph

NATPHYLAB

Operating Organization

National Physical Laboratory

Operating Hours

Messages(Data)

Solar and Geophysical Data
and Alerts by broadcast‑'currentdata
summaries+17.40 on
Saturdays(Forecasts)
Datacollected

in

its

Solar

data

(optical)

Solar

data

(radioSolar

cosmic

X‑ray

data

Ionosphere

ray

data

Geomagnetic

Exchanges

with

Broadcasts

area

Kodaikanal,

Hyderabadnoise)

data

(SID)

New

Delhi

data

RWC

‑

See

Messages(Data)

above

F..

ARWC

TT.ll

IRKUTSK

Supervisory and
Immediate Charge

E. S. Kazimirovsky

Mail Address

Siberian Institute ofTerrestrial Magnetism
Ionosphere and Radio Propagation(Sib IZMIR)
Irkutsk 3, Box 65, U.S.S.R.

Telephone

55‑66;

63‑48

Telegraph
Operating Organization

Siberian Institute ofTerrestrial Magnetism
Ionosphere and Radio Propagation

Operating Hours(Data)

State of ionosphere, magnetic field
and radio communications(Forecasts)

For five days and 12 hours
in advance for ionosphericradio communications

Data collected in its area
Solar data (optical)
Solar data (radio noise)
Solar cosmic ray data
X‑ray data
Ionospheric data
Geomagnetic data
Exchanges with RWC
Telegrams
Broadcasts

NATIONAL WARNING CONTACTS(as of January 1969)
Argentina
Servicio Heteorologico
Nacional,
Paseo Colon 317 ‑2°Piso,
Buenos Aires.

Bolivia*Dr. Luis Fernandes, Director
Laboratorio de Fisica Cosmica
Universidad Mayor de San Andres
La PazBrazilMr. F.E. Cook,
Ionospheric Prediction
Service Division,Commonwealth Centre,
Chifley Square,
Sydney, N.S.W. 2000
Cables: IPSO SYDNEY
Telephone: 256 3366
AustriaProf.Dr. Ferdinand Stein‑hauser, Director,
Zentralanstalt fur Meteo^o‑logie und Geodynamik,
Hohe Warte 38,
Vienna 1190
Telex: 07‑4337
Belgium
Prof. M. Nicolet,
CNRE,
3, Avenue Circulaire,
Bruxelles 18.
Cables: CENTRESFACEBRUXELLES
Telephone: 02‑74.2 7.28
Telex: 2 21563. ‑CENTRE‑SPACE BRU.

Dr. Fernando de Mendonca,
Scientific Director,
Comissao Nacional de Ativ‑
idades Espaciais,
Sao Jose dos Campos,
Sao Paulo.
Bulgaria
Hydro‑Meteorological
Service,boul. Lenin 146,
Sofia.
Telegraph: SOFIA, MGSS
Telex: SOFIA, H METEORSS 542
Telephone: Sofia, 1‑22‑71,
7‑24‑50
Immediate Charge: Sasho
Mulushev.
Burma**Mr. U Ba Kyi,
Assistant Director,
Burma Meteorological
Department
New Secretariat Building
Merchant Street,
RangoonContact for IUCSTP program
Member or consultant of Western Pacific Regional Committee of IUWDS

E. III.

(continued)

Canada・>Dr.T. R. Hartz
Communications Research Centre
Shirley Bay
Ottawa 4
Cables: RESEARCH OTTAWA

Ing. P. Triska
Geophysical Institute ofCzechoslovak
Academyof Sciences, Bodni II
Praha 4,
Sporilov.

CeylonMr. R. Mahadeva,
Secretary,
Ceylon National Committee
for IQSY,
Department of Meteorology,
Bullers Road,
Colombo 7.

Cables: MEGER PRAHATELEX: 00346‑ION PRU‑
HONICE
Telephone: 92 3 796,
99 22 04
Supervisory: P. Triska
Immediate Charge: K. Dob
Denmark

China, Republic of"Dr. T. V. Miao
Director
Radio Wave ResearchLaboratories,
Ministry of Communications,No. 54, Chi Chow Street,
Ching‑Mei Town
Taipei Hsian, Taiwan.
Columbia
Director Escuela Naval
Cadetes
Cartagena"Dr. A. N. Lundbak
Geophysics Department
Danish Meteorological
Institute
Technical University ofDenmark
2800 Lyngby"Prof. Denis G. Osborne
Department of Physics
University College
Dar es Salaam
Ethiopia

Congo (Leopoldville)

Telegraph: COUMET/LEO"Dr. Pierre Gouin
Director of theGeophysical Observatory
Haile Sellassie I
University
Addis Ababa

Cuba

FinlandDirector,
Observatorio Nacional,
Casa Blanca,
La HabanaMr. T. Haikonen,
General Direction of Posts
and Telegraphs,
Mannerheimint, 9,He lsinki.

Monsieur M. Clerebaut,Service M^t6'orologique,
Leopoldvi1le.

Cables: CLUMATO‑HAf'ANA
Telephone: 60‑1231

E. III. (continued)

FranceMonsieur P. Simon,
Service des Ursigrammes,
Observatoire de Paris,
92 Meudon,
German Democratic
Republic
Dr. H. Rurige,
Hauptwetterdienststelie,
Potsdam.

Avenida "Las Americas"
5‑76,
Zona 13, Guatemala City,
C. A.
Telephone: 63281‑2‑3
Hong Kong**Mr. G. J. Bell,
Director, Royal Observatory,
Nathan Road,
Kowloon.

Cables:WETTER
Telex: 015
116 POTSDAM

Hungary

German Federal Republic*Prof. L. Deszo,
Director,
Heliophysical Observatory,
Debrecen.

Dr. B. Beckmann,
FTZ D33
Am Kavalleriesand 3,
61 Darmstadt.

Ice landGhana

Dr. Th. Saemundsson,
Bblstadarhlfd 14,
Reykj avik.

*Prof. J. R. Koster,
Department of Physics,
University of Ghana,Legon,
Accra.

India

GreeceDenis Metaxas,
Meteorological Centre,
Hellenikon Airport,
Athens.
Cables: IQSY ATHENSSpecial Cables: LGGMYMMETAXAS

Mr. P. R. Krishna Rao,
Director‑General of Observ‑
atories ,India Meteorological De‑
partment ,New Delhi 3.
Indonesia""Dr. Ir. Sorroto Mangoensoemarto
Director, Meteorological andGeophysical Institute
Djalan Geredja Inggris 3
Dj akarata

GuatemalaEngr. Haroldo Duarte
Villela,Chief of Geophysics Section,
Direcci6n General de Carto‑
grafiaIre land
Director,
Meteorological
Service,44 Upper O'Connell
SLreet,Dub 1in.

E.

III.

(continued)

Israe1

Korea, Republic o̲f≪Dr.Aharon Eviatar,
National Committee for Space
Research,
1740 Ramat‑Aviv.

Prof. Dr. Nyong D. Kwon,
c/o National Academy of
Sciences, ROK,San 2 1, Samchung‑dong,
Chongno‑koo, Seoul.

Ital;

Cables: IQSYCENTRE
SEOULProf. M. Giorgi,
Commissione Italiana
di Geofisica,
Piazzale delle Scienze 7,
Roma 00100.
Cables: CORICERCHE‑AGI ROMA
Telephone: 490.151.

Nether lands"Dr. Leen de Feiter,
Space Research Laboratory,
Huizingalaan 121,
Utrecht.
New Zealand

Jamaica*Prof. R.W.H. Wright,
Department of Physics,
University of West Indies,
Kingston.

The Director,
New Zealand Meteorological
Service,
P.O. Box 722,
Wellington.
Cables: WEATHERLINGTON

Dr. Isao Kasuya,
Radio Research Laboratories,
Ministry of Posts and Tele‑
communications,
2‑1, Nukui‑Kitamachi
4‑chome,
Koganei‑shi,Tokyo, 184.

Korea, Democratic
People's Republic of
Lie Rak Bok,
Astronomical Observatory,
Pyongyang.

WEL‑

Nigeria
The Senior Meteorologist
Meteorological Service,
Airport,Kano.
Telephone:
Office ‑ Kano 2631 orExt. 121.
Residence ‑ Kano 2586.
Deputy Forecaster,
Telephone: Kano 3011,
Ext. 102.
Pakistan
Mr. A. W. Kahn,
Deputy Director,
Pakistan Meteorological
Service,E. III.

(continued)

Secretariat Blocks 1‑3,
Frere Road, Karachi 3.

Senegal

Cables: METEOR"Prof. H. Masson
University of Dakar
Dakar

Peru

Sierra Leone

Ing. A. Giesecke
Instituto Geofisico del Peru,
Ministerio de Fcrmento,
Apartado 3 747,
Lima.

The Director,
Meteorological Department,
Lungi Airport.
South Africa

Cables: AGI

LIMA

Philippines
The Director
Weather‑Bureau,
Department of Commerceand Industry,*wAttn: Mr. Lorenzo Tolentino
Manila,P.O. Box 2277.

Mr. G‑ H. Westhuizen,
Science Cooperation
Division,
CSIR,
P.O. Box 395,
Pretoria.
Cables: NAVORS
Telephone: 74‑6011.
Spain

Portugal
The Director,
Servi^io Meteorol6gico
Nac iciral,
Attn: Dr. A. Silva de Sousa
Rua Saraiva de Carvalho 2,
Lisboa 3.
Cables: METEOLISB
Telephone: 662188 and
663543.

Rev. Father J. 0. Cardus,
Observatorio del Ebro,
Apartado 9,
Tortosa.
Sweden*Dr .FoIke Eleman
Swedish Board of
Shipping and Navigation
Geomagnetic
Section102
50 Stockholm
27

Rhodesia
United Arab Republie
Mr. A. C. Iauld,
Federal Department of Tri‑gonometricaland Topo‑
graphical
Surveys,
P.O. Box 8181
Causeway,
Salisbury

Dr. M. F. Taha,
Meteorological Dept.,
Ministry of War,
Koubry El‑Quobba,
Cairo.
Cables: WEATHERCAIRO

E. III. (continued)
United Kingdom
Director,
Radio Research andSpace Station,
Ditton Park,
Slough, Bucks.
Cables RADSEARCHSLOUGH
Telephone: Slough

24411.

United States ofAmerica
Miss J. Virginia Lincoln,
ESSA
Boulder, Colorado, 80302
Union of Soviet Socialist
Republics
Mme. R. A. Zevakina
P/0 Akademicheskii Gorodok
Moscow District
Viet‑Nam, Democratic
Republic of
Nguyen Xien, Meteorologiste,
Service Meteorologique,Hanoi.

Contact for IUCSTP program
Member or consultant of Western Pacific Regional Committee of IUWDSPART F.

IUWDS AND ITS PROGRAMSThe International Ursigram and World Days Service is a Permanent Serviceof the International Union of Radio Science (URSI) in association with theInternational Astronomical Union (IAU) and the International Union of Geodesy
and Geophysics (IUGG). The IUWDS, as now constituted, was formed in 1962 as
a combination of the former International World Days Service, which had been
initiated in 1959 to continue many aspects of the IGY World Days program, andthe former URSI Central Committee on Ursigrams which represented rapid datainterchange activities first begun about 1930.
The IUWDS provides a mechanism for international cooperation in many ofthe more operational aspects of solar‑terrestrial and similar work, withemphasis on rapid interchange of information. Specifically, the IUWDS Steer‑ing Committee comprises representatives of the interested ICSU scientificunions, as well as some regional representatives and liaison with otherinterested organizations like the World Meteorological Organization (WMO).
The Committee gives recognition to certain national institutions for playing
international roles ‑‑ Regional Warning Centers, Associate Regional Warning
Centers, and the World Warning Agency. It also maintains a list of National
Warning Contacts (NWC), who help coordinate activities at a national level.
The Steering Committee meets almost every year, and minutes or summaries ofthese meetings appear in the URSI Information Bulletin. The officers andother leading participants are continually active by correspondence andinformal meetings. The IUWDS program is explained and coordinated throughthe issuance of program documents, the code booklet, notices in STP Notes
and other information bulletins of ICSU groups, through items like theInternational Geophysical Calendar printed in the technical literature andseparately, and through mimeographed 'RWC Circulars" issued directly to
RWCs and NWCs. Since much of the work is done by scientists who are supported
from national sources or is done in cooperation with other groups, the costof the activity to international funds is quite small. The IUWDS does receivea small allotment through the Federation of Astronomical and Geophysical
Services from UNESCO sources for printing, travel and office expenses whichcannot be covered otherwise.
The IUWDS works very closely with other ICSU organizations involved
in international cooperation in astronomical, geophysical and space sciences.
In fact there is no sharp line between the IUWDS "program" and those arranged
through other groups. The IUWDS attempts to respond to the needs of thescientific community, whether these are expressed formally or informally.
Thus IUWDS leaders participate in the work or meetings of the URSI, IAU,IUGG (particularly IAGA and IAMAP), IUPAP (Cosmic Ray Commission), COSPAR,IUCSTP, CCIR, WMO, SPARMO, SCAR, and formerly in the IGY, CIG and IQSY
activities. Also there is no sharp line between IUWDS work and the activ‑
ities of the STP World Data Centers. The data handled in the IUWDS‑sponsoredactivities also go to the World Data Centers; the institutions involved areusually the same, and the flow of preliminary and definitive data is thereby
coordinated. Finally it should be noted that there is no real distinction
between a large part of the IUWDS program and the IUCSTP Project 1 "Monitor‑
ing of the Solar‑Terrestrial Environment"; in this case also the leadershipand many of the participants are common to the two undertakings. In summary,
the IUWDS attempts to provide a central service to the scientific andF. (continued)
technical community in many aspects of what might be called the "active"
coordination of programs involving international cooperation in astronomical,
geophysical and space science.
The IUWDS program can be categorized as follows:(a) Coordination via alerts and forecasts(b) Telegraphic interchange of data(c) Coordination via calendars issued in advance(d) Coordination via intervals selected retrospectively(e) Compilations of interdisciplinary data summaries(f) Cbmmunication services to other ICSU organizations
Full information on the first two topics is given in Part E. It is
given separately because these are the programs for which this booklet isintended. The remaining programs are described in the following sections.
Coordination
viawascalendars
issuedforin theadvance.
The International
GeophysicalCalendarfirst issued
IGY observation
period, 195 7‑
1958, under the IGY "World Days" program, and has been issued annually sincethat time. On the Calendar are marked certain days or series of days selected
for special treatment as regards observations or data exchange. The conceptof the Calendar is illustrated in Figure 1. The selections provide various

F. (continued)
kinds of samples for measuring the time variation of geophysical phenomena.
The Calendar also indicates the occurrence of phenomena of interest which
can be predicted long in advance such as solar eclipses and meteor showers,
and in addition any special intervals selected for intensified international
and interdisciplinary cooperative observations such as for the Proton Flare
Project. Accompanying the Calendar are recommendations on scientificprograms to be carried out on the days and intervals marked on the Calendar;
these recommendations are compiled or reviewed by spokesmen for the various
disciplines or projects.
The present procedure is to prepare each Calendar during the preceding
year. In about May a "planning" edition is issued with a sizeable but
limited edition for use by ICSU groups and scientific institutions which
are still planning their detailed programs. For this edition the dates
selected for the "World Days" are considered to be definitely fixed, but
the recommendations for scientific programs are considered as preliminary.
The latter are then revised according to information received from projectand discipline spokesmen, and a final "operational" edition is issued in
September or October. This edition is distributed in several thousand
copies through all available channels in an attempt to reach all scientists
and observing stations involved in this kind of work. The Calendar is also
published in about a dozen scientific journals with circulation to appro‑
priate parts of the scientific community. Additional copies are available
gratis from the IUWDS Secretary and Deputy Secretary. In some disciplines,
the data exchanged through the World Data Centers is increased for some of
the World Days marked on the Calendar. For this reason, the Calendar, forpast years are of current interest; a collection of all the Calendars issued
from 1957 to 1969 is being published by WDC‑A [A. H. Shapley and J. V. Lincoln,"International Geophysical Calendars, 1957‑1959", World Data Center A, Upper
Atmosphere Geophysics Report UAG‑6, March 1969j.
Coordination via intervals selected retrospectively. Scientific studies
of solar and geophysical phenomena and their interrelationships are assisted
if coordinated attention is placed on a few phenomena which are well observed
and whose study is likely to advance scientific understanding. Various inter‑national schemes for selecting such intervals or phenomena retrospectively
have been introduced beginning with the IGY and in a general way coordinated
by IUWDS. The IQSY program placed considerable emphasis on this way of
encouraging international cooperation in data reduction, interpretation andanalysis. There were special recommendations for more detailed data to flow
to the WDCs during Retrospective World Intervals. In some cases special
symposia were organized to discuss the scientific results, and there were
publications of special reports LProf. M̲. C. Ballario "A Study of the Plages
and Sunspot Groups Observed during the Retrospective World Intervals for 1964"
IQSY NOTES No. 17, p. 2‑8, July 1966; Prof. M. C. Ballario "The Solar andGeomagnetic Activity Observed during this IQSY Retrospective World Intervalfor 1965", IQSY NOTES NO. 18, p. 4‑8, November 1966; Prof. M. C. Ballario"The Quiet Sun Year 1964 Relationship between the CMPs of Solar Recurrent
Plages and Terrestrial Phenomena", IQSY NOTES No.21, p. 36‑48, December 1967]

F. (continued)
or symposium volumes [The Proton Flare Project (the July 1966 Event),
Annals of the IQSY, Volume 3, in press].
These kinds of selections are continuing under the IUCSTP program andpossibly some others. The role of the IUWDS is to coordinate the selections
and to help distribute within the scientific community the dates of theselected intervals, the summary reasons for the selections and any plansfor coordinated discussion of results or symposia. An example of extensive
interchange through a publication of data of many forms for such an interval
has been issued by WDC‑A [J. V. Lincoln compiler, "Data on Solar Event of
May 23, 1967 and its Geophysical Effects", World Data Center A, Upper Atmos‑
phere Geophysics Report UAG‑5, February 1969J.
Compilations of interdisciplinary data summaries. During the IGY it
was proposed by Professor Sidney Chapman that there ought to be available
an interdisciplinary summary of the solar and geophysical conditions andevents for every day of the IGY. This Calendar Record was compiled under
the auspices of the IGY World Days Program and the project has been con‑tinued since that time under IUWDS auspices. The Calendar Record for
1957‑1959 was published in Annals of the IGY L1J and that for 1960‑1965
in Annals of the IQSY !̲2j.The arrangement of the material is by days,
and gives all the commonly used solar, geomagnetic and ionospheric indices,
the times of solar flares and geomagnetic storm beginnings, descriptive
characterization of solar and terrestrial conditions, and much additional
information and data which are otherwise scattered in dozens of different
publications. The Calendar Record is not regarded as a primary source ofdata and information, but instead is a convenient guide for researchstudies and a reference to the detailed primary sources. The IUWDS aids
the latter by compiling and publishing lists of selected data publicationsin the solar‑terrestrial sciences [3,4j.
During the IQSY, it was suggested by Dr. N. V Pushkov that the use‑
fulness of the Calendar Record was diminished because of the unavoidable
long delay in making such detailed compilations and then in publication.
The scientific community would be better served if the compilations could
be accelerated even if less complete or based on preliminary data reports.
Thus under IUWDS auspices an "Abbreviated Calendar Record" was published
on a more timely schedule in IQSY Notes beginning with data for January
1964■With the completion of the IQSY program, publication has continued
in STP Notes, issued several times each year by the Inter‑Union Commission
on Solar‑Terrestrial Physics. The Abbreviated Calendar Records for 1964
and 1965 have been superseded by the published final Calendar Record [2J.
[lj IGY Calendar Record, Part I, and Calendar Record for theInternational Geophysical Cooperation 1959, Part III,
Annals of the International Geophysical Year, Vol. XVI,Pergamon Press, 1962‑3.
[2] Solar and Geophysical Events 1960‑1965 (Calendar Record),
Annals of the IQSY, Vol. 2, M.I.T. Press, 1968.
C3J Annals of the IQSY, Vol. 1, pp. 308‑309, M.I.T. Press, 1968.
[4] Abbreviated Calendar Record 1966‑1967, WDC‑A Upper Atmosphere
Geophysics Report UAG‑4, pp. 164‑169, December 1968.

F. (continued)
Those for 1966 and 1967 have been collected in a publication of WDC‑A [5J
and there is no intention to publish a more definitive Calendar Record
compilation for these or subsequent years.
Communication and other services provided for other ICSU organizations.
It is clearly efficient to make some other appropriate uses of the communi‑
cation channels and system established by IUWDS mainly for solar‑geophysicalpurposes. The Regional Warning Centers which operate seven days a week andin some cases 24 hours a day can be a valuable asset to other undertakingsin scientific cooperation which have only occasional but very important needs
for rapid and dependable communications of information. Thus the IUWDS has
arranged to cooperate with the IAU, COSPAR and other organizations to provide
some additional services somewhat outside its main area of emphasis.
The Central Bureau of Astronomical Telegrams, IAU Commission 6, has thetask of distributing to astronomical observatories telegraphic announcementsof important discoveries such as comets and novae. The Bureau, located at
the Smithsonian Astrophysical Observatory, Cambridge, Massachusetts, USA,02138, makes use of some of the RWCs to relay their messages to observatories.
Since the service is on a subscription basis, this cooperation by IUWDS isaccomplished at the cost only of a small amount of time of the RWCs. A fulldescription of the service (ASTROGRAMS) is available from the Central Bureau for
Astronomical Telegrams, Smithsonian Astrophysical Observatory, Cambridge,
Massachusetts, USA, 02138.
Alerts of unusual warmings in the stratosphere and major changes instratospheric circulation are distributed through the same channels as the
IUWDS solar‑geophysical alerts, since these conditions are of interest to
many ionospheric and aeronomical institutions as well as to meteorologists.
The identification of these conditions is made by a group at the U. S.
Weather Bureau through data and analysis reports some of which flow via
the RWCs. The STRATWARM messages, in plain English language, are issued
by the IUWDS World Warning Agency at 0400 UT daily during the period of thewarmings in winter or early spring, and the messages are distributed via
the RWCs by radio broadcast and through the meteorological telecommunica‑
tions networks along with the IUWDS GEOALERT messages. The plan for STRAT‑WARM alerts was worked out cooperatively by IUWDS and by the IQSY Committee
in association with IAMAP and WMO.
For COSPAR, the IUWDS has provided the service of distributing timely
information on earth satellites. This activity started in 1958 when inter‑national cooperation in space research was under IGY auspices. The so‑called
SPACEWARN system now distributes to the scientific community the announcementsof satellite launchings and the corresponding international designations, aswell as information needed in international cooperation in satellite work.
COSPAR in fact has delegated to IUWDS the assignment of the international
designations, and this work is carried out by the IUWDS World Warning Agency.
̲5J Abbreviated Calendar Record 1966‑1967, WDC‑A, Upper Atmosphere
Geophysics Report UAG‑4, pp. 1‑163, December 1968.

F. (continued)
Some of the distributions are by telegram through channels which parallel
and in some cases are the same as the solar‑terrestrial communication
channels, but most is by a mail SPX Bulletin distributed every two weeks
to National SPACEWARN Contacts and other scientists. This SPX Bulletinhas been compiled by the IUWDS World Warning Agency. IUWDS continues towork with COSPAR to provide the most effective timely service to spacescientists.
The IUWDS has provided special forecasting and alert services for
the Solar Particle Monitoring Organization (SPARMO) for planned periodsof coordinated balloon launchings. These projects involve a limited
number of organizations and the forecasts and alerts require special
interpretations of and decisions on the basic data assembled for the
more general solar‑terrestrial purposes. The RWC for Western Europe atParis has provided the SPARMO services in close connection with the
Director of SPARMO.
Several of the projects of the IUCSTP call for special kinds ofalerts or forecasts, for example the SID project and the low latitudeaurora project. The detailed plans and arrangements will appear in
STP Notes or in bulletins to participants. As with all parts of the
IUWDS program, additions to or modifications of IUWDS services are madein order to assist as well as possible in the active coordination ofinternational cooperative work, and the most appropriate channels areused for getting the necessary information and details on arrangements
to participants and potential participants.
Membership of the IUWDS Steering Committee. According to thearrangement among URSI, IAU and IUGG, the IUWDS is administered by aSteering Committee consisting of:(a) One representative from each of the following scientificUnions: URSI, IAU and IUGG.
(b) One representative from each of the Regional Ursigram
and World Days Committees.
(c) The IUWDS Secretary and the IUWDS Deputy Secretary.
(d) The Secretary General of URSI.
In addition, the Steering Committee seeks cooperation, by direct repre‑
sentation or otherwise, with other international bodies interested in thework of the service. The Steering Committee elects its Chairman andappoints the two secretaries; the position of these officers are reviewed
at the occasion of each General Assembly of URSI. The Steering Committee
is responsible for the worldwide and interregional aspects of the service,for overall plans and guidance, and for the necessary central publications
In practice the only regional committees which are formally organized
and active are those for the Western Pacific, Eurasia and for Australasia
and Antarctica. Since the regional committee for Western Europe has been
inactive, the other regions are represented by common consent by individualfrom the institutions maintaining the RWC.

F. (continued)
The membership of the IUWDS Steering Committee as of February 1969
is:
Mr. A. H. Shapley, Western Hemisphere Region, Chairman
Dr. R. L. Smith‑Rose, European Region
Dr. I. Kasuya, Western Pacific Region
Mme. R. A. Zevakina, Eurasian Region
Mr. C. McCue, Australasia and Antarctica Region
Dr. A. P. Mitra, U.R.S.I.
Dr. R. Michard, I.A.U.
Dr. M. Nicolet, I.U.G.G.
Dr. P. Simon, Secretary
Miss J. V. Lincoln, Deputy Secretary
Dr. C. M. Minnis, Acting Secretary General, U.R.S.I.
Liaison Mr. 0. M. Ashford (WMO)
Dr. J. F. Gabites (WMO)
Mr. Fournier d'Albe (UNESCO)
Mr. J. P. Legrand (SPARMO)

PART G. ALPHABETICAL INDEX TO CODES

Footnote: Codes

no longer recommended for active use.

From 1965 edition and amendments

From 1963 edition
UFLAB
UFLAR
UPDIA

With the exceptionof the Alert codes it has been necessary to create new codes
to accommodate the change from 2‑characterto 5‑character station indicators.