InternationalUrsigram and World
Days Service
I.U.W.D.S.

Synoptic Codesfor
Solar and Geophysical Data
Revised edition
1965

Published by the IUWDSSecretariat,Utrecht, Netherlands

with thp financialassistance of UNESCO

InternationalUrsigram and World
Days Service
I.U.W.D.S.

Synoptic Codesfor
Solar and Geophysical Data
Revised edition
1965

Additional copies may
P. Simon, Observatoire

be obtained from one of fhe following addresses;
de Paris, Meudon

Miss J. V. Lincoln, Deputy Secretary IUWDS(Seine et Oise) France

Steering Committee

Environmental Science Service Administration
Boulder, Colorado, 80301, U.S.A.
PnhlishpH with the finanrialassistance nf UNFSCO

C.R.P.L.

CONTENTS

Page
PART

A GENERAL

INFORMATION

1. Introduction
2. Aims and Structureof IUWDS, and present
membership of the IUWDS Steering Committee
3. Organizationof the Ursigram Service
4. Addresses of the Regional Warning Centers andAssociateRegional Warning Centers
5. Ursigram Broadcasts
6. Areas served by RWC
7. National Warning Contacts
8. Prioritylistfor interchangeamong Regions
PART

CODES

B

I. Solar

OpticalObservations

1.1 Sunspots;USSPO, USSPM, USSPE 34
1.2 Solar Flares;UFLAG, UFLAL, UPAT^
UPATE 41
1.3 Calcium Plages and Centers of Activity;
UPLAG, UPDIE, UACTA 51
1.4 SolarCorona; UCORA 58
1.5 SolarX‑rays; USOXA 61
Solar

Radio

Observations

II. 1 Flux measurements on discrete frequenciesj
URANA,URANP,URANE
II. 2 Spectrograph^ Observations, URANT,URANS
II. 3 Interferometric Observations, URALA,
URALO

33

III. Ionospheric

Observations

III. 1 Critical Frequencies; UFOFA,
UFOFE
III. 2 Sudden Ionospheric Disturbances; USIDA,
UDISE
III. 3 Cosmic Noise Absorption; UABSB
III.4 Combined
Event; UEVTA
IV. Geomagnetic

andauroralactivity

IV. 1 Geomagnetic
Activity Indices and Special
Events; UMAGA
IV. 2 Auroral Observations; UAURA
V. C

osmi

c RaysV. 1 Cosmic
VI. Alert

Ray Events; UCOSA,

UCOSC

Messages

VI. 1 Advice from Regional Warning
ADV‑‑
VI. 2 Alert Messages for the IUWDS;GEOALERT
VII. Specialized

Centers;
ADALERT,

NetworkVII. 1 Radio Propagation Indices; PROPA,
PQ‑,
N‑Q
VII. 2 Radio Propagation Forecasts; PREVI, ST‑,
MT‑, AD‑
VII. 3 Detailed Riometer Data; SRIOD, SRIOM
VII. 4 Detailed Ionospheric Data; ION‑‑
VII. 5 Detailed Cosmic Ray Data; CORAJ,RAYCCPART

C LISTSOF OBSERVATORY

INDICATORS

I. Observatories in numerical Order
II. Observatories in alphabetical OrderPARTD INDEXOF MENTIONED

CODES

PART

A

1. INTRODUCTION.
Summaries of Solar and Geophysical data sent by telegram
or radio broadcast, the so‑called Ursigrams, are normallycast into simple synoptic codes when collected, interchan‑ged and distributed in the rapid exchange plan coordinatedby the International
Ursigram
and
World
Days
Service(IUWDS). This booklet includes the explanationof the codes currently used in this exchange plan.
Only those codes which are in current and widespread use
are included in this booklet. In most cases these are theso‑called Universal interchange codes (identified by key
words beginning with the letter U), which are designed
according to the same principle. Also these codes provide
just the amount of scientific information for which a rapid
exchange is needed. In some cases, however, a more de‑tailed report from a limited number of stationsis needed;
e.g. time variation of cosmic rays during disturbed periods
This type of information can be encoded in the codes, which
are presented in section VII, the Specialized network codes
In some Regions special codes for use in these regions only
have been designed. These regional codes however are pro‑
gressively being replaced by the equivalent universal inter‑change codes. This development
is stimulated by the
IUWDSSteering Committee, because it is felt highly de‑sirable that a uniform system of codes be in use for bothregional and inter‑regional purposes.
A manualcontaining essentially all the solar and geophy‑sical codes in use anywhere during the past decade waspublished in loose leaf form by the URSI Secretariat in1960 with supplements issued when needed. This manual
shouldtobeconsidered

1963.

The

physical

Data

ence

books

code
1963
since

as

the

booklet
and
then.

the

reference

book

for

all

Synoptic

Codes

for

Solar

codes
and

present

bookletaretherefer‑upIn‑

It is to be noted that the present booklet does not include
the COSPAR
Unified Synoptic Codes for rapid communica‑tion of satelliteorbital data, even though this information
passes through some of the same communication
channels
as the solar‑geophysical summaries. The IUWDS
cooperates
with COSPAR
in this work and coordinates the so‑called
SPACEWARN
system for international interchange of satel‑
lite information. The explanation of the codes used in thiswork has been published in COSPAR
Information Bulletin
No. 9 1962.
In designing this present IUWDS
code booklet, we have
tried to make it convenient for the everyday user of the
Ursigrams to work with codes in an efficient and accurate
way. Thus all particulars of a code are to be found in one
place and all codes are described according to the same
scheme. In addition different colours of paper have beenused for codes of different disciplines,and ample space isprovided for notes by the user.
This booklet replaces the one issued in 1963. It is a neces‑sary companion
to the IUWDSManualfor WorldDays,
1966 (issued in CIG News, No. 7‑
and also available separately from the IUWDS
secretaries).
The manual contains all other details of the arrangements
for rapid data exchange as well as the plan for solar andgeophysical alerts and other aspects of the World Days pro‑gram arranged by IUWDS.
The publication and free distribution of this booklet has
been made possible financially by UNESCO
through theFederationof AstronomicalandGeophysical
Services(FAGS), which is the body of the Interna‑
tional Councilof ScientificUnions(ICSU),
that coordinates the work of the Permanent Services of thedifferent Scientific Unions in the field of Astronomy andGeophysics, of which IUWDS
is one.
Though the material presented in this booklet has beenchecked several times, there, no doubt, have remained
inaccuracies and ambiguities. In order to remove theseshortcomings in future editions, the user is invited to makeany criticism known to the IUWDSSecretariat.
Utrecht, September

1965 TheIUWDSSecretaries

J.V. Lincoln

2. AIMSAND

STRUCTURE

OF

IUWDS.

1. Name.
The International Ursigram and World Days Service (IUWDS)
is a Permanent Service of the International Scientific Radio
Union (URSI) in association with the International Astro‑
nomical Union (IAU) and the International Union of Geodesy
and Geophysics (IUGG). The IUWDS
adheres to the Federa‑tion of Astronomical and Geophysical Services (FAGS). The
IUWDS
is a combination (1962) of two former permanent
services, the International World Days Service and the URSI
Central Committee
on Ursigrams.
2. Terms

ofreference.

The service aims to provide information rapidly to the world
scientificcommunity to assistin the planning, coordinationand conduct of scientific work in the relevant disciplines.
These

aims will be achieved by thea. Advance specification of Regular World Days, World
Geophysical Intervals and other periods of geophysical in‑terest, which will be published annually in World Geophy‑sical Caldendars.
b. Collection, coordination, interchange and distribution
by rapid means of selected current observations and infor‑mation of immediate significance to geophysical and spaceresearch and the provision of suitable interchange synoptic
codes.
c. Specification on a current schedule, byAgency, of Solar Activity and Geophysicalcasionally Special World Intervals.

a World Warning
Alerts and oc‑

d. Preparation and publication of periodic post‑facto Calen‑
dar Records of significant indices and outstanding solar andgeophysical events.
e. Untertaking of similar activities in cooperation with theparticipating scientific Unions or other international scien‑tific bodies.
3. Regional

structure.

3.1. In view of par. 2 b and 2 c there shall be Regional
Ursigram and World Days Services in each of the Geograph‑ical Regions. At present (1965) there are four such regions:
Europe and Africa
Western Hemisphere
Western PacificEurasia3.2. In each Region communication
facilitiesare provided
by the respective National communications
services for thecollection and distributionof current observations and in‑formation. One of the centers engaged in this work shallbe designated as the Regional Warning Center, through whichcenter the interchange of data between the regions is ac‑complished. Other centers in this region may be called As‑
sociate Regional Warning Centers.
3.3. One of the Regional Warning Centers shall be desig‑
nated as the World Warning Agency which declares theworld‑wide alerts and special observing periods, with theactive cooperation of the other Regional Warning Centers.

3.4. In each Region there shall be a Regional Ursigram
and World Days Committee, for which rules are given un‑
der par. 5.
4. Steering

Committee.

4.1. The IUWDS
shall be administered by an IUWDS
ing Committee
consisting ofSteer‑

a. One representative from each of the following scien‑tificUnions: URSI; IAU; IUGG.
b. One representative from each of the Regionalgram and World Days Committees.

Ursi‑

c. The IUWDS
tary.

Secre‑

d. TheSecretary and the IUWDSSecretary General of URSI

Deputy(ex. officio).

4.2. In addition the Steering Committee shall have the pow‑
er to seek cooperation, by direct representation or other‑ .
wise, with other international bodies interested in the workof the service. Such relations have been established with
the World Meteorological Organization (WMO), the Special
Committee
for Antarctic Research (SCAR), the Committee
for Space Research (COSPAR), the Solar Particles and Ra‑
diation Monitoring Organization (SPARMO)
and the Inter‑national Geophysical Committee (CIG).
4.3. The Steering Committee
shall elect its Chairman andappoint the two secretaries; the position of these officers
will be reviewed at the occasion of each General Assemblyof URSI.
4.4. The Steering Committee
shall be responsible for theworld‑wide and interregional aspects of the service, foroverall plans and guidance, and for the necessary central
publications.

4.5. The Steering Committee
Warning Agency from among
Centers.
5. Regional

shall designate the World
the existing Regional Warning

Committees.

5.1. Inasmuch as IUWDS
is administered by URSI, theRegional Committees are formed under the auspices of thereleya^t URSI National Committees, with the direct parti‑
cipation, ' if they desire, of National Committeesof IAUand IUGG.
5.2. The Regional Committees
existing in 1962 on Ursi‑
grams were considered to be reconstituted as the nucleusof the Regional Ursigram and World Days Committees with‑out further formality.
5.3. In addition the Regional Committees
shall have thepower to seek cooperation, by direct representation or other‑wise ,with others in the region actively engaged in obtain‑
ing observational data, the communications
network, theRegional Warning Centers and the users.
5.4. The Regional Committees
are responsible for the ac‑tivitiesof the Service in their region, including the col‑lection of information from observatories and the coordi‑
nation and dissemination of summaries and other appropriate
information to the other regions through their Regional Warn‑ing Center, according to the plans set up by the IUWDSSteering Committee.
5.5. Each Regional Committee shall designate the Regional
Warning Center ,for its region and recognize any Associate
Regional Warning Center deemednecessary for the effective
conduct of the work.
5.6. Regional Committees
shall otherwise dispose of thelargest autonomy for the conduct of their own affairs withthe provision that any modification of the interchange codes
to be used and the attribution of indicator numbers of sta‑tions remain matters for the IUWDS exclusivelv.

Present Membership(and address)
Mr. A.H.
Chairman

Shapley,Dr.

Smith‑Rose

R.L.

Dr. H.

Mme.

Uyeda

R.A.

Dr.

A.P.

Dr.

R.

Zevakina

IviitraMichardof Steering

Committee

Representative Western Hemisphere
Regional Committee
ITSA (formerly CRPL) Environmental
Science Services Administration
Boulder. Colorado. 8Q301.

RepresentativeEuropean Regional
Committee
High Winds
Tumble wood Road
Banstead, Surrey, England
RepresentativeWestern PacificRegional Committee
Director,Radio Research Labora‑
toriesKokubunji, P.O. Koganei‑shi
Tokyo, Japan
Representative Eurasian Regional
Committee
Institute of Terrestrial Magnetism,
Ionosphere and Radio Propagation(IZMIRAN)
Leninskii r‑p, P/O Vatutenki
Moscow, USSR
Representative URSI
National Physical Laboratory
Hillside RoadNew Delhi 12, India
Representative IAU
Observatoire de Paris
Meudon (Seine et Oise)France

Dr.

Mr.

Miss

M.

Nicolet

L.D.

J.V.

de

Representative IUGG
Service Du Rayonnement
3 Avenue Circulaire
Uccle, Belgium
FeiterLincoln

SecretaryIUWDS
Sterrewacht "Sonnenborgh"
13, Servaas Bolwerk
Utrecht, The Netherlands
Deputy Secretary IUTO)S^ITSA^formerly CRPyEnvironmental
Science Services
Administration
Boulder,
Colorado,,
U.S.A.

Colonel E. Herbays

3. ORGANIZATION

IRM

Secretary General URSI
7, Place Emile Danco
Brussels 18, Belgium

OF

THE

URSIGRAMSERVICE.

The flow of Solar and Geophysical data summaries ischanneled through the Regional Warning Centers and As‑
sociate Regional Warning Centers. These Centers collectthe information from the observatories within their region,interchange this information, at least once daily, with theother Regional Warning Centers, and distribute the data,
so obtained among the interested observatories and insti‑
tutions within their region. In addition some of these cen‑ters communicate
the information through radio broadcasts.
No special communication
facilitiesare used in this work;
the most effective and economical means available areused and many organizations cooperate most generously inproviding such channels.
The following table illustratesthe flow of current datasummaries among the Regional Warning Centers.

TOKYO

5 = via
6 = via
7 = via
8 = via* Saturday,Sunday only.

1 = direct
2 = via AGIWARN
3 = via Darmstadt
4 = via Parisfromto AGIWARN

NERA
PragueWMO
JJD broadcast

MOSCOW

DARMSTADT

PARIS

NERA

1 = direct
2 = via AGIWARN
3 = via Darmstadt
4 = via Paris

AGIWARNTOKYO
MOSCOW
DARMSTADT
PARIS
NERA
SYDNEYSTOCKHOLM
NEWDELHI
PRAGUEIRKUTSK

fromto SYDNEY

5 =
6 =
7 =
8 =

NEW

via NERA
via Prague
via WMO
via JJD broadcast

STOCKHOLM

DELHI

1
1
1
1

PRAGUEIRKUTSK

Solarand Geophysical stations may contact the appropriate
Regional Warning Center regarding arrangements for receiv‑
ing by, telegram or mail, the Solar‑Geophysical data sum‑maries. In each Region there are also Regional Committees
for this work, and the national memberof this Committee
is often in a position to help with such arrangements.
On the basis of the current observation summaries whichflow through the Ursigram network, each Regional Warning
Center issues whatever messages are appropriate. Someofthese are ADVANCEALERTSof really outstanding solar or
geophysical events and are given even wider distribution
within the region and are interchanged among the RWC's.
Once each day, the RWC
designated as the IUWDS
WorldWarning Agency, issues, when appropriate, a world‑wide
Alert, a GEOALERT,
which is given still broader distri‑bution through the cooperation of the WMO
meteorologicaltelecommunication
network. A detailed plan of the systemof alertsIUWDS has been described in the IUWDS Instruc‑tion‑Manual
for the World
Days
Program.

4. REGIONALWARNINGCENTERSADDRESSES

The addresses and other information for the various RWC's
are
stationsto establish
givencommunication
below to enablegeophysicalsuitablechannels
for receipt and trans‑mission of data.
1. IUWDS

World

Mail:

Box 178, Ft. Relvoir, Virginia,
22060, U.S.A.

Telephone:

Washington, D.C.
,780‑1444
1436

WASHINGTON
Cable and Radiogram: AGIWARN(Commercial)
AGIWARNWUXTelegraphic:
WASH
DC(Commercial)703‑339‑5771
TWX:
Government Teletype: AGIWARNESSA FT BELVOIR VA
Operating Organization: Telecommunications and Space Dis‑In Charge:

turbance ServicesCenterBox 178, Ft. Belvoir, Va. 22060
U.S.A. (E.J. Wiewara, Engineer‑in‑Charge)
Kent D. Boggs
Head, World Warning Agency

General Supervisor:

Dutch Section 2.1.1
Mail:
Telegraph:
Telex:
Supervisory:
Immediate
Charge:Paris Section 2.1.2
Mail:

2. Regional

Warning

2.1 Western

EuropeCenters

Radio Receiving Station NERA
Nederhorst den Berg
The Netherlands
AGI NEDERHORSTDENBERG"Amsterdam 12308

T.C. Dito (PTT Leidschendam)

H. VanLohuizen

Telegraph:

Service des Ursigrammes
Mondiaux
Observatoire de Paris
Meudon (Seine et Oise)FranceCNETAGI

Telex:

25312

TelephoneSupervisory:
Immediate
Charge:R. Michard
P. Simonet Jours

Darmstadt
Mail:

Section 2.1.3
FTZ
Rheinstrasse 110, 61 Darmstadt
Federal Republic of Germany

IONOSPHAERE

Telegraph:

DARMSTADT

Telex:

4‑189291

Telephone:Darmstadt 83‑2530 (Beckmann)
2549 (Ochs)
2533 (Richter)

Supervisory:

B. Beckmann
Asst. : A. Ochs

Immediate

G.

Charge:Richter

2. 2 Eurasia
Mail:

Telegraph:
Telephone:Supervisory:
Immediate Charge:

Institute of TerrestrialMagnetism,
Ionosphere and Radio Propagation(IZMIRAN)
Leninskii r‑p, P/O Vatutenki
Moscow. USSRNIZMIR MOSCOWr^t)3‑50
B2‑19‑21,

Mme.
Mme.

R.A. Zevakina

L.N.

Liakhova

2.3 Western Pacific
Mail:

Radio Research Laboratories
Ministry of Posts and Telecommuni‑
cations
Kokubunji P.O. Koganei‑shi,Tokvo

Telegrams:

DEMPA TOKYO
20‑219‑12 (DEMPA

Telex:

Telephone:Supervisory:
Immediate
Charge:042321‑1211

H. Uyeda
K. Kondo

TAC)

T elex:

Telephone:Supervisory:
Immediate
Charge:1208 (radiogen sth)1734 (radiocentr stkm)
Stockholm

94‑00‑00

ext. 2105

P. $kerlind
G. Malmgren
3.3 India

Mail:

Telegraph:

Telephone:Supervisory:

Associate Regional Warning Center(IUWDS)
National Physical Laboratory
New Delhi 12, India
NATPHYLAB

55298, 53051. 52045
A. P. Mitra
3.4 Czechoslovakia

Telegraph:

Czechoslovak Academyof Sciences
Geophysical InstituteIonosphere De‑partment
Praha 4, Sporilov, Czechoslovakia
MEGER
PRAHA

T elex:ION PRUHONICE

Mail:

Telephone:Supervisory:
Immediate
Charge:923796
P. Triska
K. Dobi ￡s00346

3.5 U.S.S.R.
Mail:

Telephone:Supervisory:

Siberian Instituteof Terrestrial
Magnetism, Ionosphere and Radio
Propagation (Sib IZMIR)
Irkutsk 3, Box 65, U.S.S.R.
55‑66: 63‑48

E.S. Kazimirovsky

AREASRWC

SERVED

BY

AGIWARN

Argentina
Bolivia
BrazilCanadaChile
Colombia
Cuba
GuatemalaMexicoPeru
Philippines
Trinidad
USA
Venezuela
ARWC
SydneyRWC

WARNINGRWC

CENTERSIZMIRAN

Bulgaria
German Dem. Rep.
Hungary
Korea Dem. Rep.
Mongolia P.R.
PolandRumania
USSR
Viet‑Nam Dem. Rep.
Yugoslavia
ARWC Irkutsk
ARWC New Delhi
ARWC Prague

RWC

Austria
Belgium
German Dem. Rep.
Germany, Fed. Rep.
Greece
ARWC
Prague
ARWC
Stockholm+ RWC

REGIONAL

receives only.

FranceGerman Dem. Rep.
Germany, Fed. Rep.
Netherlands
Surinam
ARWC Prague
ARWC Stockholm

RWC

Paris

RWC

+ Belgium
France+ Greece+ Italy+ Malagasy Rep.
+ Overseas French Stations+ Spain* Senegal* South Africa* United Kingdom

Tokyo**. Burma** Hong Kong** Indonesia
Japan** New Zealand** Philippines* * Taiwan* * ARWC
New Delhi
ARWC
Sydney**(Europe, Africa)**ARWCNew Delhi
ARWC
Prague

ARWC

Stockholm: Finland,

ARWC

Prague: (assumed)

Sweden.

Bulgaria,

GermanCzechoslovakia,

Dem.Rep.

Poland,,Hungary,

Rumania,

ARWC

Irkutsk: Siberia.

ARWC

Sydney: Australia,

ARWC

New

Delhi

: India,

Yugoslavia.

*

**

New

Burma,

Zealand.

**

Ceylon,

**

stan.

+ RWC
* RWC
**some
RWC.

receives only.
sends only.
areas which,inprinciple,

receivebroadcasts

Paki‑

NATIONALWARNINGCONTACTS(as of September
Argentina
Servicio Meteoroldgico
Nacional,
Paseo Col6n 317 ‑ 2° Piso,
Buenos Aires.
Australia
Mr. F.F. Cook,
Ionospheric Prediction
Service,CommonwealthCentre,Chifley Square,
Sydney, N.S.W.

1965)

CNRE,
3, Avenue
Circulaire,
Bruxelles 18.
Cables: CENTRESPACEBRUXELLES
Telephone: 02‑74.27.28
Telex: 2‑21563.‑ CENTRE‑SPACE BRU.
BrazilDr. Fernando de Mendonga,
Scientific Director,

Cables: IPSO SYDNEY
Telephone: 20340

Comissao Nacional de Ati‑
vidades Espaciais,
Sao Jos￡ dos Campos,
Sao Paulo.

Austria

Bulgaria

Prof.Dr. Ferdinand Stein‑hauser, Director,
Zentralanstalt fttrMeteoro‑
logie und Geodynamik,
Hohe Warte 38,
Vienna 19.

Hydro‑Meteorological
Service,boul. Lenin 146,
Sofia.

Telex: 07‑4337
Belgium
Prof. M.

Nicolet,Telegraph: SOFIA, MGSS
Telex: SOFIA, H METEORSS 542
Telephone: Sofia, 1‑22‑71,
7‑24‑50
Immediate
Charge: Sasho
Mulushev.

CanadaL ￡opoldville.

Mr. C. Collins,
Divisionof Pure Physics,
National Research Council,
Ottawa 2.

Telegraph: COUMET/LEO

Cables: RESEARCH

Director,
Observatorio Nacional,
Casa Blanca,
La HabanaOTTAWA

CeylonMr. R. Mahadeva,
Secretary,
Ceylon National Committee
for IQSY,
Departmen of Meteorology,
BullersRoad,
Colombo 7.
China,

Republicof

Mr. Miao Tsao‑vong,
DirectorateGeneral of Tele‑
communications ,Ministryof Communications,Taipei, Taiwan.
Columbia
Director Escuela Naval
Cadetes
Cartagena
Congo

( L

opoldv i11 e )Monsieur M. Clerebaut,Service M ￡t￡orologique,

Cuba

Cables: CLIMATO‑HABANA
Telephone: 60‑1231
Czechoslovakia
Geophysical Instituteof the
Czechoslovak Academyof Sciences,
Praha
4,
Sporilov.
Cables:MEGER
PRAHA
Telex: 00346‑ION
PRU‑
HONICE
Telephone: 92 37 96,
99 22 04
Supervisory: P. Triska
Immediate
Charge: K. Dobi3s

F i nla nd
Mr. T. Haikonen,
General Direction of Posts
and Telegraphs,
Mannerheimint, 9,Helsinki.

FranceAthens.

Monsieur R. Mi chard,
Service Solaire,
Observatoire de Paris,
Meudon, (S‑et‑O).

Cables: IQSY ATHENSSpecial Cables: LGGMYMMETAXAS
GuatemalaGermanRepublic

Democratic

Dr. H. Runge,
Hauptwetterdienststelle,
Potsdam.
Cables: WETTER
Telex: 015 116

POTSDAM

Engr. Haroldo Duarte
Villela,Chief of Geophysics Section,
Direcci6n General de Carto‑
grafia,Avenida "Las Americas"
5‑76,
Zona 13, Guatemala
City,
C. A.

GermanFederalR e pub li c

Telephone:

FTE Arbeitsgemeinschaft
Ionosphaere

IcelandRheinstrasse 110,
61 Darmstadt.

Dr. Th. Saemundsson,
B61stadarhlfd 14,
Reykjavfk.

63281‑2‑3

Ghana
India
Chief Meteorological Officer
Meteorological Office,
P.O. Box 744,
Accra.
GreeceDenis Metaxas,
Meteorological Centre,
Hellenikon Airport,

Mr. P. R. Krishna Rao,
Director‑General of Observ‑
atories,
India Meteorological De‑
partment,
New Delhi 3.

Ireland
Director,
Meteorological Service,
44 Upper O'Connell Street,
Dublin.

Cables: DEMPA
KOKUBUNJI
Supervisory: Hiroyuki Uyeda
Immediate
Charge: Toohio )Takignohi.
Korea,
Democratic
People's
Republicof

ItalyProf. M. Giorgi,
Consiglio Nazionale delle
Ricerche,
Piazzale delle Scienze 7,
Rome.
Cables: CORICERCHE‑AGI ROMA
Telephone: 490.151.

Lie Rak Bok,
Astronomical Observatory,
Pyongyang.
Korea,

Republic

Prof.Dr. Nyong

ofD. Kwon,c/o National Academyof
Sciences, ROK,San 2‑1, Samchung‑dong,
Chongno‑koo,Seoul.

Jamaica
Mr. C.R. Dickenson,
Jamaica Telephone Com‑
pany,
P.O. Box 21,
Kingston 5.

Cables: IQSYCENTRE
SEOULNetherlands
Receiving Station NERA

of

Cables: COTELKINGSTON
Telephone: 68131

the Netherlands PTT,
Nederhorst den Berg.

Japan

Telegraph: AGI NEDER‑
HORSTDENBERG
Telex: AMSTERDAM
12308

Radio Research Laboratories,
Ministry of Posts and Tele‑
communications,
Kokubunji P.O.,
Koganei‑shi,Tokyo.

New

Zealand

The Director,
New Zealand Meteorological
Service.

Lima.

P.O. Box 722,
Wellington.
Cables: WEATHERLINGTON

Cables: AGI

LIMA

Phi li ppine

s

WEL‑

Nigeria
The Senior Meteorologist,
Meteorological Service,
Airport,Kano.
T elephone:
Office ‑ Kano 2631 or 3011,
Ext. 121.
Residence ‑ Kano 2586.
Deputy Forecaster,
Telephone: Kano 3011,
Ext. 102.

Pakistan
Mr. A. W. Kahn
Deputy Director,
Pakistan Meteorological
Service,
Secretariat Blocks 1‑3,
Frere Road, Karachi 3.
Cables: METEOR
Peru
Major Juan Ernesto Barreda,
Institute Geofisico del Peru,
Ministerio de Fomento,
Apartado 3747,

The Director,
Weather Bureau,
Department of Commerceand Industry,
Manila,P.O. Box 2277.
Portuga

1

The Director,
Servigio Meteorol<5gico
Nacional,
Rua Saraiva de Carvalho 2,
Lisboa 3.
Cables: METEOLISB
Telephone: 662188
663543.

Rhodesia
Nyasaland

andMr. A.C.

Iauld,

andFederal Department of Tri‑gonometrical and Topo‑graphical Surveys,
P.O. Box 8181
Causeway,
Salisbury

SierraLeone

UnitedKingdom

TheDirector,
MeteorologicalDepartment,
LungiAirport.

Mr.A.F.Wilkins,
DSIRRadio
Station.

DittonPark,
Slough,Bucks.
SouthAfrica
Mr.G.H.Oosthuizen,
ScienceCooperation
Division,CSIR,
P.O.Box395,
Pretoria.
Cables:NAVORS
Telephone:74‑6011.
Spain
Rev.FaObserva
ApartadTortosa.

UnitedArabRepublic
Dr.M.F.Taha,
MeteorologicalDept.,
MinistryofWar,
KoubryEl‑Quobba,
Cairo.
Cables:WEATHERCAIRO.

Cables:RADSEARCHSLOUGH
Telephone:Slough24411.
UnitedStatesof
America

MissJ.VirginiaLincoln,
DeputyChief^ITSADataServices
EnvironmentalScienceServices
Administration,Boulder,Colorado, 80302,U.S.A.
Viet‑Nam,Demo‑craticRepublicof
Nguyen‑Xien,M^teorolo
giste,
ServiceM ￡t￡ orologique,Hanoi.

6. PRIORITY
Priority

LIST FOR DATA
Wor l d ‑ w i d e

I

data

eac h

RWC.

dat a

are

UFLAL

available

these
among

Solar
and

‑ Solarof

the

Flare,

RWC's)

Solar

Ionospheric

Flares,at

categories

interchanged

Noise
UFLAG,

normally(i.e.

‑ Combined

UEVTA

INTERCHANGE.

Ralio

event.

opticalv^L

importance2

orgreater.
URANA,URANP‑ Solar

Radio

Noise

‑ SolarRadio

Spectra.

‑ Solar

Radio

Noise

at

about

200

Mc/s;

at

3000

Mc/s;

events.
URANT,

URANS

URANE

and
UABSB

‑ Other

ionosphericincluding
USIDA

flux

events.
absorption

polar‑ Suddencap

Ionosphericportance

2

SEA,

Disturbance,orgreater,SCNA,

UCOSA,UCOSC‑ Cosmic

UPATA,UPATE‑ Observing

SPA,
ray

general

for

data.

optical

which

first

corona

(only

SWF,

SFD.

flux
of

im‑

including
SES,

hours

patrols

events,absorption.

solar

flare

analysis

has

bee

made.
UCORA

‑ Eastlimb

5694
URALA,URALO%‑ Locationsor
AD

UPDIE,UAC TA
ALERT

solar

‑ The

exceptdaily

enhanced

in

of
by

solar

the

from

servatoryper
X‑rays.

activecenter:Alertnormallytheregionone
region.

oforigincontaining

world‑wideWorldissueddistribute<

Message

K‑figuresformationofAdvance

Warning‑ Geomagnetic‑ Solarof
notdeclarations

USOXA

of

activity

regions;issued
UMAGA

line,

chromosphere.
copy

all

further,
GEOALERT

sourcesandthe‑ AdvisoryinyellowI).

noise.

‑ Locationinpriorityofradio
UPLAG,

has

Alerts,Warningandrepresentativeas

Agency.
storm

in‑
ob‑

RWC
will normally have data from its
own region (i.e. these categories ofdata are not regularly interchanged
among the RWC's).
‑ Sunspot data.
‑ Sudden ionospheric disturbances with
an importance smaller than 2.
‑ Solar flares with an importance small
er than 2.
‑ Ionospheric radio propagation disturb‑
ance.
‑ Ionospheric critical frequencies.
‑ Intensitiesof coronal line emission,
including green line 5303 5 .
‑ Auroral observations.
In case of the necessity of limiting message length,
the centers should include data types in order of
the above list.
Flares of importance 1 should be sent whenated with great terrestrialevents.

associ‑

Also SID of importance 1 associated with greatflares should be reported.

NOTESB.I. Solar

OpticalObservations

1.1 Sunspots
Code 1; USSPO
Code 2; USSPM
Code 3; USSPE
1.2 Solar Flares
Code 1; UFLAG
Code 2; UFLAL
Code 3; UPATA
Code 4; UPATE
1.3 Calcium Plages and Centers of Activity
Code 1; UPLAG
Code
2 jUPDIE
Code 3;UACTA
1.4 Solar Corona
Code 1; UCORA
1.5 Solar X‑rays
Code 1: USOXA

B.I.ICode

SUNSPOTS
1. USSPO

1. Content.
Relative sunspot number
General activity indices for disk and limb
Area, position, importance, stage of evolution and Brun‑ner type of spot groups
2. General

3. Definition

form.

of

symbols.

USSPO = key word, sunspots
JJ = Greenwich date of observation
T = time of observation in tenths of the Greenwich day
II = observatory indicator (see also listsin part C)

01 = Arcetri
04 = Herstmonceux
07 = Kodaikanal
09 = Mt. Wilson
11 = Ondrejov
13 = Tashkent
14 = Belgrade
15 = Ziirich
16 = KanzelhQhe
17 = Schauinsland
18 = Wendelstein
20 = San Miguel
21 = Tortosa

29 = Locarno
30 = Arosa
31 = USNO Washing‑ton
32 = Sacramento Peak
37 = Dunsink‑Dublin
40 = Culgoora
46 = NERA
49 ‑‑Rome
51 = Mitaka
54 = Wellington
55 = Manila
59 = Baguio

62 = Freiburg
79 ‑ Moscow
80 = Irkutsk
81 =83 = Athens
86 = Voroshilo

87 = Kislovodsk
89 = Abastumani
92 = Potsdam
93 = Wroclaw
96 = Lvov
97 = Ljubljana
99 = Bucharest

aaa = relative sunspot number (R) and observing conditions
if observing conditions are good 600 is added to R
if observing conditions are fair 300 is added to R
if observing conditions are poor R is left unchangedb = general activity index for the disk in a scale from
1 to 5j 1 means small, 5 means great activity
c = general activity index for the limb; samefor bscale asee = serial number of spot group, assigned by the reporting
observatory on the basis of observations on precedingdays
fff = area of spot group in tens of millionths of the solar
hemisphere
Q = Quadrant (heliographic coordinates) in which the spotgroup is situated
1 = NE (north‑east)
4 = NW (north‑west)
2 = SE (south‑east)
3 = SW (south‑west)XX= distance to central meridian in degrees

YY= heliographic latitude in degrees

importance of spot group on a scale of 1 to 3, com‑bined with information on the stage of evolution
increasing stage
increasing stage
increasing stage
stablestablestabledecreasing stage
decreasing stage
decreasing stage
given
number of days group observed since limb
firstappearance on disk
1 = A
2 = B
3 = C
kk = number

4 = D
5 = E
6 = F
of spots counted in the group

NOTES

passage or

7 = G
8 = H
9 = I

B.I.ISUNSPOTS

Code 2. USSPM
1. Content.
Relative sunspot number
General activity indices for disk and limb
Area, position, importance, magnetic and Brunnerof sunspot groups, spot count

key word
3. Definition
USSPM

of

symbols.

= key word, sunspots
and especially their magnetic
JJ = Greenwich

type

date of observation

T = time of observation in tenths of the GreenwichdayII = observatory indicator (see also lists in part C)
09 ‑‑ Mt. Wilson 79 = Moscow
92 = Potsdam
jtewJLaaa = relative sunspot number (R) and observing condi‑
tions
if observing conditions are good 600 is added to R
if observing conditions are fair 300 is added to R
if observing conditions are poor R is left unchangedb = general activity index for the disk in a scalefrom 1 to 5; 1 means small, 5 means great activity
c = general activity index for the limb; same
as for b

scale

ee = serial number of spot groups assigned by the re‑porting observatory, on the basis of observations
on preceding days
fffarea of spot group in'tens of millionths of thesolar hemisphereQ = quadrant (heliographic coordinates) in which the
spot group is situated
1 = NE (north‑east)
4 = NW(north‑west)
2 = SE (south‑east)
3 = SW (south‑west)XX= distance to central meridian in degrees

YY= heliographic latitude in degrees
g = importanceof spot group in a scale of 1 to 3m

= magnetic classificationof the spot group
1 ‑ alpha 2 = beta 3 = beta/gamma
4 = gamma
5 = delta configuration 1)
i = Rrunner classification
1 = A
4 = D
7 = G
2 = B
5 = E
8 = H
3 = C
6 = F
9 =

kk = numberof spots counted in the group1) delta configuration consistsof spots of opposite polarity‑
separated by,more than 2^/vithinthe same penumbra.

SUNSPOTS

B.I. 1
Code 3. USSPE
1. Content.

Relative sunspot number
General activity indices for disk and limb
Position, importance and Brunner type of sunspot groups

3. Definition
USSPE

of

symbols.

= key word, sunspots

JJ = Greenwich

date of observation

T = time of observation in tenths of the Greenwich

day

II = observatory indicator (see also lists in part C) 40
Culgoora
aaa = relative sunspot number (R) and observing condi‑
tions
if observing conditions are good 600 is added to R

if observing conditions are fair 300 is added to R
if observing conditions are poor R is left unchangedb = general activity index for the disk in a scale from
1 to 5; 1 means small, 5 means great activity
c = general activity index for the limb; same
as for b

scale

Q = Quadrant (heliographic coordinates) in which the
spot group is situated
1 = NE (north‑east)
4 = NW (north‑west)
2 = SE (south‑east)
3 = SW (south‑west)XX= distance to central meridian in degrees

YY= heliographic latitude in degrees

g = importanceof spot group on scale of 1 to 3

i = number of days group observed since limb
or first appearance on disk
j ‑ Brunner classification
1 = A
4 = D
5 ‑ E
2 = B
6 ‑ F
3 = C
kk = numberof spots counted in the grouppassage

7 = G
8 = H
9 =

B.I.2

SOLAR

FLARES

Code 1. UFLAG
1. Content.
Position, importance and duration of solar flares as re‑ported, by a single observatory to be used
begin‑
ning January
1, 1966,in conformance with therecommendationsof IAU Commission
10.

3. Definition
UFLAG

of

symbols.

= key word, solar flares
JJ = Greenwich

date of observation

U = quality of observation;
1 = poor, 2= fair, 3= goodII = observatory indicator (see also lists in part C)

01 Arcetri
02 Catania
04
05 Herstmonceux
Huancayo

10 Meudon
06 Kharkov
07 Kodaikanal 11 Ondrejov
08 McMath
09 Mt. Wilson 13
15 Tashkent
Ztirich16 KanzelhOhe
17 Schauinsland
18 Wendelstein
19 Stockholm
20 San Miguel
21 Tortosa
22 Anacapri‑S
29 Locarno
30 Arosa
32 Sacramento
Peak
34 Climax

37 Dunsink
40 Culgoora
41

46 NERA47 Anacapri‑G
48 Nizamiah
51 Mitaka
53 Utrecht
54 Wellington
57 Ottawa
59 Quezon
64 Uccle

City

78 Burba nk
79 Moscow
80 Irkutsk
81 Kiev
83 Athens
86 Voroshilov
88 Alma‑Ata
89 Abastumani
91 Nanking
94 Capetown
96 Lvov
99 Bucharest

Q = quadrant (heliographic coordinates) in which theflare is observed
1 = NE (north‑east)
4 = NW(north‑west)
2 = SE (south‑east)= SW (south‑west)
distance to central meridian in degrees
heliographic latitude in degrees
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
4 = First observation of a flare in progress, endof flare not observed
5 =6 = Time of maximumof flare
7 = Time of secondary maximumof flare8 =9 = Nominal time of beginning of a subflaretime in hours and minutes (UT)
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 = importance3 = importance
4 = importance2; area 5.2‑12.4 square degrees
3; area 12.5‑24.7 square degrees
4; area >24.7
square degrees

importance based uponation
7 = faint
8 = normal
9 = brilliant

relative intensity evalu‑

duration or period of observation of the flare, in
minutes, depending on whether the indicator P
in previous group is 1 or 2, 3, 4. If no good
estimate of the duration can be given use DDD=000

As many times (PHHmm)
as are significant may
be given to describe a flare, in order of increas‑
ing value of the time indicator P. Also,a second(and third, etc. ) flare in the same region may
be fully reported without ambiguity without re‑peating the groups UFLAGJJUII QXXYY.

B.I.2 SOLAR

FLARES

Code 2. UFLAL
1. Content
report on a flare, based upon observations of several ob‑
servatories,or revised flare data from one observatory

3. Definition
UFLAL

of

symbols.

= key word of code giving correction to previously
sent UFLAG
message or a composite report fromseveral observatories
JJ = Greenwich
a = number

date of observationof observatories reporting the flare

II = observatory indicator, if composite report, insert
XX (or slant line in teletype message) (see also
lists in Part C)

01 Arcetri
02 Catania
04 Herstmonceux
05 Huancayo
06 Kharkov
07 Kodaikanal
08 McMath
09 Mt. Wilson
10 Meudon
11 Ondrejov
13 Tashkent
15 Ztlrich
16 KanzelhOhe
17 Schauinsland
18 Wendelstein
19 Stockholm

20 San Miguel
21 Tortosa
22 Anacapri‑S
29 Locarno
30 Arosa
32 Sacramento
Peak
34 Climax
37 Dunsink
40 Culgoora
41

46 NERA47 Anacapri‑G
48 Nizamiah
51 Mitaka
53 Utrecht

54 Wellington
57 Ottawa
59 Quezon City
64 Uccle
78 Burbank
79 Moscow
80 Irkutsk
81 Kiev
83 Athens
86 Voroshilov
t88 Alma‑Ata
89 Abastumani
91 Nanking
96 Lvov
94 Capetown
99 Bucharest

Q ‑ quadrant (heliographic coordinates) containing theflare (clockwise direction)
1 = NE (north‑east)
2 = SE (south‑east)
3 = SW (south‑west)
4 = NW (north‑west)XX= distance to central meridian in degrees

YY= heliographic latitude, in degrees

b = importance, or revised importance, based upon"corrected" area in square degrees
0 = subflare (S)j area < 2.0 square degrees
1 = importance lj 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
HHmm= time, or revised time, of beginning in hours andminutes UT
C = importance
7 = faint

based upon

relative intensity evaluation

8 = normal
9 = brilliant
HHmm= time, or revised time, of maximum
minutes UT

in hours andB.I.2 SOLAR

FLARES

Code 3. UPATA
1. Content.
solar flare survey intervals for Ha
ographic
only

3. Definition
UPATA

of

patrols, cinemat‑

symbols.

= key word, flare patrol hours, photographic
JJ =Greenwichdate of observation

U = overall quality of observations
0 = no data 1 = poor 2 = fair 3= goodII = observatory indicator (see also lists in part C)

07 = Kodaikanal
08 = McMath

11 =
13 =
15 =
16 =
17 =
18 =
19 =

09 = Mt. Wilson
10 = Meudon

20 = San Miguel
21 = Tortosa

01 = Arcetri
02 = Catania
04 = Herstmonceux
05 = Huancayo
06 = Kharkov

Ondrejov
Tashkent
ZtlrichKanzelhChe
Schauinsland
Wendelstein
Stockholm

22 = Anacapri‑S
29 = Locarno
30 = Arosa32 = SacramentoPeak
34 = Climax
37 = Dunsink
40 = Culzoora
41 =46 = NERA
47 = Anacapri‑G
48 = Nizamiah
51 = Mitaka
53 = Utrecht
54 = Wellington
57 = Ottawa

59 =
64 =
78 =
79 =
80 =
81 =
83 =

Quezon City
Uccle
Burbank
Moscow
Irkutsk
Kiev
Athens

85 =
86 =
88 =
91 =
94 =
99 =

SimeizVoroshilov
Alma‑Ata
Nanking
Capetown
Bucharest

UT of beginning of patrol period in hours andtenths of hours
UT of end of patrol period, in hours and tenthsof hours, withtens digit
suppressed.

Repeat "UPATAJJUII" whenever observing period
covers two (universal time) dates. If ambiguity,
possible upon decoding insert an extra group"aaabb".
UPATA
sent only if the flare observations havebeen reduced and are being reported in the samemessage.

B.I.2 SOLAR

FLARES

Code 4. UPATE
1. Content
solarflaresurvey intervalsfor H a patrols,visual
only

3. Definition
UPATE

of

symbols.

= key word, flare patrol hours, visual
JJ = Greenwich

date of observation

U = overall quality of observations
0 = no data 1 = poor 2 = fair 3= goodII = observatorv indicator (see also lists in part <
01 =
02 =
04 =
05 =
06 =
07 =
08 =
09 =
10 =

Arcetri
Catania
Herstmonceux
Huancayo
Kharkov
Kodaikanal
McMathMt. Wilson
Meudon

11
13 ==
15 =
16 =
17 =
18 =
19 =
20 =
21 =

Ondrejov
Tashkent
ZttrichKanzeUiShe
Schauinsland
Wendelstein
Stockholm
San Miguel
Tortosa

22 = Anacapri‑S
29 = Locarno
30 = Arosa32 = SacramentoPeak
34 = Climax
37 = Duns ink
40 = Culgoora
41 = Honolulu

46 =
47 =
48 =
51 =
53 =
54 =
57 =

NERA
Anacapri‑G
Nizamiah
MitakaUtrecht
Wellington
Ottawa59 = Queron City
64 = Uccle
78 = Burbank
79 = Moscow
80 = Irkutsk
81 = Kiev
83 = Athens

85 =
86 =
88 =
91 =
94 =
99 =

SimeizVoroshilov
Alma‑Ata
Nanking
Capetown
Bucharest

UT of beginning of patrol period in hours andtenths of hours
UT of end of patrol period, in hours and tenthsof hours with tens digit suppressed

Repeat "UPATEJJUII" wheneverobserving period
covers two (universal time) dates. If ambiguity
possible upon decoding insert an extra group"aaabb".
UPATEsent only if the flare observations havebeen reduced and are being reported in same

B.I.3 CALCIUM

PLAGESAND
ACTIVITYCENTERSOF

Code 1. UPLAG
1. Content.
Area,・ importance and intensityof calcium pages

3. Definitionofsymbols＼G = keyword, plages
JJ = Greenwich day of observation
T = time of observation in tenths of the Greenwich day
II = station indicator (see also lists in part C)
08 McMath
Hulbert 10 Meudon
59 Quezon Citv
q = quality of observation in a scale from 1 to 5;
1 means very poor, 5 means excellentnumber of days since last message from this station
always xx (or slant bar in teletype messages)
number of plages (three five‑digit groups each)for which information will follow.
serial number, assigned by observatory
importance of plage region on a scale of 1 to 3
combined with information on the stage of evolution
1 = importance 1, increasing stage
2 = importance 2, increasing stage
3 = importance 3, increasing stage
4 = importance 1, stable
5 = importance 2, stable
6 = importance 3, stable
7 = importance 1, decreasing stage
8 = importance 2, decreasing stage
9 = importance 3, decreasing stage
X = no evaluation given
age of the region
1 = born on disk
2 = born on invisiblehemisphere, firstdisk transit
3 = second disk transit
4 = thirdetc.
9 = eighth disk transit
X = no evaluation givenXX
YY

quadrant (heliographic coordinates) containing theplage
1 = NE (north‑east)
4 ‑ NW(north‑west)
2 = SE (south‑east)= SW (south‑west)= distance to the central meridian in degrees= heliographic latitude in degrees

iii = area in millionths of the solar hemisphere, di‑vided by 100
i = 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.

B.I.3 CALCIUM

PLAGESAND
ACTIVITYCENTERSOF

Code 2. UPDIE
1. Content
Disappearances of filaments, dark surges on the disk,
loop and surge prominences at the limb (normally Ha
observations)‑ Position, importance and time of occurrence .

3. Definition
UPDIE

of

symbols.

= key word, prominenceof filaments

activity or disappearances

JJ = Greenwich date of observation
U = overall quality of observation
0 = no data
1 = poor
2 = fair
3 = good
II = observatory indicator (see also listsin part C)
08 = McMath
Hulbert 10= Meudon11 = Ondrejov
32 = Sacramento
34 = Climax

40 = Culgoora
Peak

59 = Quezon
64 = Uccle

City

Q = quadrant (heliographic coordinates) in which pheno‑menon is observed
1 = NE (north‑east)
4 = NW(north‑west)
2 = SE (south‑east)
3 = SW (south‑west)XX
YY= distance to central meridian in degrees= heliographic latitude in degrees

a = type of phenomenon
1 = disappearance of major filament (SDF) between
morning observation and afternoon observation
2 = disappearance of major filament (SDF); 1 day
interval between disappearance and when fila‑
ment was still visible.3‑*=disappearance of major filament (SDF); 2 days
interval between disappearance and when fila‑
ment was still visible
5 =6 = bright surge on disk (BSD)
i 7
surge
on disk (DSD)
fe.* ―.― ―UT= loop prominence at limb (APR)
9 = bright surge at limb (BSL)
HHmm=hour and minutes UT of phenomenon
for a = 1,
2 or 3, it is the time of first observation after
the disappearance; for a = 7, 8 or 9, it is thetime of beginning of the phenomenonb = importance (for disappearances importance of fila‑
ment before disappearance)
1 = slight 2= moderate 3=‑ highHHmm=hour and minutes UT of end (or *Sft)B.I.3 CALCIUM

Code

PLAGESAND
ACTIVITYCENTERSOF

3. UACTA

1. Content.
calcium plage position, area and intensityj magnetic
and Brunner type of sunspot, and spot count within theplage

3. Definition
TAofsymbols.

= key word, active center, code

A

JJ = Greenwich date of observation
T = time of observation in tenths of the Greenwich day
II = observatory indicator (see also lists in part C)
08 = MacMath 10= Meudon 59= Quezon Citya = quality of observation
1 = poor 2= fair 3= goodb = number of days since last message fromtory given in II
cc = number of active centers describedd = number of centers with sunspots

observa‑e = indicator, if center contains sunspots e = 9, or
if no sunspots e = 6
ff = serial number of centerg = importance of spot group on a scale of 1 to 3,
combined with information on the stage of evo‑lution1 = importance 1, increasing stage
2 = importance 2, increasing stage
3 = importance 3, increasing stage
4 = importance 1, stable
5 = importance 2, stable
6 = importance 3, stable
7 = importance 1, decreasing stage
8 = importance 2, decreasing stage
9 = importance 3, decreasing stage
X = no evaluation given (slant bar on teletype)h = age of the center
1 = born on disk
2 = born on invisible hemisphere, firstdisk transit
3 = second disk transit
4 = thirdetc.
9 = eighth disk transit
X = no evaluation given (slant bar on teletype)

Q =

XX
YY

containing thequadrant (heliographic coordinates)
plage
■ .
4
=
NW
(north‑west)
1 = NE (north‑east)= SW (south‑west)
2 = SE (south‑east)= distance to the central meridian in degrees= heliographic latitude in degrees

iii = area in millionths of the solar hemisphere, di‑vided by 100
i = i
7 = 4.0
4 = 2.5
1 = (faint)
8 = 4.5
5 = 3.0
2 = 1.5
9 = 5.0 (very bright)
6 = 3.5
3 = 2.0
check, units digit of sum of preceding 14 digits
if center has no sunspots or X (slant bar on tele‑type) if center contains sunspots
magnetic classificationof sunspot group
1 = alpha 2 = beta 3 = beta gamma
4 = gamma
Brunner tvoe of
7
=
G
4 = D
1 = A
8 = H
5 = E
2 = B
9 = J
6 = F
3 = C
im = number of spots counted in the groupo = check, units digit of sum of preceding 19 digits

The group "effgh" begins the descript^Snof anactive center.Beginning with "6"・or''9"thecenter is identifiedwithout ambiguity, especiallywith the serialnumber following.The group"QXXYY" begins with 1 to 4, "iii" has little
chance of beginning with "5" or "6" and "1" isbetween 1 to 4. The informationgiven for thesunspot groups is succinct,but rapidlycoded byobserver,and it is hoped that the magnetic typewill be routinelygiven.

B.I.4 SOLAR

CORONA

Code 1. UCORA
1. Content.
Intensity of coronal line emission as a function of helio‑graphic latitude

3. Definition
UCORA

of

symbols.

= key word, corona
JJ = Greenwich date of observation
T = time of observation in tenths of the Greenwich day
II = observatory indicator (see also lists in part C)
05 ‑ Huancayo 16= Kanzelhohe

18 = Wendelstein
26 = Norikura
30 = Arosa32 = Sacramento Peak
34 = Climax

36 = Pic du Midi
45 = Skalnate Pleso
87 = Kislovdsk
88 = Alma‑Ata

a = line observed (see key word COLOR
below)
1 = green (X 5303A)
3 ‑ red (A 6702A)
2 = red ( X6374A)
0 = yellow ( X5694A)
b = scattered light intensity (measure of observation
quality)
1 = weak ( < 30 millionths) or observation highquality
2 = moderate (30‑60 millionths) or observation
moderate quality
3 = strong (> 60 millionths) or observation low
qualityqqq = quadrants of limb for which values are given in
4 = NW(north‑west)
1 = NE (north‑east)
3 = SW (south‑west)
2 = SE (south‑east)‑ if all four quadrants insert 999‑, if fewer
than three quadrants, complete group with
O'slatitude (divided by 10) of intensity reported inddintensity measured at latitude indicated by c(millionths divided by ten)
intensity measured at next succeeding 5 posi‑tion angle ‑ proceeding N‑E‑S‑W‑(millionths divided by ten) (see Note 1)
more than one line reported, wordchange of line being reported

signifies

optional key word, CORonaPic‑du‑Mididescription of measurements
Note 2)of east limb(see

where "a" signifies that those portions of this quadrant nottransmitted in message have been observed but the intensi‑
ties are less than threshold, or were measured but are with‑out interest;"b" signifiesthose portions not sent have not been measured
but reason to believe they are without interest;"c" signifies those portions not sent have been measured
and their significance is unknown.
0 = the two quadrants have been completely measured andall values have been reported.
X = neither of the quadrants have been measured
W
HHH= description of measurements
described for "E" above)of west limb (same as= UT hour of observation in tenths of Greenwich day.
The sky brightness will be indicated by adding to
the UT hours, 0, 30 or 60 according to the bril‑

Always give observations in order of increasing
position angle, i.e. N‑E‑S‑W.
A group giving
intensities at equator and poles is usually neces‑sary to avoid ambiguity.
Usually enough measurements
will be given tooutline the intensity peaks and usually only for
East limb, green and yellow line.

B.I.5 SOLAR

X‑RAYS

Code 1. USOXA
1. C

o nt e nt .

Intensity of solar X‑ray radiation as measured
satellites

3. Definition
USOXA

of

by )

symbols.

= key word, SOlar

X‑ray events, code

A

JJ = Greenwich date of observation >r ^ *)3A
a ‑ satellite
1 = 1965‑16D Solar Radiation
II = observatory indicator g
25 = U.S. Naval Research Laboratory, Washing
ton, D. C.

33 = ESSA Boulderb = importance of level of daily average flux
1 = lower than previous pass
2 = same as previous pass
3 = higher than previous pass
4 = much higher than previous pass̲^> = saturated, usually plain language will follow
HHmm= UT hours and minutes of beginning of satellite
pass

HHmm

c = number of groups to follow= UT hours and minutes of end of satellitepas
d = band of flux measurement0 = 0 ‑ 3
Angstroms
if 1= 0 ‑ 8 Angstroms
2 = 8‑12
Angstroms
3 = 8‑20
Angstroms
if 4= 44 ‑ 60 Angstroms
e = qualifier to "ff"
0 = value on scale as given in "ff"
8 = less than value given in "ff"
9 = greater than value given in "ff"
ff = flux in ergs cm‑2 sec‑* xl0 §g = exponent of 10 in group "ff"
1 = 1
2 = 2
etc.

NOTESNOTES

B.II. Solar

Radio

Observations

II. 1 Flux
Code
Code
Code

measurements
1; UPANA
2; UPANP
3; URANF

on discrete frequencies

II. 2 Spectrographs
Observations
Code 1; URANT
Code 2; URANS
II. 3 Interferometric Observations
Code 1; URALA
Code 2: URALO

B. II.1 FLUXONMEASUREMENTSDISCRETEFREQUENCIES

Code 1. URANA
1. Content.
Frequency, period of observation, median
flux, type ofoutstanding occurrence, time of beginning, amplitude
and duration.

3. Definition
URANA

of

symbols.

= key word, RAdio

Noise, codeA

JJ = Greenwich date of observation
X = Nominal radio frequency of observation (precise
frequency depends upon observatory)
1 = less than 50 Mc/s 3 = 150 to 300 Mc/s
2 = 50 to 150 Mc/s 4= neighborhood of 500 Mc/s
II = observatory indicator (also see lists in
02 Cambridge
34 Seattle
79 Moscow
09 College
41 Maui
80 Irkutsk
11 Ondrejov
46 NERA84 Simferopol
12 Jodrell Bank
51 Mitaka
85 Simeis
20 Buenos Aires 56 Paramaribo
86 Voroshilov
24 Berlin H.Hertz 63 Kiel
87 Kislovodsk
26 Hiraiso
64 Humain
89 Abastumani
28 Nangay
66 Lwiro
92 Potsdam
33 ESSA Boulder 78 Perm. State U. 95 Krakow
aa = UT hour nearest beginning of period of obser‑
vations reported
bb = UT hour nearest ending of period of observations
reportedc = number of 5 digit groups following which refer
to observations between aabb
dd = median flux for whole period reported, in tenthsof quiet sun; if greater than 9. 9 then01 = 10 to 19 times quiet sun
02 = 20 to 29 times quiet sun

09 = 90 to 99 times quiet sun
00 = 100 times quiet sun
e = variation in median flux in interval reported
0 = less than 10 per cent change in median flux
level from hour to hour
1 = 10 to 25 per cent change
2 = 26 to 55 per cent change
3 = 56 to 100 per cent change
4 = over 100 per cent change
X = uncertainf = burst classification

0 = 0‑5 bursts per hour
1 = 5 to 100 bursts per hour
2 = 100 to 500 bursts per hour
3 = more than 500 per hour
4 = period of storm with several great bursts
g = burst amplitude
0 = no bursts
1 = 0 to 1/2 times median flux
2 = 1/2 to 1 times median flux
3 = 1 to 3 times median flux
4 = 3 to 5 times median flux
5 = 6 to 9 times median flux
6 = 10 to 19 times median flux
7 = 20 to 29 times median flux
8 = 30 to 39 times median flux
9 = > 39 times median flux
h = key to type of outstanding phenomenon
1 = rise in base level; temporary, less than
2 hours
2 = series of minor bursts
3 = group of minor bursts
4 = minor: characteristic isolated burst (fewseconds)
6 = noise storm in progress; jHHmm
will be en‑coded jXXXX
7 = onset of noise storm
8 = major
9 ‑ major plus *HHmm= UT of beginning of phenomenon
HHmm

j = burst amplitude as in "g"‑ UT end of phenomenon* For type 9 there will be four time groups ;begin andend for "first part" and begin and end for "plus part";
use XXXX
for end of "plus" if unknown
at time of
message.

B. II.1 FLUXONMEASUREMENTSDISCRETEFREQUENCIES

Code 2. URANP
1. Content.
Information on outstanding occurrences in solar radio
emission, type of occurrence, time of beginning, ampli‑
tude and duration.

3. Definition
URANP

of

symbols.

= key word, solar RAdio

Noise, code

P

JJ = Greenwich date of observation
X = Nominal radio frequency of observation (precise
frequency depends upon observatory)
1 = less than 50 Mc/s
2 = 50 to 150 Mc/s
3 = 150 to 300 Mc/s
4 = neighborhood of 500 Mc/s
II = observatory indicator (also see listsin part C)

34 Seattle
02 Cambridge
09 College
41 Maui
11 Ondrejov
46 NERA
12 Jodrell Bank
51 Mitaka
20 Buenos Aires 56 Paramaribo
24 Berlin H.Hertz 63 Kiel
26 Hiraiso
64 Humain
28 Nan^ay
66 Lwiro
33 ESSA Boulder 78 Penn. State U.

79 Moscow
80 Irkutsk
84 Simferopol
85 Simeis
86 Voroshilov
87 Kislovodsk
89 Abastumani
92 Potsdam
95 Krakow

UT hour nearest beginning of period of obser‑
vations reported
UT hour nearest ending of period of observations
reported
number of five‑digit groups following which refer
to observations between aabb
key to type of outstanding phenomenon
9 = major plus burst (see Note 1)
8 = major burst
7 = onset of noise storm
6 ‑ noise storm in progress; jHHmm
will beencoded jXXXX
4 = minor: characteristic isolated burst (fewseconds)
3 = group of minor bursts
2 = series of minor bursts
1 = rise in base level; temporary, less than 2
hours
UT of beginning of phenomenon
burst amplitude
1 =0‑1/2 times median flux
2 = 1/2 ‑ 1 times median flux
3 = 1‑3times median flux
4 = 3‑5times median flux
5 = 6‑9times median flux
6 = 10‑19
times median flux
7 = 20 ‑ 29 times median flux
8 = 30 ‑ 39 times median flux
9 ‑‑ >39
times median flux

UTof ending of phenomenon

For type 9 there will be four time groups jbe
ginning and end for "first part" and beginningand end for "plus part"; use XXXX
for end of"plus part" if unknown at time of message.

NOTES

B.II.l FLUXONMEASUREMENTSDISCRETEFREQUENCIES

Code 3. URANE
1. Content
Daily flux level and outstandingphenomena.

3. Definition
URANE

of

symbols.

= key word, solar RAdio

Noise, code

E

JJ = Greenwich date of observation
X = Nominal radio frequency of observation
4 = neighborhood of 500 Mc/s
5 = neighborhood of 1,500 Mc/s
6 = neighborhood of 3,000 Mc/s
7 = neighborhood of 10,000 Mc/s
II = observatory indicator (see also listsin part

03 Sydney

46 NERA24 Berlin H. Hertz 57 Ottawa ‑35 Toyokawa
Algonquin

58 Penticton
78 Penn. Stataa = UT hour nearest beginning of period of obser‑
vations reported
bb = UT hour nearest ending of period of observations
reportedc = number of 5 digit groups following which refer
to observations between aabb
ddd = flux level at hour given in eeunits: 10 22 W m‑2(c/s)""^ee = nearest hour UT of flux level measurement

HHmm

f = key to burst phenomenon(based on Covington,
Astron. Soc. Canada. 45. 1951)
0 = doubtful
5 = post‑burst decrease
6 = complex
1 = simple 1
7 = fluctuations
2 = simple 2
3 = simple 3
8 = group
4 ‑ post‑burst increase 9 = precursor= hours and minutes UT of beginning of phenomenon

HHmm

g = key to intensity class
1 = 0 ‑ 7.5 flux units
2 = 7.5‑75
3 = 75 ‑ 750
4 = 750 ‑ 7500
5 = 7500= hours and minutes UT of end of phenomenon

Notes: 1. Designation of simple bursts based uponregion of"intensity" versus "duration" diagram
Region 1 ‑ Intensity 7.5
flux units‑
Duration ^ 7.5 minutes
Region 2 ‑ Intensity > 7.5 flux units
Region 3 ‑ Duration > 7.5 minutes
Simple 1 ‑ Burst in Region 1 ‑ may be impulsive
Simple 2 ‑ Burst in Region 2 ‑ Impulsive burst

Simple 3 ‑ Burst in Region 2 ‑ long enduring
gradual rise and fall burst
Commencement
time of bursts.
‑ taken when enhancement
departs from dailylevel by receiver noise ( ≫ 1 flux unit)‑ for impulsive bursts, this may be determined
generally within a time interval of one min‑ute.
Great bursts ‑ these are very intense bursts whici
are generally very complex‑ the fluctuations are comparable to averagebursts ‑ their intensity is greater than 1000
flux units.

B. II.2 SPECTROGRAPHSOBSERVATIONS

Code 1. URANT
1. Content.
Outstanding phenomena,
type, time of beginning andend, relative intensity, frequency range showing the ac‑tivity;decametric frequency range.

3. Definitions
URANT

of

symbols.

= key word, solar RAdio

Noise, code

T

JJ = Greenwich date of observationa = number of phenomena
reported
II = observatory indicator (also see lists in part C)
33 = HAO
Boulderb = type of spectral activity
2 = slow‑drift burst
3 = fast‑driftburst
4 = broadband continuum
5 = continuum associated with fast‑driftburst

HHmm

HHmm

= UT

hour and minutes of beginning of activity

c = relative intensity on scale of 1, 2, 3,: except
that
7 = importance 1 +8 = importance 2 +9 = importance 3 += UT hour and minutes of end of activity
dd = lowest frequency of activity in Mc/s
ee = highest frequency of activity in Mc/s
f = units digit of sum of preceding 14 digits.

NOTES

B. II.2 SPECTROGRAPHICOBSERVATIONS

Code 2. URANS
1. Content.
Outstanding occurrences, type of spectral activity, im‑portance, time of beginning, polarization, time of end‑
ing, position and type of position measurement.

3. Definition
URANS

of

symbols= key word, solar RAdio
JJ = Greenwich

Noise, codeS

date of observationb = key to spectral type of activity
1 = type I storm
2 = type II (slow‑drift) burst
3 = group of type III (fast‑drift)bursts
4 = storm of type III (fast‑drift)bursts
5 = compound
burst: group of type III (fast‑drift)
bursts followed by a type II (slow‑drift) burst
6 = unclassified activity

7 = type IV (broadband continuum) burst
8 =9 ‑II = observatory indicator (also see lists in
40 Culgoora
31 Big Pine
32 Ft. Davis
62 Freiburg
33 HAO
Boulder
importance (see Note)
2 = large
3 =. very large
9 = exceptional
hours and minutes UT of beginning of activity‑ if mm= 99 signifiesactivity in progress when
firstobserved (at HHoo + 30 mins. )‑ if mm= 88 signifiesstarting time known tonearest hour only
sense and degree of polarization
0 = no polarization
1 = less than 50 per cent left‑handed polarization
2 = less than 50 per cent right‑hand polarization
3 = more than 50 per cent left‑hand polarization
4 = more than 50 per cent right‑hand polarization
9 = polarization not measured
hours and minutes UT of end of activity‑ if mm= 77 signifies continuing when lastob‑
served (at HHoo + 30 min. )‑ if mm= 66 signifiesstarting time known tonearest hour only
heliographic position angle measured eastwards
from the north of the projected solar axis in ten‑degree steps.
00 = heliographic position angle in range 0 +5 degrees
01 = heliographic position angle in range 10 +5 degrees
02 = heliographic position angle in range 20 +5 degrees35 = heliographic position angle in range 350+ 5 degrees
type of position measurement
1 = strip‑scanning position in which case theposition given is that of the point along themid‑line of the source‑strip which is closest
to the center of the disk
2 = spot‑scanning position, in which case thecenter of the source spot is given
radial distance from the center of the disk in*tenths of the photospheric radius R
00 = radial distance in range 0.0 + 0.05 RQ(i.e. center of disk)
01 = radial distance in range 0.1+
0.05 RQ
02 = radial distance in range 0.2 + 0.05 RQ

10 = radial distance in range 1.00
(i.e. optical limb)
11 = radial distance in range 1.10

+ 0.05RQ+ 0.05

RQ

Importance should be assessed on the basis ofintensity, duration and rarity. As a guide:"Large", "Very Large" and "Exceptional" shouldroughly correspond in frequency of occurrencewith flares of importance 2, 3 and 3+.

B. II.3 INTERFEROMETRICOBSERVATIONS

Code 1. URALA
1. Content.
Position, maximum
noise source.

3. Definition
URALA

of

intensity and flux of solar radio

symbols.

= key word, solar RAdio

noise Location, code A

JJ = Greenwich date of observation
T = time of observation in tenths of the Greenwich
day
II = observatory indicator (also see listsin part C)
03 Sydney 28
Nan §ay 31
Stanford
Q = quadrant (heliographic co‑ordinates) containing

XX =
YY =

1 = NE (north‑east)
4 = NW (north‑west)
2 = SE (south‑east)
3 = SW (south‑west)
distance to the central meridian, in degrees
heliographic latitude, in degrees

aaa = max. intensityin tens of thousands of degrees Kelvinbb = flux of region in 10"22 w/m^/cvcle/second

B. II.3 INTERFERON!

ETRICOBSERVATIONS

Code 2. URALO
1. Content.
Importance3. Definition
URALO

and location of solar radio noise sourcesofsymbols.

= key word, solar RAdio

noise Location, code

O

JJ = Greenwich date of observation
X = nominal radio frequency of observation (precise
frequency depends upon observatory
1 = 50 Mc/s
2 = 50 ‑ 150 Mc/s
3 = 150 ‑ 300 Mc/s
4 = neighborhood of 500 Mc/ s
5 = neighborhood of 1,500 Mc/ s
6 = neighborhood of 3,000 Mc/s
7 = neighborhood of 10,000 Mc/s
8 = neighborhood of 35,000 Mc/s
II = observatory indicator (see also lists in part C)
31 = Stanford
03 = Sydney
46 ‑ NERA
28 = Nan^ay
importance on scale 0, 1, 2, 3 where 3 has thegreatest importanceangular location with respect to North‑South dia‑meter at meridian transit

1 = North, east
5 = Central, east
2 = South, east
6 = Central, west
3 = South, west
7 ‑ ‑ ‑ ‑ , east
4 ‑ North, west
8 = ‑ ‑ ‑ , west
distance to NS diameter at meridian transit,
percent of the solar optical radius (e.g. 075
75%, 125 = 125% of the radius).

NOTES

NOTESNOTES

B.III. Ionospheric

Observations

III. 1 Critical frequencies
Code 1; UFOFA
Code 2; UFOFE
III. 2 Sudden
Ionospheric Disturbances
Code 1; USIDA
Code 2 jUDISE
III. 3 Cosmic
Noise Absorption
Code 1; UABSB
III.4 Combined
Event
Code 1; UEVTA

B. III.1

CRITICALFREQUENCIES

Code 1. UFOFA
Code 2. UFOFE
1. Content.
Critical frequencies of F2 region (foF2) as a function ofStandard Meridian time (if code UFOFA)
or Universal
time (if code UFOFE)
maximum
and minimum
values of foF2 and hour of oc‑
currencef‑min frequencies as a function of same times as given
for foF2

3. Definition
UFOFA
UFOFE

of

symbols.

= key word, foF2, code
= key word, foF2, codeA (Standard Meridian time)
E (Universal time)

JJ = local date of beginning of 24‑hour period report‑
ed if UFOFA or Greenwich date of beginning of
24‑hour period reported if UFOFE
T = time indicator for approximate time of beginningof 24‑hour period
0 = 0000
4 = 1200
1 = 0300
5 = 1500
2 ‑ 0600
6 = 1800
3 = 0900
7 = 2100
II = observatory indicator (also see lists in part C)
05 = Huancayo
07 = Kodaikanal
08 = St. John's
09 = College
13 = Gorki
17 = Uppsala
19 = Lycksele
20 = Tucuman
21 = Tortosa
22 = Lulea
25 = Ft. Belvoir
26 = Taipei
27 = Okinawa
29 = Tamanrasset

30 = Kiruna
32 = White Sands

73 = Breisach
74 = Rabat
33 = ESSA Boulder 75 = Bangui
34 = Barrow
76 = Kerguelen
41 = Maui
77 = Poitiers
42 = Thule78 = Anchorage46 = Leidschendam 79 = Moscow
51 = Kokubunji
80 = Irkutsk
82 = Terre Adelie
56 = Paramaribo
57 = Ottawa
84 = Simferopol
88 = Alma‑Ata
59 = Quezon City
66 = Lwiro
93 = Juhlesruh
94 = Cape Town
69 = Pruhonice
71 = Lindau
97 = Budapest

f = even hour indicator, give data for 0000, 0600,
1200 and 1800, beginning with the appropriate
hour aftpr thp Hatp
0 = 0000 hours
6 = 1200
3 ‑ 0600
9 ‑ 1800
ggg = value of foF2 (in tenths of Mc/s; report as 000
if symbols only are applicable)
h = descriptive letter symbol (see Piggott and Rawer,
URSI Handbookof Ionogram interpretation andreduction, 1961, for fullinformation)

X = none (use slant bar 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 = 1, interpolated value
9 = T, smoothed value
0 = any other
MAXMI= key word, indicating that following groups give
MAXimumand Minimum
foF2 during 24‑hour
period reported

HH = nearest hour of maximum
value
ppp = maximum
value of foF2 in 24 hour period report‑
ed, in tenths of Mc/s
HH = nearest hour of minimum
value
qqq = minimum
value of foF2 in 24‑hour period reported,in tenths of Mc/s
EFMIN

= f‑MINdata to follow

ii = f‑min in tenths of Mc/s
group above
jj = f‑min in tenths of Mc/s
group above

for time of first"fgggh"
for time of second "fgggh"

kk = f ‑min in tenths of Mc/s for time of third "fgggh"group above
11 = f‑min in tenths of Mc/s for time of fourth "fgggh"group above

Notes: 1. In "iijjk kllxx" groups "99" will signify f‑min
9.9 Mc/s^

2. If symbol to be used for f‑min, encodelows:
XI ‑ A
X2 ‑ B

as fol‑X3 = C
X5 : E(The X!s should be slant bars in teletype mes‑
sages )
always "XX"(or slant bars in teletype messages).

NOTES

B. III.2
SUDDENIONOSPHERICDISTURBANCES

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

3. Definition
USIDA

of

symbols= key word, Sudden.
Ionospheric Disturbance

JJ = Greenwich date of observation
X = number of phenomena
reported
II = observatory indicator (see also lists in part
19 = Stockholm
20 = Tucuman
22 = Enktfping
24 = Berlin H.Hertz
25 = Ft. Belvoir
07 = Kodaikanal
08 = McMath
26 = Hiraiso
09 = College
27 = Okinawa
10 = Bagneux
29 = Tamanrasset
15 = Ktihlungsborn 31 = Troy
18 = Weissenau
31 ‑ Ft. Monmouth
02 = New Delhi
03 = Sydney
04 = Trinidad
05 = Huancayo

32 = White Sands
33 = HAO Boulder(SCNA‑SEA)
33 = ESSA Boulder(SWF‑SPA‑SFD)
37 = Dunsink
41 = Maui
46 ‑ NERA
52 = Canberra
56 = Paramaribo

69 = Pruhonice
71 = Lindau
72 = Darmstadt
73 = Breisach

75 = Bangui
76 = Kerguelen
77 = Poitiers
78 = Anchorage

79 = Moscow
82 = Terre Ad ￡lie
93 = Juhlesruh

type ol phenomenon
0 = sudden frequency deviation
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 irregularin both dropout and recovery)
4 = SEA (sudden enhancementof atmospherics)
5 = SPA, positive (sudden phase anomaly)
6 = SCNA(sudden cosmic noise absorption)
7 = SES (sudden enhancementof signal at about
15 kc/s)
8 = SPA, negative (sudden phase anomaly)
9 = solar radio noise storm at 18Mc/s (could bereported by URANA
code)
hours and minutes (UT) of beginning of phenomenonof
7 = importance 1 +0 = importance 1 ‑1 = importance 1
8 = importance 2+
2 ‑ importance 2
9 = importance 3 +3 = importance 3
cc = duration of phenomenon
in minutes‑ if 99: duration equal to or greater than 99
minutesd = reliabilityof time
5 = beginning of phenomenon
itself is not clear
6 ‑ nominal time
7 = firstobservation
8 = beginning time less certain than 2 min.
9 = beginning time accurate to nearest 2 min.
or lesse = definiteness of phenomenonon recording
0 = questionable
3 = reasonable
1 = possible
4 = reasonably definite
2 = fair
5 = definite

B. III.2 IONOSPHERICDISTURBANCES

Code 2. UDISE
1. Content.
Type and strength of ionospheric disturbance on a radio
propagation circuit, frequency range affected, time andduration.

3. Definition
UDISE

of

symbols.

= key word, ionospheric Disturbance.

JJ = Greenwich date of observation
X = always a "0"
II = observatory indicator (see also lists in part C)
03 Sydney
22 EnkOping
25 Ft. Belvoir
26 Hiraiso

46 NERA78
79 Anchorage
Moscowtype of disturbance reported
8 = abnormal absorption
9 = ionospheric storm
0 = disturbance cause undetermined
strength of disturbance and circuits involved
1 = weak disturbance affecting some circuits

2 = weak disturbance affecting all circuits
3 = moderate disturbance affecting some circuits
4 = moderate disturbance affecting all circuits
5 = strong disturbance affecting some circuits
6 = strong disturbance affecting all circuits
nominal frequency range most affected
0 = traffic frequency < 1 Mc/s
1 = traffic frequency between 1‑2 Mc/s
2 = traffic frequency between 2‑4 Mc/s
3 = traffic frequency between 4‑8 Mc/s
4 = traffic frequency between 8‑16 Mc/s
5 = traffic frequency 16
Mc/s
UT hour of beginning combined with duration
00 to 23 = duration of 3 hours
30 to 53 = duration of 6 hours (hour +30)
60 to 85 = duration of 9 or more hours (hour +
60)

NOTES

B. III.3 COSMIC
Code

NOISE

ABSORPTION

1. UABSB

1. Content.
Ionospheric absorption measurement
by riometer tech‑nique (SCNA, aurora or cosmic ray associated phenomena).

3. Definition
UABSB

of

symbols.

= key word, ionospheric ABSorption

JJ = Greenwich date of observation
X = number of phenomena
reported
II = observatory indicator (see also listsin part C)

08 Resolute Bay 31 Mc Murdo
09 College
32 South Pole
19 Spitzbergen 33 Byrd
30 Kiruna
41 Maui

42 Thule46
Roi Baudouin
57 Churchill
58 Great Whale
78 Anchoragea = type of phenomenon
1 = SCNA (sudden cosmic noise absorption ‑ solar
flare associated)
2 = Aurora ‑ associated absorption .
3 = PCA (polar cap absorption event
6 = noise storm of solar radio emission superposedon absorption

HHmm= hours and minutes UT・ nonof beginning of phenome‑

bb = number of decibels of maximum
absorption be‑fore hour indicated by next HH
X = always an X (or slant line in teletype message)
HH = UT hour when the phenomenon
reported (if also
the ending time of the event, increase the hourby 30)NOTES

B. III.4
COMBINED
Code

SOLAR‑GEOPHYSICAL

EVENT

1. UEVTA

1. Content
Solar flare and solar radio noise events together with asso‑
ciated terrestrialeffects such as sudden ionospheric dis‑turbances, cosmic noise absorption, and cosmic ray events.

3. Definition
UEVTA

of

symbols= key word, combined

event, code

JJ = Greenwich date of observation
X = number of phenomena
in combined
reportedA

event being

II = indicator of RWC
or observatory preparing com‑bined report. Note observations may have comefrom several different observatories (see list C).
02 = New Delhi
03 = Sydney
10 = Meudon
25 = Ft.Belvoir

33 = ESSA Boulder 72 = Darmstadt
46 = NERA
79 ‑ Moscow
51 = Kokubunji
80 = Irkutsk
69 = Pruhonice

Q = quadrant (heliographic coordinates) in which theflare or solar radio noise burst is observed
4 = NW (north‑west)
1 = NE (north‑east)
2 = SE (south‑east)
3 = SW (south‑west)
XX = distance to central meridian in degrees
YY = heliographic latitude in degrees (QXXYY
given asslant bars if position unknown)a = type of event used for beginning time in HHmm
following
1 = solar flare
2 = solar radio noise position
3 = sudden ionospheric disturbance
4 = ionospheric absorption measurement
5 = cosmic ray event
HHmm= time in hours and minutes (UT) of beginning ofevent
b = importance of solar flare 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
importance of solar flare based upon relative in‑tensity evaluation
7 = faint
8 = normal
9 = brilliant
duration or period of observation of flare in min
utesj if no good estimation use 000
solar x‑ray event reported by satellite
1 ‑ small 2= moderate 3= largesolar radio noise event at neighborhood of 3,000
1 = simple 1
6 = complex
2 = simple 2
7 = fluctuations
3 = simple 3
8 = group
4 = post‑burst increase
9 = precursor
5 = post‑burst decreaseg = intensity of event described in "f"
1 = 0‑7.5
flux units
2 = 7.5 ‑ 75
3 = 75 ‑ 750
4 = 750 ‑ 7500
5 = 4>V500
h = solar radio noise event in neighborhood of 100 ‑300 Mc/s
1 = rise in base level, temporary, less than 2hours
2 = series of bursts
3 = group of minor bursts
4 = minor: characteristic isolated burst (fewseconds)
6 = noise storm in progress
7 = onset of noise storm
8 = major
9 = major plus
i = burst amplitude of event described in "h"1 = 0 to 1/2 times median flux
2 = 1/2 to 1 times median flux
3 = 1 to 3 times median flux
4 = 3 to 5 times median flux

5 = 6 to 9 times median flux
6 = 10 to 19 times median flux
7 = 20 to 29 times median flux
8 = 30 to 59 times median flux
9 = > 39 times median flux
j = type of spectral activity of solar radio noise
2 = slow‑drift burst (type II)
3 = fast‑driftburst (type III)
4 = broad band continuum (type IV)
5 = continuum associated with fast‑driftburst*
storms (type V)
k = frequency range of spectral solar noise burst
1 ‑ 7 to 41 Mc/s (HAO)
2 = 25 to 320 Mc/s (Ft. Davis)
3 = 10 to 25 Mc/s (Culgoora)
1 = type of sudden ionospheric disturbance0 = SFD, sudden frequency deviation
1 = typical S‑SWF, short wave fadeout, sudden
dropout
2 = slow S‑SWF, short wave fadeout, dropout
taking 5 to 15 minutes and gradual recovery
3 = G‑SWF,
short wave fadeout, fade irregularin dropout and recovery
4 = SEA, sudden enhancementof atmospherics
5 = SPA, positive sudden phase anomaly
6 = SCNA, sudden cosmic noise absorption
7 = SES, sudden enhancementof signal at about
15 kc/s
8 = SPA, negative sudden phase anomaly
9 = solar radio noise storm at 18 Mc/sm = importance of phenomenon
0 = importance 1 ‑1 ‑ importance 1
7 = importance 1 +2 = importance 2
8 = importance 2+
3 = importance 3
9 = importance 3+
n = type of ionospheric absorption (usually identified
on riometer)
2 = aurora‑associated absorption
3 = polar cap absorption event (PCA)

oo = number of decibels of maximum
absorption
p = type of cosmic ray event (usually from neutron
monitor)
7 = solar x‑ray increase
8 = proton increase
9 = auroral x‑rays
q = intensity of beginning of event
1 = smaller than 10% of normal, or backgroundlevel
2 = between 10 and 50% of normal, or backgroundlevel
3 = between 50 and 100% of normal, or back‑ground level
4 = between 100 and 500% of normal, or back‑ground level
5 = between 500 and 1000% of normal, or back‑ground level
6 = between 1000 and 5000% of normal, or back‑ground level
7 = between 5000 and 10000% of normal, or back‑ground level
8 = between 10000 and 50000% of normal, or back‑ground level
9 = larger than 50000%
r = check, unit digit of sum of preceding 34 digits.

Note: 1. Insert slant bars for missing or unknown data.
Observatories reporting each type of event will
not be designated nor will the times of all typesof events be designated.
2. For 114" if several types of SID reportable, use
following priority order: SPA, SES, SCNA, SWF,
SEA, SFD.

A new provisional ccde PSTPA is given below.
It is strongly recommended for interchange
messages in order to reduce the number ofindividual codes needed to report the same
information. If PSTPA is used, detailed codesneed to be sent only at descretion of the RWCor ARVC.
1. Content
the general solar and geophysical activityof the day up to time of message: sunspots,
solar flux, geomagnetic activity, cosmic
ray level, x‑ray level and flare activity.
General form

key vord
PSTPA = key word provisional Solar‑Terrestrial
Physics?code A
1 ― key number for suns potsaaa
sunspot numberbnumber of births of sunspots or E limb
appearances2
key number for solar flux
ccc = ■10 cr> fluxu ‑ number of large events
3 = key number for geomagnetic
activityeee = Ak of the station of reference
for center reporting
f ;= event in order of priority
8 ‑ very marked storm so
7 ‑ storm sudden commencement
6 = gradual storm beginning
1 = storm end
0 = nothing unusual‑ key number for cosmic ray level
ggg = percentage of the mean level for
event given in flh"h = event in order of priority
5 = solar cosmic ray event￡ announcementof a Forbush
Decrease
3 = Forbush Decreaseh = end of a Forbush Decrease1 zz pre‑decrease
0 = normal daily variation
5 ‑ key number for solar x‑ray leveliii = mean level on a standard band
(each center should indicate
with first message band chosen)
i = event in order of priority
9 ‑ outstanding event
8 = inarnrsmall events
7 = one small event
6 = important increase suspectedwithout flare
5
important decrease suspected
and not part of flare event
0 ‑ nothing unususalknumber of flares of importance
1 = .number of flares of importancem = number of flares of importancen = number of flares of importanceo = number of flares of importance

4 reported
3 reported
2 reported
1 reported
S reported

For more than 9 flares of the same
importance the number is always 9‑
If data of any of the above types are notreported by a center, the group may beomitted or slant lines used following the
key number.

NOTES

B.IV. GeomagneticandAuroralactivity

IV. 1 Geomagnetic
activity indices and events
Code 1; UMAGA
IV. 2 Auroral Observations
Code 1; UAURA

B. IV. 1
GEOMAGNETICAND

ACTIVITYSPECIAL
EVENTS

INDICES

Code 1. UMAGA
1. Content.
Geomagnetic
Geomagnetic
Geomagnetic

3. Definition
UMAGA

A^ index
K‑indices for the period reported
disturbances with time of occurrenceofsymbols.

= key word; MAGnetic

activity,code A

JJ = Greenwich date of beginning of 24‑hour period
reported
T = time indicator for UT hour of beginning of 24‑
hour period
0 = 00
1‑03
2 = 06

3 = 094 = 12
5 = 15

6 ― 18
7 = 21II = observatory indicator (see also lists in part C)

03 = Sydney
04 = Abinger
05 = Huancayo
07 = Kodaikanal
09 = College
14 = Sodankyla
16 = Nurmijaryi
21 = Tortosa
24 = Wingst
25 = Ft. Belvoir
26 = Kakioka

28 = Chambon‑la‑Foret
29 = Tamanrasset
31 = Fredericksburg
32 = Sitka
33 = ESSA Boulder
34 = Barrow
38 = Helwan
40 = Gnangara
42 = Thule
46 = Witteveen

52 ‑ Canberra
57 = Ottawa
67 = Dourbes
69 = Pruhonice
74 = Rabat
75 = Bangui
77 = Garchy
78 = Anchorage
79 = Moscow
82 = Terre Adelie
85 = Simeis

aa = A^‑index for Greenwich date JJ (hundreds digit
omitted). (Note this is not the 24‑hour period
reported, unless T is 0. If notavailable atobservatory, put XX or slant bar in teletypemessage)kkkkkkkk = K indices for the 24‑hour period reported

HHmm

P = indicator telling the time reported in HHmm
is
1 = storm end
6 = gradual storm beginning
2 = bay (psc)
7 = storm sudden com‑
3 = typical crochet
mencement(sc)
4 = provisional figures 8 = very marked storm sc= UT hour and minute of phenomenon
indicatedby P. (if P = 4, HHmm
used for reporting up to
four additional 3‑hour periods following the 24‑hour interval reported by the "k's").

B.IV.2 AURORALi
Code B. UAURAOBSERVATIONS

1. Content.
Occurrence, principal forms, activity, brightness andcolour of aurorae as functions of time and place of ob‑
servations.
Quality of observations and cloudiness.

3. Definition
UAURA

of

symbols.

= key word, AURoral

observations, code

A

JJ = Greenwich date of message
a = type of message
1 ‑ warning
2 = survey
II = observatory indicator (also see lists in part09 = College
31 = Ithaca
17 = Uppsala
33 = Byrd
19 = Lycksele
45 = Lomnicki Stitt
22 = EnkGping
30 = Kiruna

57 = Saskatoon
71 = Lindau

bb = Greenwich date of observations
HH = UT hour of warning or of beginning of obser‑
vationsd = tens of minutes after HH for warning or numberof five digit groups "efghi" to follow if survey
messagee = type of aurora during the firsthour0 = no observation
1 = no aurora
2 = veil
3 = pulsating patches
4 = homogeneous
bands in the north
5 = 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 colour of aurora during the firsthour
0 = no observation
1 = colour uncertain (because of other lights,
moonlight, dawn, etc. )2 = faint yellowish green
3 = moderate " "4 = bright " "5 = faint yellowish green with red
6 = moderate " """7 = bright """"8 = faint red only
9 = bright " "g = quality of observations and cloudiness during thetwo hours covered by ef and hi
0 = cloudy
1 = occasional observation and semi‑cloudy
2 = " " andalmost clear
3 = " " andclear
4 = periodical observation and semi‑cloudy
5 = " " andalmost clear

6 = periodical observation and clear
7 = continuous observation and semi‑cloudy
8 = " " andalmost clear
9 = 11 " andclear
h = type of aurora as in "e" above, during the sec‑
ond hour or "0" if warningi = brightness and colour of aurora as in "f" above
during the second hour or "0" if warning
BB = UT date of end of observations
CC = UT hour at ending of the 60 minutes
referred toby hi in the last "efghi" groupk = always a "9"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. If all "efghi"‑groups are alike it is enough tocode one of them flanked in by bbHHl and
BBCC9.
3. The observer should be able to judge which in‑formation is most important for each one hour

B.V. Cosmic

Ray

Messages

Cosmic ray events
Code 1; UCOSA
Code 2; UCOSCNOTES

B.V.I COSMIC

RAY

DATA

Code 1. UCOSA
1. Content.
Outstanding occurrences, times

3. Definition
UCOSA

of

and percentage variation

symbols.

= key word, COSmic

ray data, code

A

JJ = Greenwich date of observationa = type of apparatus
0 = neutron monitor (IGY‑type)
1 = high counting rate neutron monitor(IQSY‑type)
2 = meson monitor (IGY‑type)
3 = meson monitor (IQSY‑type)
4 = telescope, no shielding
5 = telescope, shielded
6 ‑ inclined telescope, directed N
7 = inclined telescope, directed S
8 = inclined telescope, directed E
9 = inclined telescope, directed W

II = observatory indicator (also see listsin part C)
20 = Buenos Aires
26 = Norikura
30 = Kiruna
34 = Climax
36 = Pic‑du‑Midi
45 = Lomnicki
51 = TokyoStitt

57 = Deep
63 = KielRiver

65 = Predigstuhl
71 = Lindau
72 = Kranzbach
81 = Tiksi Bayb = type of outstanding event
0 = slow decrease
1 = sudden decrease
2 = after effect of decrease
3 =4 = slow increase
5 = sudden increase
6 = after effect of increase
7 = daily variation of large amplitude
8 = daily variation of anomalous phase
HHmm= hour and minutes UT of beginning of event
ccc = maximum
deviation from pre‑event level inunits of 0.1%
dd = rise time of event (or decline) in minutes
HHmm

X = always an "X"(or slant bar in teletype= hour and minutes UT of end of event

B.V.I COSMIC
Code

2. UCOSC

RAY

DATA

1)

1. Content.
Special events, detected by particle and radiation de‑tectors carried bv stratosphericballoons

3. Definition
UCOSC

of

symbols.

= key word, COSmic

Ray balloon observations

JJ = Greenwich date of observation
M = type of detector flown
1 = Standard SPARMO
detector
1)
This code is especially used by the European Solar Par‑
ticles and Radiation Monitoring Organization (SPARMO).

2 = Standard SPARMO
detector with ionizationchamber
3 = Scintillation counter
4 = Cerenkov counter
5 = Special detector
II = Observatory indicator (see also listsin part C)
01 =
10 =
12 =
22 =
29 =

Bologna
MeudonLondonAndenes
Locarno

30 =
71 =
75 =
94 =

KirunaLindauAir sur Adour
Dakar

type of alert
0 = routine flight
1 = important activity center with intense 3 cm
emission on the disk
2 = optical flare
3 = type IV radioburst
4 = type III ionospheric absorption (PCA)
5 = type II ionospheric absorption
6 = magnetic storm
7 = cosmic ray storm
time of launching, UT
if launching took place on JJ―1:add 30 to HH
if launching took place JJ‑2: add 60 to HH
type of event
7 = solar ray increase
8 = proton increase
9 = auroral x‑raystime of beginning of event, UT
intensity of beginning of event
1 = smaller than 10% of normal, or backgroundlevel
2 = between 10 and 50% of normal, or back‑ground level
3 = between 50 and 100% of normal, or back‑ground level
4 = between 100 and 500% of normal, or back‑ground level5 = between 500 and 1,000% of normal, orbackground level
6 = between 1,000 and 5,000% of normal, orbackground level
7 = between 5,000 and 10,000% of normal, orbackground level
8 = between 10,000 and 50,000% of normal, orbackground level
9 = larger than 50,000%
time of maximum
intensity, UT
duration of the event in tenths of an hourinterval of reception of telemetry signals in hours.

When more than one event, observed during theflight, must be reported, the three groups THHmm,
IHHmm
and DDDdd
will be reported with dd re‑placed by xx in each case except the last one,when it has its original meaning.

117

In section B,V Cosmic Ray Messages, insert
the following new code UGOSB on the blankpages lxc‑119, This new code UCOSB (replacing
code TiTOSC) not
the form of UCOSB publishedin the J963 edition of the IUWDS Code Booklet
and in SPArj'O Bulletin No, i, January 1965.
The nc" fern below ixasadopted by SPARMO.
eiferci vroMay 1, 1966, for transmitting
balloon flight results.
Syiib.'"1l1fcr&s
Key Words UCOSB
1st group; "UCC8T3 JJIII AHHisimTKHrem
iBKir̲mEDDdd'

JJ = Day count of the month
M =Monitor:
1 = SPARMO Standard detector with
1 GM counter
2 = SPARMO Standard detector with
2 GM counters + 1 telescope
3 = SPARMO Standard detector with
3 QM counters + 2 telescopesb = SPARKO sf ntillator detector
5 = other kinas of detectors

II = Station indicator
14 = Sodankyla
20 = Buenos Aires
30 = Kir‑ana'
43 = Reykjavik^‑6 = Roi Baudoin
53 = Utrecht
71 ―i‑jinctS‑U.
7'+ = Potcbef stroom
75 = Aire/ildour
76 = Fort aux Francais
94 = Dakar

A =Type of alert
1 = protonalert
2 = MAGALP1ET
3 = ftECTTRALERT ,4 = AURORATKRT (Local Auroral
Alert)
5 = ROUTINE

HHram = Launching time UT (Hr. + min.)^̲rd groiros
T― Tvpf? nf eire!+.

7 = so?Lar x‑reys= protcn events
9 ‑ aur‑ci‑alx‑rays
HHmm = Ber‑i ":ning time of event UT (Hr.
+ rein,)・4th p^oupsi￨ 0Intensity at maximum of event measured
on the most sensitive channel‑ 0,1 to 1 the(1<$ to 100^)

normal level

1=1

to 10 thenormal level(100$ to 1,000$)
2 = 10 to 130 bjr.es the normal level(1,000$ to 10, 000)
3 = 100 to 1,000 tidies the normal level(10,, 000^ to 1005000l)
4 = greater than 1,000 times (>.100,000
HEtoi = Time of maximum intensity DT (Hr.
+ min.)
5th group;
DDD. = Duration of event in tenths of an hourdd =Duration of reception in hours

NOTES;
1. If no event or phenomenon occurs9 write thecorresponding groups with XXXXX (or slant
lines on teletype).
2. If
several even Lb occur during a flight?
groups THHimiu :iFrri;ui?
DBDdd mil be rer^ied
as often as events b'lt, in this cr^e? 5*'ddv?
mil be written by XX, ?*ddl ＼ y&ll be written
in hours after the last at
the end ofrecent*e ≪≪3. The amplitude of event will always be cal‑culated on the most sensitive channel.

)

B.VI. Alert

Messages

VI. 1 Advice
from Regional Warning
Code 1; ADV‑‑
VI. 2 Alert messages for IUWDS
Code 1; ADALERT
Code 2: GEOALERTCentersB, VI. 1
ADVICEFROMREGIONAL
CENTERSWARNING

Code 1. ADV‑‑
1. Content.
Notification of Geophysical Alerts or Suggested
tervals
Type and importance3. DefinitionofRetroin‑symbols.

ADV = ADViceaa = Regional Warning Center
BE = Belvoir (AGIWARN)
BO = Boulder
DA= Darmstadt
IR = Irkutsk
KO= Kokubunji
MO= Moscow

giving advice
ND = New Delhi
NE = Nederhorstdenberg
PA = Paris
PU = Prague
ST = Stockholm
SY = Svdnev

bbbbb = code word as defined below
ALADA= advise issue GEOALERTof same typeas the ADALERT
issued today in thisregion
ALNIL = advise no GEOALERTALBEG = advise begin GEOALERTof type men‑tioned in next group of message
ALCON= advise continue GEOALERTof type inprogress
ALFIN = advise finish GEOALERTof type inprogress
REPRE = we predict MAG
STORM for the future
period given by "eeff/"
RETRO= dates given in "eeff/ (month)" groups
suggested as possible RETROINTERVALNOLOX= insufficientinformation available formaking any advice(type) = added word with ALBEG or RETRO
and signifies
type of GEOALERT
advised(MAGSTORM,MAGCALME,
SOLACTIVITYOR
COSMICEVENT)
ortype of RETROINTERVAL
advised (IONOMAG‑STORM,
INTERPLANET,QUIETSUN,MICRO‑PULSATION
or RIOMETER)(ddddd) = strength of opinion, when desired
FORTE= strong
PIANO = weak
(ee = date of start of period for REPRE or RETRO
ff = date of finish of period for REPRE or RETRO/) = always an X (or slant line in teletype message)(month)= if advice is RETRO
cated for complete
RETROINTERVAL

the month should be indi‑clarity of dates suggested for

JJ = UT date advice given
HH = UT hour advice given
g = always a "0"

B.VI.2

ALERT
NATIONALMESSAGESFORINTER‑U R S I GRAM
AND
WORLD
DAYS
SERVICE

Code 1. ADALERT
1. Content.
Notification of advance alert
Type and importance3. Definition
IUWDS
ADALERTofsymbols.

= International Ursigram and World= Advance

Days Service

Alert(a) = place of origin
name of the Regional Warning Center, or ob‑
servatory, issuing the advance alert. Examples:
MEUDON,KOKUBUNJI,
SIMEIS, etc.
(b) = type of alert
MAGSTORM,
MAGCALME,
SOFLARE,
ACTIVITY,
or COSMICEVENT.
Not STRATWARM.

SOL‑

(c) = timing information
1. if phenomenon
has already started the nom‑
inal time of start is given by a date‑timegroup of the form: JJHHmmZ,
where
JJ =
Greenwich date
HHmm
= hours and minutes UT
Z =conventional symbol to indicate UT
2. if phenomenon
is in progress, indicate by
the word EXISTS
3. if phenomenon
is predicted, indicate by theword EXPECTED(d) = elaboration
1. for MAGSTORM
one can add the words:
AURORAOBSERVEDor AURORAPROBABLE,
or COSRAYDECREASE,
if appropriate
2. for COSMIC
EVENT one can add words:
COSRAYINCREASE,
or POLCAP
ABSORP‑TION
3. for SOLACTIVITY
one can add words:
FLARES or EAST LIMB or GAMMASUN‑SPOT or RADIO
SPOT
BORN, if appropriate

or NEWREGION(e) = time of issue
this time is indicated by the usual date‑timegroup JJHHmmZ
as in c.l.
Note: this group may be omitted if the timeof the phenomenon
is given in c.

NOTES

B.VI. 2 ALERTNATIONALMESSAGESFORINTER‑U RSI GRAM
AND
WORLD
DAYS
SERVICE

Code 2. GEOALERT
1. Content.
Notification of Geophysical Alert
Type and importance3. DefinitionIUWDSGEOALERTofsymbols.

= International Ursigram and World Days Service= World‑wide

GeophysicalAlert(a) = Date‑serial number, a 5‑digit group of theform JJnnn, where
JJ =Greenwich date of issue
nnn = Serial number of GEOALERT
message(b) = type of alert
MAGSTORM,
MAGCALME,

SOLACTIVITY,COSMICEVENT,
Not SOFLARE.

or STRATWARM.

(c) = timing information
1. if phenomenon
has already started the nom‑
inal time of start is given by a date‑timegroup of the form: JJHHmmZ,
JJ =Greenwich date
HHmm
= hours and minutes UT
Z =conventional symbol to indicate
UT
2. if phenomenon
is in progress, indicate by
the word EXISTS
3. if phenomenon
is predicted, indicate by
the word EXPECTED(d) = elaboration
1. for MAGSTORM
one can add words AURO‑RA OBSERVED,
or AURORAPROBABLE,
or COSRAYDECREASE,
if appropriate
2. for COSMIC
EVENT
one can add words
COSRAYINCREASE,
or POLCAP
ABSORP‑TION
3. for SOLACTIVITY
one can add words FLA‑RES, or EAST LIMB, or GAMMA
SUN‑
SPOT, or RADIO
SPOT, or NEW REGIONBORN, if appropriate(e) = Geographical Region of initial detection andmovement
expected, used only in connection
with STRATWARM
Note 1: an IUWDSGEOALERT
message is transmitted each
day soon after 04.00 UT; when no Alert is issued
the message reads IUWDSGEOALERT
NIL.
Note 2: the retrospective intervals of various kinds are in‑dicated in a GEOALERT
message of the form:

For further details see the IQSY
or C.I.G. News.

Instruction Manual

No. 1,NOTESNOTESNOTESNOTES

B.VII. Specialized

Network

Radio Propagation Indices
Code 1; PROPA
Code 2; PQ‑ N‑
Radio Propagation Forecasts
Code 1; PREVI
Code 2j ST‑
Code 3; MT‑
Code 4 j AD‑
Detailed Riometer
Code 1; SRIOD
Code 2; SRIOM

Data

Detailed Ionospheric Data
Code 1; ION ―Detailed Cosmic
Code 1; CORAJ
Code 2: RAYCO

Ray Data

B. VII. 1 RADIO

PROPAGATION

INDICES

Code 1. PROPA
1. Content.
Radio propagation indices for certain radio circuits,
monitored at the observatory

3. Definition
PROPA

of

symbols.

= key word, PROPAgation
JJ = Greenwich

conditions

date

X = always a "X"
II = observatory indicator
72 = 7TZ Darmstadt, observing station Detmold
a = circuit monitored
1 = North America
2 = South America
3 = Eastern Asia
4 = Canada
5 = India
6 = South Africa
bb = propagation index referring to day‑time, in tenthsof degrees in a scale from 0.0 ‑ 9.8 where
1 = useless
2 = very poor
3 = poor
4 = poor‑to‑fair5 = fair
6 = fair‑to‑good
7 = good
8 = very good
9 = excellent
cc = propagation index referring to night‑time, accord‑
ing to the same scale as bb
For circuits between Germany
and countries in theEast, the day period begins with sunrise in German)
and ends with sunset in the country of the corre‑
spondent. For circuits with countries in the West,the day period begins with sunrise in the countryof the correspondent and ends with sunset in Ger‑
many.
Ref. B. Beckmann;
About the definition of radio
propagation conditions.
URSI, 1954, No. 84, Comm.
III.
The quality indices are evaluatedfifthof a unit.

to the nearest

B. VII. 1 RADIO

PROPAGATION

INDICES

Code 2. PQ‑
Code 3. N‑Q
1. Content.
Preliminary propagation quality figures
Daily code 2, or weekly, code 3, reports

3. Definition
PQ
N‑Q

of

symbols.

= key for daily report= key for weekly reporta = circuit, or combination of circuits
A = Atlantic circuits
JJ = Greenwich date of beginning 24 hour period, incode 2
Greenwich date of beginning of first24 hour period,in code 3
cdef = preliminary quality figures for each of the periodsof the day, wherec refers to 1800‑2400
d refers to 0000‑0600
e refers to 0600‑1200
f refers to 1200‑1800
scale of quality figures is 1‑9
g = preliminary quality figure for whole day on scaleof 1; useless to 9, excellent

B. VII. 2
RADIO

PROPAGATIONFORECASTS

Code 1. PREVI
1. Content.
Daily radio propagation forecast for the direction Ger‑
many‑North America

3. Definition
PREVI

of

symbols.

= key word, "prevision"

JJ = Greenwich date of begin of the 24 hour period towhich the forecast refersa = expected quality figure for begin of day periodb =' expected quality figure for end of day periodc = expected quality figure for begin of followingnight periodd = expected quality figure for end of night period
scale of quality figures is from 1 to 9, where
1 = unusable and 9 = excellent
Note 1: The
quality figures give deviations from normal
conditions, which are predicted in the monthly
forecasts.
Note 2: As day period is considered the period in whichusually the day frequencies can be used; as night
period is considered the period in which usually
the night frequencies are to be used.
Note 3: For every forecast period two quality figures are
given in order to indicate the expected developmentof the conditions during the forecast period.

B. VII. 2
RADIO
Code

PROPAGATIONFORECASTS

2. ST‑

1. Content.
‑ Shortterm forecast

3. Definitionofsymbols.

a = Circuit, or combination
forecast is given
A = Atlanticof circuits for which

theJJ = Greenwich date to which forecast portion (number)of firstforecast statement (letter and number)appliescc‑ff = forecast statements, consisting of a letter and anumberj letters are encoded as follows:
W = 3 U
= 5 N
= 7numbers give expected quality, in a scale from
1 to 9periods to which the forecasts apply are as follows
cc : 0000‑0600
dd : 0600‑1200
ee : 1200‑1800
ff : 1800‑2400
g = always 0
h = check, units digit of sum of preceding 11 digits

B. VII.2
RADIO

PROPAGATIONFORECASTS

Code 3. MT‑
1. Content.
Mediumterm forecast

3. Definitionofsymbols.

a = circuit or combination
casts are given
A = Atlanticof circuits for which

fore‑

JJ = Greenwich date for which first twelve hour fore‑
cast applies
c = forecast quality figure; 0000‑1200, if a = A
d = FOT forecast for c: 1 = low; 2 = normal; 3 = highe = forecast quality figure; 1200‑2400, if a = A
f = FOT forecast for e: 1 = low; 2 = normal; 3 = highg = check, units digit of sum of preceding 6 digits

B. VII. 2
RADIO
Code

PROPAGATIONFORECASTS

4. AD‑

1. Content.
forecast for coming

3. Definitionof

7 day period

symbols.

a = circuit, or combination of circuits
H = high northern latitude
JJ = date of beginning of seven‑day period to which
forecast applies
cc = date of ending of seven‑day period to which fore‑
cast applies
dd.dd = forecast quality figures for each of the seven daysof the period
e = check, units digit of sum of preceding 11 digits
ff = date of beginning of disturbed period
gg = date of end of disturbed period
h = check, units digit of sum of preceding 4 digits

B. VII.3 DETAILEDRIOMETERDATA

Code 1. SRIOD
Symbolicform:

SRIOD DDXXX

Key:

/aabb

JJ/II eeeee
kkkkk

eeeee

hhhhh hhhhh

kkkkk

FF/oo /pp/qq/rr/ ss/tt uuuuu

ggggg

mmmmm

ggggg

mmmmm
uuuuu

vvvw

wvwx

MMNNX

SRIOD

= Specializednetwork RIOmeter Daily data

DDXXX

= identifyinggroup for key‑punch operators

aa = lasttwo integersof the year
bb = number of the month
JJ = day of the month
II = stationindicator
eeeee eeeee = hourly two‑digit values scaled in percent
of fullchart width for period 00‑04 UT
ggggg ggggg = hourly two‑digit values scaled in percent
of fullchart width for period 05‑09 UT
hhhhh hhhhh = hourly two‑digit values scaled in percent
of fullchart width for period 10‑14 UT
kkkkk kkkkk = hourly two‑digit values scaled in percent
of fullchart width for period 15‑19 UT
mmmmm
=
mmmmm

of

hourly two‑digit values scaled in percent
fullchart width for period 20‑23 UT

FF = monitored frequency in Mc/soo = calibration point for 0 ma in percent offull chart widthpp = calibration point for 1 mafull chart widthin percent of

qq = calibration point for 2 mafull chart widthin percent of

rr = calibration point for 3 mafull chart widthin percent of

ss = calibration point for 4 mafull chart widthin percent of

tt = calibration point for 5 mafull chart widthin percent ofuuuuu= check sum for each of the columns
inthe array formed by the data following
DDXXX

vvv = check sum for each of the rows in thearray formed by the data following DDXXX
w = checksum of uuuuu

uuuuu

x = checksum of vvwv

wv

MM

= daily maximum
chart widthscaled in percent of fullNN= daily minimum
chart widthscaled in percent of fullX = check sumof MMNNSamplemessage

SRIOD DDXXX/

6103 05//4 54545

75759

58585

86467 73798 37381 87767

37877

72676

259/2 30/00 /20/4 1/61/

81102

60754

18266 96267 69055 88534

B. VII. 3 DETAILED
Code

DATA

2. SRIOM

SymbolicKey:

RIOMETER

form:

SRIOM
EVTXX

SRIOM

EVTXX

/aabb

JJ/II /TSTA/T MAX/TEND

dddee /AAFF

uuuuu

vvvvv

vvwx/

= Specialized network RIOMeter

event report= identifying group for key‑punch

operators

aa = last two integers of the year
bb = numberof the month

JJ = date
II = station indicator
TSTA= time of start of event in UT

TMAX= time of maximum

TEND= time of end of event in UTof event in UT

ddd = maximum
absorption during event intenths of db
ee = numberAAof peaks during event= antenna identification

ff = frequency monitoreduuuuu

in Mc/s= check sum for each column
in thearray formed by the data following
EVTXX

vwvv

Samplevv = check sum for each row in the array
formed by the data following EVTXX
w = checksum of uuuuu

x = checksum of vwvv

vv

message:
SRIOM EVTXX /6302

12/19

/1740

/2032 /2347 04207

/1030

18557

13276 3466/

B.VII.4 DETAILEDAll Purpose

IONOSPHERIC

Ionospheric

CodeThis code is used for both weekly
Code

word:

Symbolic
IONaa

ION

DATA

and monthly

messages.

for ionosphere

form:
bbbbb
ccdee

fgggh ijjjk (plus additionalgroups like fgggh ijjjk) 11111

Key:
aa = station indicator

PO ‑ Pole Station
LA ‑ LittleAmerica
EL ‑ Ellsworth
KX ‑‑ Byrd
WilkesBD
bbbbb

AR ‑ Cape Adare
AN ‑ Anchorage
BE ‑ Belvoir
etc.

= ionospheric characteristic reported:
FOFTO ‑foF2
HIFTO ‑ h'F2
FOFON ‑
foFl
HIFFF ‑ h'F
FOEEE ‑
foE
HIEEE ‑ h'E
FOESS ‑
foEs
HIESS ‑ h'Es
EFBES ‑fbEs
EFMIN ‑ f‑min

MUFTO‑
MUFON‑

MM(3000)F2(3000)F1

beginning date of observationsreported(indi‑vidual hourly values)ormonth; 01 = Jan. ,02 = Feb. , etc. (monthly
median values)

types of values
0 ‑ hourly values within a 24‑hour period(Standard Meridian Time)
9 ‑ monthly median values (Standard MeridianTime)8 ‑ values at 6‑hour intervals for a period of
more than 24 hours starting on date cc
Note: In reporting a week's data, startwith 00 hours on Monday(Standard Meri‑dian Time)
7 ‑ values at 6‑hour intervals, from scheduled
ionograms taken on hour nearest to Local
Mean
Time.
Note: By arfangement, Universal Timemay be used instead of Standard MeridianTime.
ee = number of groups of data of characteristic
bbbbb which follow
f = even hour indicator: (see Table

NOTES

1, below)TABLE
Coding

Coded
as

1

Hour of Observation (f and i)

If coded in firstgroup of pair, (i.e. "f")hour isIf coded in second
group of pair, (i.e. "i")hour isvalue (report as 000 if symbol
symbol (list A, below)
Numerical

only applicable)

LIST A
Coding for Letter Symbols (h and k)

The following numbers are used as the final
digit of each group to indicate symbols which
explain doubtful or missing values.

Coded asSymbol

X

none

1 6
2 7
3 8
4 9
5 0

AB FL
C I
D T
E any

other

i = odd hour indicator; (Table 1, above)
jjj = valuek = symbol (see list A, above)
11111= sum of all ggg and jjj values in precedinggroupsNOTES

B. VII. 5 DETAILEDCodeCOSMICRAY

DATA

1. CORA]

Symbolic

Form:
CORAJ

JJall bcdef

gijkl nosst

HHHvv

Key:
CORAJ

= COsmicRAydata (Japan)

JJ = Greenwich date of observation (UT)a = apparatus
0 = Neutron Monitor
1 = Meson Monitor (10 cm Pb, + 45 °,
14,400 cm2)
2 = Counter telescope (no shielding, + 70 °,
14,400 cm2)
3 = Counter telescope (10 cm Pb, + 70 °,
14,400 cm2)
4 = Counter telescope (10 cm Pb, + 20 ° x+ 70°,16,630 cm2)
5 ‑ Inclined telescope directing North (10cm Pb, 30 ° +15 °,4, 190 cm2)
6 = Inclined telescope directing South (thesame as 5)
7 = Inclined telescope directing East (thesame as 5)
8 = Inclined telescope directing West (thesame as 5)
II = observatory indicator
26 = Cosmic Ray Observatory (I.P.C.R.),
Mt. Norikura, 2770 m above sea level
51 = The Instituteof Physical and Chemical
Research, Tokyob = meanintensity for 0000‑0200

U.T.

Daily mean value is expressed by the figure
5, and the deviation for two hours' period
from the daily mean value is expressed asfollows:

9 = +
8 = +
7 ―+
6 = +
5 = 0

4%
3%
2.%
1%

4 = ‑ 1%
3 = ‑ 2%
2 = ‑ 3%
1 = ‑ 4%0 = ‑ 5%The scale unit of deviation for the observa‑
tional data obtained by apparatus "0" should
be doubled.

(0.2% for apparatus "0") corrected for thebarometer effect, 50 corresponds to that of
September 1, 1961.
t = classificationof unusual phenomena
0 = calm
1 = increase
2 = after‑effect of increase
3 = decrease
4 = after‑effect of decrease
5 = daily variation of large amplitude
6 = daily variation of anomalous phase
If "t" is other than "1", HHHvv
HHH

are omitted= time of maximum
intensity in hours andtenths U.T.
vv = percentage of the increment.

B. VII.5 DETAILEDCOSMICRAY

DATA

Code 2. RAYCO
1. Content.
bi‑hourly flux values of cosmic rays,daily variation,
special events.

3. Definition
RAYCO

of

symbols.

= key word, Rayons

Cosmique

JJ = Greenwich date of firstperiod for which flux
values are given
T = type of apparatus
1 = meson telescope, 130 x 130, without shield‑
ing
2 = meson telescope, 50 x 100, shielded with
10 cm of lead
7 = neutron monitor, Simpson type
II = observatory indicator (see also lists in part C)
10 = Meudon 36= Pic du Midi 46= NERA
HH= hour indicator; deviation of flux from the normal
value following under aaa refers to the interval
HH‑1, HH + 1 hours
if the deviation is positive 30 is added to thehour to obtain HH.

deviation of cosmic
level in 0/00

ray flux from the "normal1

sign of daily variation
7 = negative 8= zero 9= positive
type of variation during the day
0 = normal daily variation
1 = beginning of a prebaisse
2 = prebaisse
3 = commencementof a Forbush decrease
4 = Forbush decrease
5 = recurrent activity
average deviation from normal flux .

NOTES

List 1.

PART

‑

C.

Observatories andindicatorsorder and codes applicable

UFLAG, USSPO,UPATAUCOSC,URANA
URANA,USSPc
U fZA<v P
UFLAR,USIDAURANS,USIDA,UDISE, UMAGA,
ADV, URANE,URALA,URALO
UFLAG, USSPO,
UPATA
UMAGA
USIDA
UFLAG, USIDA,
UCORA,UMAGA,UFOFA, UFOFE,UPATA
UFLAG, UPATA
UFLAG, USIDA,
UMAGA,USSPO,UFOFA, UFOFE,UPATA
UFLAG, USIDA,
UPLAG,UPDIA,UPATA,UACTA,UEVTAUABSBUFOFA, UFOFE.
UFLAG, USSPO,USSPM,
UPATA

Codes

indicators in numerical

Observatory

20
21

14
14
15
15
16
16
17
17
18
19
19
19
20
20

12
12
13

10
10
11

09

Indicator

Observatory
Country

USIDA,UFLAG,UMAGA
URANA,USIDA,UFLAG,UFLAG,UABSB,
UCOSA
UAURA
USSPO
URALA,UFOFE
URANE
URALA,URALC
UFOFA,UFOFE
UPATAUSSPO, UPATAUFOFE, UAURA,(SOA/US'UFOFA,UPATA,URANP,UMAGA,USSPO,UCORA,UFOFA,URALO

UFLAG, UPATAUSIDA, UDISE, UAURA,ADVUFOFA, UFOFE
UCOSC
UMAGA
URANA
jURANP,URANE,USIDAUSIDA, UDISE, UMAGA,UFOFA,UFOFE, ADV, UEVTAUS OX AUCORA,UCOSA
UMAGAURANA,URANP,USIDA, UDISEUFOFA, UFOFE

Codes

USSPO,Polef USSPOUABSBUCORA,UEVTA
UAURA,UFLAG,URANP

UFOFA,UMAGA,UFLAG,

UMAGA

UCOSC

UFLAG,UPATA,

UPATE,UFLAG,UMAGAUCOSAUSIDA,UCORA,

URANE

USIDA

URANA,UPATA

ADV

URANP,URANA,UFOFE,

URANS,

URANT,UMAGA

USIDA,UFOFA,UFLAG,U.S.A.

Sacramento

32

URANS

UCORA,
UACTA

UABSB

Antarctica

South

32
Peak

UABSB

Antarctica

McMurdo31

UFOFA,USIDA,U.S.A.

Ft.

31

Monmouth

UMAGA

U.S.A.

￡oXA

Codes
0

Frederickst/urg

＼‑Ay

31

Country
0 ＼S

Observatory

3JL

Indicator.

USSPE,URANE

USSPO,UFOFE

UPDIE,:UMAGA,USIDA,

USIDA

UFOFE

UPDIA,UFOFE

URANS,UPATAUCOSA,USOXA,UFOFA,UPATA,

51
51
52
53
54
55

46
46
46
47
48
49
51

42
43
43
45
45
46

41
41
41

Indicator

Observatory

Country
URANA,UFOFE
UFLAG,UFOFE,
UAURA
UABSB
UCOSA
UFLAG
URANE
UABSB
USSPO
VPLA&,UFOFE,UEVTA
USSPOURANA,UFLAG,URANA,URANA,UMAGA
USIDA,USIDA,USIDA,UEVTAUCOSAUSIDA,

Codes

UFOFA,UPDIE,UCOSAUPATA,USIDA,UPATA,URANP,UPDIA,URANP
URANP,UFOFE,UFOFA,UMAGA

UFOFA,UFOFE
UFOFE, UCOSA
ADV, PROPA,
PREVI

UFOFE

UACTA

UPLAG,UACTA,UFOFA,UFOFA,UMAGA,UFOFA,UDISE,UFOFA,UMAGA,USIDA,

URANE,UPATA

URANP,

80

Irkutsk

U.S.S.R.

UFOFA,UFOFA,ADVUSSPO,UPATA,UFLAG,USSPO,URANP,UPATA
URANA',UFLAG,URANA,UMAGA,UFLAG,UPATA

UMAGA,USIDA,UCOSAUEVTA,URANA,UACTA,UFLAG,ADV

UEVTA,UACTA,

USSPM,URANA,UFLAG,UPATA,UPATAUSSPO,, UMA/A

URANP

UFOFE

UFOFA,UFLAG,UDISE,USIDA,UMAGA

UFOFA,USIDA,UMAGA,USIDA,UCOSCUSIDA,UMAGA,

UCo$$

Codes

UFOFE

URANP,UFLAG,"UPATA

UFOFA,UPATA

UFOFA,URANP,UFOFA,UDISE,URANP,＼0

UABSB,

UFOFE

UFOFE

UFOFA,.

USSPO,

USSPM,USUFOFEUFOFE,USSPO,UFOFE,UMAGA,USIDA,

UMAGA

UFOFE

iP/j

Indicator

Observatory

Country

URANA,USSPO,USSPOUFOFA,UFLAG,URANA,UPLAG,UFOFA,UFLAG,UPATA
URANA,UFLAG,URANA,UFOFA,USSPO
UFLAG,

Codes

UPATA

UPATA

UFOFE
USSPO,UFOFE,UFOFA,URANP
UFLAG,USSPM

USSPO,
USIDA

UPATA

UFLAG

UFOFE,USSPO,USSPO,UFOFA,UCORA,UACTA

URANP,UPATA
URANP,UFOFE,URANP,UPDIE,UFOFEUCORA,

INDEXOFMENTIONED
CODES
Nuniber

Keywordofcode.Page;
1ADALERTVI2‑1
2AD‑VII2‑4
3ADVVI1‑1
4CORAJVII5‑1
5GEOALERTVI2‑2
6ION ―VII4‑1
7MT‑VII2‑3
8N‑QVII1‑3
9PQVII1‑2
10PREVIVII2‑1
11PROPAVTT1‑1

Number
KeywordofcodePage
44
86
86
.06
47
49
53
51
80
81
66
72
69
77
75
90
61
39
36
34

NOTESNOTES