Diese Mitteilungen setzen eine von Erich Regener begrundete Reihe fort, deren Hefte

auf der vorietzten Seite genannt sind.

Bis Heft 19 wurden die Mitteilungen herausgegeben von J. Bartels und W. Dieminger.

Von Heft 20 an zeichnen W. Dieminger, A. Ehmert und G. Pfotzer als Herausgeber.

Das Max-Planck-Institut fur Aeronomie vereinigt zwei Institute, das Institut fur Strato­

spharenphysik und das Institut fUr lonospharenphysik.

Ein (5) oder (I) beim Titel deutet an, aus welchem Institut die Arbeit stammt.

Anschrift der beiden Institute:

3411 Lindau

X-RAY MEASUREMENTS

IN THE AURORAL ZONE

FROM JULY TO OCTOBER 1964

by

G. KREMSER. E. KEPPLER. A. BEWERSDORFF. K. H. SAEGER.

A. EHMER T. and G. PFOT ZER

Institut fUr Stratospharenphysik am Max-Planck-Institut fUr Aeronomie

3411 Lindau/Harz. Germany

W. RIEDLER

Kiruna Geophysical Observatory Kiruna C. Sweden

J. P. LEGRAND

Laboratoire de Physique Cosmique Station de Chalais -Meudon

Meudon. France

ISBN 978-3-540-03365-3 ISBN 978-3-662-13448-1 (eBook) DOI 10.1007/978-3-662-13448-1

- 3 -

Contents

I. Introduction...................................... p. 5

II. Technical remarks 5

III. Solar activity and its terrestrial effects .••......•.. 7

IV. List of the balloon launchings ••.....•.........•.... 13

V. Representation of the measurements 14

Summary......................... ..•....••.•••... 22

Acknowledgement.................................. 22

References 23

VI. Diagrams of the flights ..•.••......•....•.••••.•••. 25

- 5 - I., II.

I. Introduction.

In this report the data of balloon flights, carried out from July to October 1964 in Kiruna/Sweden

are compiled. They were performed by the joint group of the Institut fUr Stratospharenphysik am Max­

Planck-Institut fUr Aeronomie, Lindau/Harz, Germany, of the Kiruna Geophysical Observatory, Kiruna,

Sweden, and of the Laboratoire de Physique Cosmique, Meudon, France.

Herewith the sequence of flights started in 1960 by the Lindau and Kiruna group [PFOTZER et a!.

1962a) and since 1963 executed in the frame of SPARMO is continued [PFOTZER et a!. 1962b, PFOTZER

et a!. 1965).

In this campaign 53 balloons were launched, which carried scintillation counters, Geiger-Miiller­

tubes, and ionization chambers in different combinations.

In what follows one finds

technical remarks concerning the balloons and the instruments ( section II ),

a description of the solar activity and its terrestrial effects during this balloon launching period

( section III ),

a list of the balloon launchings ( section IV ),

representations of the radiation measurements,remarks on the indications for launchings and some

special comments ( section V ),

diagrams of the flights ( section VI ).

II. T e c h n i cal rem ark s .

a) Ball 0 0 n s

As in the 196~ campaign [PFOTZER et a!. 1965) tetrahedron type balloons of 5 DOG m 3 were em­

ployed, which were manufactured by the" Centre de Lancement, Aire/l'Adour, du Centre Natio­

nal d 'Etudes Spatiales, France".

b) Instrumentation

The instruments used during this campaign differed only slightly from those launched in 1963.

According to their composition they are denoted by : TESI, TESCI, TESIO, I. C.

TESI: A threefold coincidence telescope formed by three Geiger-Miiller-counters, where also the coun­

ting rates of the topmost and the middle counters are telemetered to the ground ( Victoreen 1 B 85

and 6306 ). The TESIS are manufactured by the factory Albin Sprenger K. G., St-Andreasberg/Harz

[KEPPLER; 1964].

TESCI: A combination of a threefold coincidence telescope of Geiger-Miiller-tubes ( 3 counters Victoreen

1 B 85 ) and a Na I ( Tl )-scintillation counter. Tn some flights only the uppermost counter of the

telescope was used to compare the counting rates of the Geiger-MUller-tube and the scintillation

counter. The TESCIS wer.e manufactured by the Institut fUr Stratospharenphysik am Max-Planck­

Institut fUr Aeronomie, Lindau/Harz, Germany [ROSSBERG and SPITZ to be published).

II. - 6 -

TESIO:Version of balloon instruments used until 1962, contained a vertically mounted AI-walled Geiger­

MUller-counter, a telescope as in the TESCI and an ionization chamber ( see I. C. ). The TESIOS

were manufactured by the Institut fUr Stratosphlirenphysik am Max-Planck-Institut fUr Aeronomie,

Lindau/Harz, Germany.

1. C. Ionization chamber of the Neher-type.

Table 1 gives the characteristics of the various detectors.

Table 1

Characteristics of the various detectors.

absorb. Energy-eff. layer of geom. threshold ( MeV)

Detector Type diD length the wall factor*)

elec- protons 2 cm2ster cm cm mg/cm trons

Al-GM 1 B 85 1. 9/- 7.0 30 75 0.16 3.8

Bi-GM 6306 1. 9/- 7.0 135 75 0.4 5.5

TESI 1.9/4.6 7.0 360 6.9 0.9 14

Telescope TESCI 1. 9/4. 6 7.0 150 6.9 0.6 9

TESIO i.9/4.6 7.0 150 6.9 0.6 9

Ionization NEHER 25/- - 480 3080 1.1 16 Chamber

Scintillator TESCI 2.54/- 2.54 50 48 0.22 4.7

It) Definition of the geometry factor G for isotropic radiations: ,..-d-.. I , , , , ,

N = £ • G, <P ( Ephot )

N = counting rate

E = efficiency

G = geometry factor

4>( Ephot ) = flux of monoenergetic photons/cm2 sec sterad

- 7 - III.

III. Sol a r act i v i t y and its t err est ria 1 e f f e c t s •

The balloon flights were performed during the solar rotations 1792 to 1795 of which following rele­

vant features are represented in Figs. 1-4 :

the ZUrich relative sunspot numbers ( CRPL Boulder reports ),

the position of plage regions on which flares occurred ( CRPL Boulder reports ),

the duration of balloon flights at Kiruna, marked by rectangular boxes, whereby the letter X above

a box means that X-rays were measured during these flights,

the duration of balloon flights at other stations,

3 -hourly· planetary amplitudes ap (by courtesy of Geophysikalisches Institut, Univers. Gottingen ),

hourly neutron counting rates at Deep-River :( CRPL Boulder reports ).

The solar activity during these rotations was very low due to the approach towards the minimum

of the sunspot cycle. The relative sunspot number never reached 40 ; it was even zero during periods of

ten and more days. Only a few flares of importance 1 and 2 occurred, none of importance 3.

In spite of this very low solar activity several weak or even medium geomagnetic storms occurred.

Some of them began with an ssc and/or were accompanied by small Forbush effects « 2%). However, none

of the Forbush effects could be linked to a solar flare.

As the geomagnetic storms and the Forbush effects are manifestations of solar plasma clouds

which are in some way also the source or the cause of the X-ray bursts, we have measured during our

balloon flights, they shall now be described in more detail.

Solar rotation 1792 (July 2 to July 28, 1964) (Fig. 1)

Three weak geomagnetic storms occurred. Only the first one began with an ssc,on July 2 at 23.25 UT.

No Forbush effect was observed on this day. This happened, however,. in association with the third grad-I

ually commencing storm, on July 17. Flights K1/64 to K4/64 were started to cover this disturbance

period.

As can be seen on Fig. 5 all storms are linked to. more or less persistent M-regions passing the

central meridian [BARTELS, 1932). The first storm during this rotation is connected with an M-region,

which recurred five times. The second one belongs to an M-region, which appeared in August 1962 and

returned until October 1964. This region showed an outstanding recurrence tendency; it recurred at least

30 times. The third storm occurred again during the recurrence of a less persistent M-region, which re­

turned perhaps 8 times and which began 2 days earlier for the next three rotations.

Solar rotation 1793 (July 29 to August 24, 1964) (Fig. 2)

On August 5' a flare of importance 2 could even be observed in the visible light *) • But we cannot

find terrestrial effects attributable to it. Again three geomagnetic ally disturbed periods belonging all to

M-regions can be distinguished. In the second and third period weak geomagnetic storms occur ed, begin­

ning with ssc's on August 4 at 01.30 UT and on August 11 at 00.55 UT respectively. Both were accompa­

nied by small Forbush effects. Flights K 9/64 to K 12/64 were launched to cover the second disturbance

period, flights K13/64 to K16/64 to cover the third one.

*) Ionospharen-Berichte, edited by Deutscher Wetterdienst, Hamburg, and by the Arbeitsgemeinschaft Ionosphare, Darmstadt (Germany).

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Solar rotation 1794

(August 25 to September 20, 1964) (Fig. 3)

During this rotation four weak geo­

magnetically disturbed periods can be dis­

tinguished. The third of them was a geo­

magnetic storm beginning with an ssc on

September 6 at 19.55 UT.

This disturbance and the fourth

one were accompanied by small Forbush

effects.

Flights K21/64 to K24/64 were

launched during the second, flights

K27/64 to K32/64 during the third, and

flights K33/64 to K35/64 during the

fourth disturbed period.

Solar rotation 1795

(September 21 to October 17, 1964 (Fig. 4)

The geomagnetic activity was

higher than during the preceding rota­

tions. During a storm beginning with an

ssc on September 21 at 11.48 UT the

apts reached even a value of 179. This

was also the only storm accompanied by

a Forbush effect. The recurrent dis­

turbed periods which developed from

those of the preceding rotation lasted

longer and partly overlapped. Flights

K37/64 to K53/64 cover more or less

closely this rotation until the end of the

launching campaign.

Fig.5 : Daily geomagnetic character fi­gures C9 and sunspot number R. Sym­bolic tabulation in the 27 -days sequence of the solar rotations after BARTELS. The recurrences of the M-regions are clearly seen. These diagrams are dis­tributed by the Geophysikalisches In­stitut der Universitat Gottingen, Ger­many, on request.

- 12 -

R C9 "553J,11 19 J23 .. ,13 .. 1 ... 5 .. 5.,35"3"'1'. 1'31 ,7]"3,,16. n9 .d312H .111."1 .. 31'1.1 .. 1'3' .. ,'5 JJ 11.3 10118 141' ... 1 ... 1 .. 3 1'3 1" '3' 51 ... 11 131 '55'3H33 1762 A 11, .1113135'3.3311 .. 11 •.. 51 ... '1.3"; 31d5"31 6310111 1.3 "z .. 3 ....... 3. ,.52 .. 313 1.5 '.1 1335'3133 61, J 71.5'.2.13 ..... 33' .. 15'''111'15'313. 1111111.. 65 J I, H3 13.11131 .... 3'311' ,"51' 3'33.1 ... ,14331 66 JIf 3'33.155'53 ... 15555'. ",HI'"'''' .355"'11 67A27 .• ,,""'45'U31'53'11."351'·,'11 I." 113 553 68 S23 , .. '11 54' 533 3,'3 "5 '13 '35 1" 3'55" 33311. 11' 69 020 345 5""53'11" 5.5 41 .. J .. "1"1 ... 5 53. 1.3 43. 1770 N16 '1. ..5 '54 5'1 11' 1 .. '1. ... .'J '31 ." 1 • J 1 .. 13. 71 013 '33 ." "5 3 ... , .... 3, .. 1. .,.' ..•• "

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"I III 111 7798 077 . I • I' '" . . . . . • •. .... J I. . ., I •. J

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Symbol . 1 3 , R . 0

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DAILY GEOMAGNETIC CHARACTER FIGURES C9

AND SUNSPOT NUMBERS R

-13- IV.

IV. List of balloon launchings, Kiruna 1964.

Start End of Ceil- balloon stayed above Duration

Flight Type of transmission ing 50 mb pressure level of flight

Nr. Detector date time date time pres- from to above Remarks (UT) (UT) sure date time date time 50 mb

(mb) (UT) (UT) pressure level (h).

K 1/64 TESI 16.7 2200 17.7 1900 8 16.7 2320 17.7 1900 20 K2/64 TESCI 17.7 2020 18.7 0700 7 17.7 2142 18.7 0450 7 K3/64 TESCI 18.7 1938 18.7 2258 7.5 18.7 2115 18.7 2300 2 K4/64 TESI 19.7 2208 20.7 1300 6 19.7 2326 20.7 1300 14 K5/64 TESI 21. 7 2110 22.7 0905 7 21. 7 2224 22.7 0900 11 K6/64 TESCI 27.7 21201 28.7 0036 6 27.7 2243 27.7 2345 1 K 7/64 TESCI 29.7 2110 - failure K8!64 TESI 30.7· 2112 31. 7 1200 6 30.7 2226 31. 7 1200 14 K9/64 TESI 2.8 2104 3.8 2030 6 2.8 2218 3.8 2030 22 K10/64 TESCI 3.8 2108 - failure K11!64 TESI 4.8 2101 5.8 2032 6 4.8 2225 5.8 2030 22 K12/64 TESCI 5.8 2115 6.8 2000 9 5.8 2335 6.8 2000 21 K13/64 TESI 11.8 2005 12.8 2045 7 11. 8 2135 12.8 2045 23 K 14/64 TESCI 12.8 2002 13.8 1920 7 12.8 2115 13.8 1920 22 K 15/64 TESCI 13.8 2000 14.8 2300 6 13.8 2115 14.8 2230 25 K16/64 TESCI 14.8 2145 15.8 0335 8 14.8 2306 15.8 0100 2 K17/64 TESI 18.8 2007 19.8 2117 6.5 18.8 2131 19.8 2115 24 K 18/64 TESCI 20.8 2210 - failure K19!64 TESI 25.8 1942 26.8 2020 8 25.8 2140 26.8 2020 22 K20/64 TESI 29.8 1912 - failure K21/64 TESCI 30.8 1912 31.8 2200 7 30.8 2145 31.8 1925 22 K22!64 TESI 31. 8 1910 - failure K23/64 TESCI 31. 8 2202 1.9 2020 7.5 31. 8 2325 1.9 2000 21 K24/64 TESI· 1.9 1948 2.9 2200 7 1.9 2109 2.9 2010 23 K25!64 TESI 3.9 2033 - failure K26/64 TESI 4.9 1728 4.9 2000 8 4.9 1850 4.9 1947 1 K27!64 TESCI 5.9 1709 6.9 2310 5 5.9 1820 6.9 1900 25 K28/64 TESI 6.9 1810 6.9 2220 8 6.9 1945 6.9 2130 2 K29/64 TESI 6.9, 2317 7.9 2030 10 7.9 0051 7.9 1900 18 K30/64 TESCI 7.9 1645 7.9 1922 14 7.9 1800 7.9 1850 1 K31/64 TESI 7.91 2051 8.9 1856 7 7.9 2210 8.9 1815 20 K32/64 TESI 8.9 1843 9.9 1955 7 8.9 2010 9.9 1845 23

+ I.C. did not work K33/64 TESCI 14.9 1855 15.9 1630 5 14.9 2005 15.9 ? ? after ceiling K34!64 TESCI 15.9 2312 16.9 1800 7 16.9 0145 16.9 1740 16 K35!64 TESI 16.9 1918 17.9 0042 9 16.9 2039 16.9 2355 3 K36/64 TESCI 18.9 2212 19.9 0605 5 18.9 2329 19.9 0145 3 K37/64 TESI 22.9 0947 22.9 2050 9 22.9 1103 22.9 1818 7

+ I.C. K38/64 TESIO+ 22.9' 2210' 23.9 1325 6 22.9 2315 23.9 1325 14

TESCI K39/64 TESCI 25.9 0010 25.9 0850 6 25.9 0200 25.9 0850 7 K40/64 TESI 25.9 1536 25.9 2230 6 25.9 1645 25.9 2230 6 K41!64 TESCI 28.9 0019 28.9 1025 5 28.9 0135 28.9 1025 9 K42/64 TESI 28.9 1806 29.9 0130 7.5 28.9 1923 29.9 0130 6 K43/64 TESCI 28.9 2358 29.9 1055 6 29.9 0106 29.9 1055 10 K44/64 TESI 30.9 1805 1.10 0320 7 30.9 1911 30.9 2340 5 K45/64 TESI: 2.10 2039 3.10 1000 no pressure

measurement K46/64 TESCI '3.10 1551 4.10 0200 6 3.10 1700 4.10 0200 9 K47/64 TESI 4.10 0954 4.10 1630 7 4.10 1054 4.10 1455 4

TESCI + I.C.

K48/64 TESI 4.10 1758 5.10 0030 7 4.10 1903 5.10 0030 5 squibbed at K49/64 TESCI 5.10 0433 5.10 0645 14.5 5.10 0545 5.10 ? ? 14.5mb K50/64 TESI 5.10 1714 5.10 1927 10 5.10 1825 5.10 1905 0.5 K51/64 TESIO+ 6.10 0413 6.10 1435 10 6.10 0520 6.10 1300 8

TESCI K52/64 TESI + 7.10 0333 7.10 1440 5 7.10 0440 7.10 1240 8

TESCI K53/64 TESCI 7.10 1955 8.10 1030 6.5 7.10 2118 8.10 1030 14

V. - 14 -

V. Representation of the measurements.

The counting rates of all flights during which X-rays were measured are plotted versus time. In

addition the counting rates of the single Geiger-MulIer-tubes and the telescopes as well as of those scin­

tillation counters, which descended just after ceiling, are plotted versus pressure.

The intensity versus time diagrams.

a) The counting rates of the various detectors or of the different channels of the scintillation coun­

ters are plotted versus time on a logarithmic scale as given on both sides of the diagrams.

Under each curve a base line is drawn which indicates how the logarithmic scale must be ad­

justed for this curve. The following notifkations hold:

AI-GM:

Bi-GM

Te

1. C.

AI-walled Geiger-MulIer-tube ( Victoreen 1 B 85 ),

Bi-coated Geiger-MulIer-tube ( Victoreen 6306 ),

Telescope,

Ionization chamber.

Curves, which are labeled with energy thresholds represent the counting rates due to different

energy losses in the crystals of the scintillation counters. Corrected values for the thresholds

as determined retrospectively after an inflight calibration are inserted in Table 2. ( See remarks

on the preflight and inflight calibration in section d. )

b) The air pressure P at the balloon altitude is indicated by full dots. It is plotted also on the same

logarithmic scale as the counting rates. In order to indicate the appropriate decade one pressure

level is marked on each diagram.

c) CNA-curve. During these flights the riometer did not always work satisfactorily. Sometimes the

CNA-curve is therefore omitted or only indicated by a dashed line ( short dashes ). On most of the

diagrams a quiet day absorption curve is tentatively drawn also by a dashed line ( long dashes ).

d) Remarks on the calibration of the thresholds for the energy losses in the scintillation counters.

Preflight calibration.

A nominal setting of the thresholds was provided at 20 keY, 40 keY, 100 keY, and 500 keY. But

these are only inserted in the diagrams, if they deviated by less than 10"/0 from final preflight cali­

bration values. This calibration was based on the 662 keY line of 137 Cs. On the base of a linear

relation the thresholds were calculated from the ratio of the pulse height due to this line and those

at which the discriminators for the different channels responded.

Inflight calibration

A probably more reliable calibration can be achieved by means of an average curve of the

pulse height distribution due to the cosmic radiation at its secondary maximum.

Assuming that allowance can be made for the deviation of the cosmic ray intensity from a cer­

tain arbitrary chosen reference level, for instance on account of a neutron monitor record [ERBE,

1959) and assuming furthermore that the variation of the energy distribution and of the particle

composition is a second order effect in this concern, the counting rates at the outputs of the dif­

ferent energy channels must be a unique function of the corresponding thresholds. Hence from the

counting rates of the maximum, normalized after the above viewpoint, the actual threshold for each

channel can be checked or respectively redetermined inflight.

This calibration function

has been obtained retro­

spectively on a statistical

base by plotting in Fig. 6

the counting rates of the

maximum for times when

no excess radiation was

present, versus the origi­

nal preflight values ( see

above ). We took then the

best fit curve as true re-

sec-I

300

200

presentation of the relation 100 between the actual counting

rate and the actual thre­

shold of each individual

channel and used it for the

evaluation of the corrected

70

50

thresholds from the mea- 30 sured counting rates. These

thresholds are inserted in 20 Table 2.

10

.. I--

10

- 15 -

Calibration of the scintillation counters

by the

cosmic

.. '.

20 30

counting rates in

ray maximum

I . ,.: ..

..

50 70 100

the secondary

.

200 300 500 keV

calculated energy level

V.

Fig.6: The counting rates in the secondary cosmic ray maximum versus the calculated energy level. With the aid of this curve the energy levels (B) in Table 2 are deduced.

Table 2

Calibration of the scintillation counters by the counting rates in the secondary cosmic ray maximum

Nominal thresholds Flight Nr. 20 keY 40 keY 100keV 500 keY

A B A B A B A B

K3/64 30 20 55 45 140 153 660 530 K6/64 20 17 40 33 110 84 500 460 K 14/64 20 18 45 42 100 105 500 470 K 15/64 17 20 25 26 83 79 500 510 K 16/64 20 15 40 32 120 150 500 500 K21/64 20 17 40 39 87 96 500 490 K27/64 16 20 32 38 87 105 500 505 K33/64 25 24 40 49 115 110 500 500 K 34/64 23 31 40 38 100 95 500 540 K36/64 20 21 45 37 115 105 500 440 K 38/64 22 20 46 51 100 105 500 520 K39/64 20 34 40 51 100 69 500 480 K43/64 20 37 40 59 85 150 500 580 K46/64 20 22 40 35 100 110 500 460 K49/64 20 17 40 33 100 86 500 460 K51/64 24 20 40 41 116 150 500 500

A = energy level marked on the diagrams ( preflight calibration ).

B = energy level after Fig. 6 ( inflight calibration ).

V. - 16 -

e) The diagrams of the intensity versus pressure contain no additional curves. Here the intensity is

plotted on a linear scale. The energy levels marked at the curves of the scintillation counters are

those obtained by preflight calibration.

f) Indications for launchings and comments concerning the flights.

K 1/64

Indication: Routine flight to test the equipment.

Two weak X-ray bursts were recorded.

K2/64

Indication: Flights K 2/64 to K 4/64 were launched to cover an expected recurrence of an M-region

( see comments on solar rotation 1792 ).

Great X-ray bursts were recorded when the balloon stayed above the 40 mb pressure level. Ail

bursts were accompanied by AA-type CNA events.

K3/64

Indication: see K2/64.

One relatively soft X-ray burst occurred.

K4/64

Indication: see K2/64

The balloon was started during a disturbed period. Already at the secondary cosmic ray maximum

additional radiation was measured, which continued until about 03 UT. Especially remarkable is the

double-peaked event at about 01 UT, which is due to harder X-rays than the preceding and the follo­

wing ones. It is accompanied by less enhanced "absorption than the other events.

Another weak X-ray event occurred at about 10 UT.

K5/64

Indication: Simultaneous SPARMO flight.

No additional radiation.

K6/64

Indication: Routine flight.

Balloon was squibbed at 7 mb.

KB/64

Indication: Routine flight.

Perhaps one weak X-ray event occurred just after 00 UT.

K9/64

Indication: Flights K 9/64 to K 12/64 were launched to cover the period durihg which an M-region

was expected to recur ( see comments on solar rotation 1793 ).

One very small X-ray event occurred at about 23.40 UT. It was accompanied by a small peak in the

CNA. This event occurred during the maximum ( -BO Y ) of a very smooth bay disturbance at Kiruna.

- 17 - V.

K 11/64

Indication: see K 9/64

Some very weak ~-ray events were recorded. Remarkable is the single peak just after 20 UT on

August 5. It was accompanied by a sudden increase of the CNA of 0,5 db and a sudden decrease

of -215 y ,but only in the X-component of the geomagnetic field, which recovered slowly during

about one hour. Though the sun was above the horizon at this time, we cannot ascribe this peak to

solar y-rays, as no special events were observed on the sun.

K12/64

Indication: see K9/64

X-rays were recorded during the total flight. They were all accompanied by enhanced CNA. But

only during the first X-ray event a baylike geomagnetic disturbance was recorded at Kiruna. It is

very remarkable that even during the great peak after 02 UT no distinct disturbance can be found

on the magnetograms. According to KREMSERs findings (1964) it is very rare that a great X-ray

event, which occurs .only some hours after local midnight, is not accompanied by a baylike dis­

turbance at the same station.

The events between 05 UT and 07 UT as well as around 10 UT are heavily structured. This struc­

ture can better be seen in the E > 40 keY channel than in the E > 20 keY channel, as the counting

rates in the latter are scaled down by one more stage than in the E > 40 keY channel. This is also

the reason why the peaks in the E > 40 keY channel are sometimes greater than in the E > 20 keY

channel.

During the entire flight irregular geomagnetic pulsations. with time intervals between 20 sec and 60

sec were recorded at Kiruna [WILHELM, Institut fUr Stratospharenphysik am Max-Planck~Institut

fUr Aeronomie, Lindau/Harz, private communication 1 • The peaks are sometimes coincident with

those in the counting rates for intervals of 5 minutes and longer.

During this flight the counting rates of one of the Geiger-MUlIer-tubes, constituing the telescope,

were transmitted to the ground. Thus, one can compare the counting rates of an AI-walled Gei­

ger-MUlIer-counter with those of the scintillation counter. As expected, the less conspicuous events

are not indicated by the Geiger-MUller-counter due to its relatively low efficiency for photons.

The long lasting enhanced absorption after the burst beginning at about 05 UT resembles a special

type of events described by PFOTZER et al. (1965), and by KREMSER and BEWERSDORFF(1964)

(see also K21/64).

K 13/64

Indication: Flights K 13/64 to K 16/64 were started to cover the expected recurrence of an M-re­

gion (see comments on solar rotation 1793 ).

The abrupt increase of an X-ray burst at about 22.30 UT coincides with a rapid enhancement of the

CNA (3 db) and an as rapid starting phase of a negative geomagnetic bay disturbance ( -400 Y ).

K 14/64

Indication: s.ee K13/64

During the flight X-rays were measured nearly continuously though this period was geomagnetic­

ally rather quiet.

K 15/64

Indication: see K13/64

Weak X-ray events were recorded at the beginning and the end of the flight. It is very probable

that variations of the counting rates in the E > 83 keY and E > 500 keY channels between these

events are due to instrumental effects (see also K 2 3/64).

V. - 18 -

K16/64

Indication: see K 13/64

Balloon descended quickly after having reached the 7 mb level.

K17/64

Indication: Routine flight.

No additional radiation.

K 19/64

Indication: After some very quiet days a positive bay occurred on August 25 in the afternoon.

Only one small X-ray event was recorded.

K21/64

Indication: Flights K21/64 to K24/64 were launched to cover the expected recurrence of an

M-region (see comments on solar rotation 1794).

Several X-ray events were measured. During the three smaller peaks between about 23 UT and

24 UT the CNA was not enhanced. A remarkably persisting enhancement is observed after the

event at about 02 UT. This points probably to its relationship with a certain group of events de­

scribed by PFOTZER et a!. (1965) (see also K12/64).

Of all ~vents only that between 12 UT and 14 UT was accompanied by a (positive) bay disturbance

at Kiruna.

K23/64

Indication: see K21/64

During the total flight X-rays were observed. The greatest peak at about 03 UT coincided with an

AA-type absorption and a medium geomagnetic bay disturbance ( - 190 Y ). The other events oc­

curred during minor or no geomagnetic disturbances apart from the peak at about 17 UT. This

peak is perhaps a part of a stronger event, which began during a positive bay disturbance at Kiruna

(+200 y ). Furthermore, the highly structured burst between 08 UT and 09 UT is remarkable. The

counting rates in the E > 100 keY channel show sometimes variations a little bit more than due to

statistics, the origin of which is probably instrumental.

K24/64

Indication: see K21/64

Only one X-ray burst was registered, which was accompanied by an AA-type CNA event and a bay

disturbance ( - 400 Y ).

K26/64

Indication: Magnetic disturbances.

Balloon was squibbed at 8 mb.

K27/64

Indication: Flights K27/64 to K32/64 were launched to cover an expected recurrence of an M­

region ( see comments on solar rotation 1794).

Though the period of this flight was magnetically very quiet, some X-ray events are measured.

During the ssc at 19.55 UT no additional radiation could be recorded as the balloon had already

descended deeper than the 50 mb pressure level.

K28/64

Indication: see K 27/64

Though flights K27/64 and K28/64 were partly overlapping, additional radiation during the sse

- 19 - V.

could not be registered as the balloon was not yet high enough. The balloon was squibbed at 8 mb,

so only a part of an X-ray event is observed.

K29/64

Indication: see K27/64

Until about 17 UT only weak X-rays were measured (the sensitivity of the riometer has changed

at about 13.40 UT).

After 17 UT a greater X-ray event began, but the balloon descended and only a part of the event is

registered. As can be seen on the CNA-curve a very intense and quickly rising event occurred at

about 18.30 UT. This event is recorded by the balloon instruments of K 30/64, which was started

when K 29/64 began to descend (see K30/64).

K30/64

Indication: see K 27/64, continuation of the events recorded at the end of K 29/64.

As one can see on the riometer curve at the end of K 29 /64 a very intense electron precipitation

event had occurred at about 18.30 UT. Though K30/64 reached only the 10mb level and then descen­

ded very quickly, the radiation during the most intense peaks of this event could be registered. The

counting rates in all channels (only the E > 18 keY channel did not work) show a very quick in­

crease (the time scale is expanded) exactly at the time of a CNA increase of about 5 db and a sud­

den decrease in the X-component of the geomagnetic field of about - 500 Y • In the E > 34 keY

channel the additional counting rate amounts to about 30000/sec (625 photons/cm2 sec sterad. )

Even in the E > 500 keY channel additional radiation was measured.

When K30/64 descended K31/64 was launched, so it was possible to continue the radiation meas­

urements with a lack of only 2 hours (see K31/64).

K31/64

Indication: see K 27/64, continuation of the events recorded at the end of K 29/64 and during

K30/64.

During the ascent the last part of the great precipitation event which began at the end of K29/64

was registered. Then the geomagnetic activity diminished, but several important X-ray bursts

were recorded until about 15 UT, when the balloon began to descend.

K32/64

Indication: see K27/64

The activity of this M-region diminished and only medium X-ray bursts could be observed. Re­

markable is the event after 22 UT, which occurred during only very little enhancement of the CNA.

Medium geomagnetic disturbances were recorded at that time at Kiruna.

K33/64

Indication: Alert:" Magcalme geoalert".

No special event.

K34/64

Indication: CNA and weak magnetic disturbances in the afternoon.

The greatest event occurred between 14 UT and 16 UT,when the X-ray activity at Kiruna is usually

low.

K35/64

Indication: Recurrence of geomagnetic disturbances was expected.

Balloon descended quickly after having reached the 9 mb level.

V. - 20 -

K36/64

Indication: Magnetic micropulsations.

No special event.

K37/64

Indication: Geomagnetic disturbances were expected.

No special event.

K38/64

Indication: Alert:" Magstorm " •

This flight shows well the differences between the scintillation counter and Geiger-Milller-counter

results for events of medium intensity. During the bursts beginning at about 07.30 UT only the

first one was also detected by the Geiger-Milller-counter. Small geomagnetic disturbances were

recorded at Kiruna.

In this flight a scintillation counter and a TESIO were flown. (The TESIO worked only until the

ceiling of the balloon). Due to this combination of instruments the counting rates of a vertically

and a horizontally mounted Geiger-Milller-counter can be compared. The differences during the

ascent are small. The counting rates of the vertically mounted Geiger-Milller-counter are lower

than those of the horizontally mounted (compare K 51 / 64) .

K39/64

Indication: Micropulsation activity in the evening.

It stopped, however, soon and only very weak X-ray events occurred.

K40/64

Indication: Events following a solar flare were expected.

No special event occurred.

K41/64

Indication: Flights K41/64 were launched during the expected recurrence of an M-region (see

also comments on solar rotation 1795 ).

At the beginning of the flight a very intense X-ray burst occurred. During its decay phase great

intensity pulsations were observed in the E > 25 keY and E > 40 keY channels which can also be

found in the CNA curve.

All events occurred during a weak geomagnetic storm.

K42/64

Indication: see K41/64

Instruments worked unsatisfactorily, when the balloon had reached ceiling altitude.

K43/64

Indication: see K41/64.

After a geomagnetic ally disturbed afternoon and night, a quiet period began, when the balloon was

launched. Nevertheless, several X-ray bursts could be observed.

K44/64

Indication: see K41/64

Balloon descended after ceiling. No special events could be observed.

- 21 - V.

K45/64 (no figure).

Indication: The flights K 45 / 64 to K 53 / 64 were launched during the expected recurrence of an

M-region (see also comments on solar rotation 1795 ).

Aurora was observed, however, no X-ray events. The intensity versus pressure curve could not

be derived as the pressure unit did not work.

K46/64

Indication: see K45/64

The balloon descended very soon. Only weak X-ray events could be observed. There are no peaks

in the counting rates at about 21. 40 UT and 01.50 Ut, when the CNA suddenly increased. This is

certainly due to the low altitude of the balloon already reached at these times.

K47/64

Indication: see K45/64

The last part of an X-ray event could be observed when the balloon reached its ceiling altitude.

It descended, however, just afterwards.

K 48/64

Indication: see K45/64

The balloon levelled during great geomagnetic disturbances. One X-ray event with gredt short­

time intensity variations was observed. It was accompanied by strong additional CNA.

K49/64

Indication: see K45/64

Signals could only be received up to 16 mb. Until then no special events occurred.

K50/64

Indication: see K45/64

Balloon descended just after ceiling.

K51/64

Indication: see K45/64

One small and soft X-ray event occurred. For the combinations of instruments see K38/64.

K52/64

Indication: see K45/64

One greater X-ray event was measured with a TESCI and a TESI. The differences in the amplitude

and the time resolution can be well recognized.

The counting rates bf the telescope of the TESI are lower than those of the TESCI. This is due to

the heavier shielding of the telescope of the TESI, as this consists of two AI-walled and one Bi­

coated Geiger-Muller-counters and that of the TESCI only of three AI-walled counters. Thus, a

vertically itlCident particle must traverse 150 mg/cm2 in the telescope of the TESCI, but

360 mg/ cm 2 in the telescope of the TESI (see Table 1, p. 6).

K53/64

Indication: see K45/64

During the whole flight X-r-ays could be detected. At about 09 UT even the E > 440 keY channel

showed additional radiation.

- 22 -

Summ<try

From July to October 1964, 53 balloon-flights were carried out at Kiruna to measure radiation

associated with auroral zone disturbances. Different kinds of detectors were employed. Here the rough

flight data are presented, which contain a great number of X-ray bursts. Some outstanding events are

commented.

Acknowledgement

The French and German groups are deeply indebted to the ROYAL SWEDISH ACADEMY OF

SCIENCE and its permanent secretary Prof. Dr. E. RUDBERG for permission to carry out the balloon

launchings at the Kiruna Geophysical Observatory. They express their gratitude to the director of the ob­

servatory, Dr. B. HULTQVIST, and all colleagues and members of the observatory staff for their cordial

and friendly cooperation.

All the authors appreciate the helpful effortE! of the scientific and technical staff members of the

cooperating institutions involved in the preparations of the instruments and the organisation of the cam­

paign, and for the participation in the field operations.

We want to nominate especially the contributions of Dr. L. ROSSBERG by supervising the develop­

ment of the TESCIs, as well as of Mr. G. SPITZ, by manufacturing and testing these instruments. The

following technicians participated in the field operations:

Mr. Flentje, Mr. Fischer, Mr. Frank, Mr. Spitz (Lindau group)

Mr. Broendel, Mr. Jouan, Mr. Pagnier, Mr. Palous (Meudon group) •

The research reported in this document has been sponsored in part:

through the Lindau group (Institut fUr Stratospharenphysik am Max-Planck-Institut fUr Aeronomie), by the

Bundesministerium fUr wissenschaftliche Forschung der Bundesrepublik Deutschland, by the Max-Planck­

Gesellschaft granted mainly by the Deutsche Landergemeinschaft and the Bundesrepublik Deutschland,

through the Kiruna group (Kiruna Geophysical Observatory, Director Dr. B. HULTQVIST), by the Air

Force Cambridge Research Laboratories under Contract AF 61 (052 )-604, through the European Office

of Aerospace Research (OAR), United States Air Force,

through the Meudon group (Laboratoire de Physique Cosmique, Director Prof. Dr. A. FREON) by the

Centre National d'Etudes Spatiales (CNES), France.

The factory Albin SPRENGElR KG., St-Andreasberg, took over the manufacturing of the balloon

equipments in series and we owe thanks to its representatives Dr. Chr. BACHEM and Mr. W. ULLRICH

for their cordial response to all our requirements.

BARTELS,J.

ERBE, H.

KEPPLER, E.

KREMSER,G.

- 23 -

References

Terrestrial Magnetic Activity and its Relations to Solar Phenomena

Terr. Magn. Electr • .:!2., 1-52 (1932).

Auswirkung der Variationen der primaren kosmischen Strahlung auf die Mesonen-und

Nukleonenkomponente am Erdboden

Mitteilung a. d. Max-Planck-Institut fUr Aeronomie, Nr. 2, Springer-Verlag, Berlin,

Heidelberg, New-York, (1959)

Description and Instruction Manual for the Sonde SPARMO 64

SPARMO Bulletin, ~r. 3, October 1964.

tiber den Zusammenhang zwischen Rontgenstrahlungs-Ausbruchen in der Polarlicht­

zone und bayartigen erdmagnetischen Storungen

Mitteilung a. d. Max-Planck-Institut fUr Aeronomie, Nr.14, Springer-Verlag, Berlin,

Heidelberg, New- York ( 1964).

KREMSER, G. und BEWERSDORFF, A. :

tiber eine besondere Art von Rontgenstrahlungs-Ausbruchen in der Polarlichtzone

Kleinheubacher Berichte 1964.

PFOTZER, G., EHMERT, A., ERBE, H., KEPPLER, E., HULTQVIST, B., and ORTNER, J.

A Contribution to the Morphology of X-ray Bursts in the Auroral Zone

J.Geophys. Res.~, 575-585, (1962a).

PFOTZER, G., EHMERT, A., and KEPPLER, E. :

Time Pattern of Ionizing Radiation in Balloon Altitudes in High Latitudes

Mitteilung a. d. Max-Planck-Institut fUr Aeronomie, Nr.9, Springer-Verlag, Berlin,

Heidelberg, New-York (1962b).

PFOTZER, G., EHMERT, A., BEWERSDORFF, A., KREMSER, G., ROSSBERG, L., RIEDLER, W.,

TREFALL, H., LEGRAND, J.P. :

Measurements of High Energetic Auroral Radiations with Balloon-Borne Detectors

in 1962 and 1963.

Mitteilung a. d. Max-Planck-Institut fUr Aeronomie, Nr.18, Springer-Verlag, Berlin,

Heidelberg, New-York (1965).

ROSSBERG, L. and SPITZ, G. :

Eine Ballonsonde zur Messung des Energiespektrums von Rontgenstrahlungs-Schauern

und zum Nachweis geladener Teilchen (to be published).

VI. Diagrams of the flights

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Verzeichnis der MiHeilungen aus dem Max-Planck-Institut

fur Physik der Stratosphare

Nr. 1/1953 lJber den Beitrag der von I-l - Mesonen angestoBenen Elektronen zu

den Ultrastrahlungsschauern unter Blei. G. Pfofzer

Nr. 2/1954 Ein Zahlrohrkoinzidenzgerat zur Registrierung der kosmischen Ultra­

strahlung. A. Ehmert

Eine einfache Me ,ode zur Einstellung und Fixierung des Expansions­

verhaltnisses von ~ebelkammern. G. Pfotzer

Nr. 3/1954 Optische Interferen7en an dunnen, bei -1900C kondensierten Eisschichten.

Erich Regener (vergriffen)

Nr. 4/1955 lJber die Messung der T emperatur des atmospharischen Ozons mit Hilfe

der Huggins-Banden. H. Zsch6rner und H. K. Paetzold

Nr. 5/1956 Ein neuer Ausbruch solarer Ultrastrahlung am 23. Februar 1956. A. Ehmert

und G. Pfotzer, vergriffen (erschienen Z. Naturforschung 11a, 322, 1956)

Nr. 6/1956 Das Abklingen der solaren Ultrastrahlung beim Ausbruch am 23. Februar

1956 und die geomagnetischen Einfallsbedingungen. A. Ehmert und

G. Pfotzer

Nr. 7/1956 Die Impulsverteilung der solaren Ultrastrahlung in der Abklingphase des

Strahlungseinbruches am 23. Februar 1956. G. Pfotzer

Nr. 8/1956 Die atmospharischen St6rungen und ihre Anwendung zur Untersuchung

der unteren lonosphare. K. Revellio

Nr. 9/1956 Solare Ultrastrahlung als Sonde fur das Magnetfeld der Erde in groBer

Entfernung. G. Pfotzer

*

Die vorstehenden Hefte k6nnen beim Max-Planck-Institut fur Aeronomie,

3411 Lindau angefordert werden.

Mitteilungen aus dem Max-Planck-Institut fur Aeronomie

Nr. (5) Waibel: Messungen von Primarteilchen der kosmischen Strahlung.

Nr. 2 (5) Erbe: Auswirkung der Variationen der primaren kosmischen Strahlung

auf die Mesonen- und Nukleonenkomponente am Erdboden.

Nr. 3 (I) Kohl: Bewegung der F-Schichl der lonosphare bei erdmagnelischen

Bai -Slorungen.

Nr. 4 (I) Becker: Tables of ordinary and extraordinary refractive indices, group

refractive indices and h'o,x(f)- curves or standard ionospheric

layer models.

Nr. 5 (5) Schropl: Ober eine Neubestimmung des Absorptionskoeffizienten von

Ozon im Ultraviolett bei kleinen Konzentralionen.

Nr. 6 (5) Erbe: Ergebnisse der Ballonaufstiege zur Messung der kosmischen

Slrahlung in Weissenau und lindau.

Nr. 7 (5) Meyer: Elektromagnelische Induktion eines vertikalen magnetischen

Dipols Gber einem leitenden homogenen Halbraum.

Nr. 8 (I u. 5) Dieminger und Mitarb.: Die geophysikalischen Ereignisse des

12. - 14. November 1960.

Nr. 9 (5) Pfotzer, Ehmert, and Keppler: Time Pattern of Ionizing Radiation

in Balloon Altitudes in High Latitudes.

Part A, Text; Part B, Figures and Diagrams.

Nr. 10 (5) Waibel: Eine Ballonsonde zur Messung von Rontgenstrahlung und

solarer Ultrastrahlung.

Nr. 11 (5) Voelker: Zur Breitenabhangigkeit erdmagnetischer Pulsationen.

Nr. 12 (5) Jaeschke: Registrierung von Pulsationen im sGdlichen Niedersachsen als

Beitrag zur erdmagnetischen Tiefensondierung.

Nr. 13 (5) Meyer: Elektromagnetische Induktion in einem leitenden homogenen

Zylinder durch auBere magnetische und elektrische Wechsel­

felder.

Nr. 14 (5) Kremser: Ober den Zusammenhang zwischen Rontgenstrahlungs-Aus-

brGchen in der Polarlichtzone und bayartigen erdmagnetischen

Storungen.

Nr. 15 (5) Keppler: Messung von Rontgenstrahlung und solaren Protonen mit

Ballongeraten in der Nordlichtzone.

Nr. 16 (5) Kirsch: Die Anisotropien der kosmischen Strahlung.

Nr. 17 (5) Guilino: Ausbau eines Wechsellichtmonochromators und seine Anwen­

dung zur Messung des Luftleuchtens wahrend der Dammerung

und in der Nacht.

Nr. 18 (5) Pfotzer and Ehmert: Measurements of High Energetic Auroral

Radiations with Balloon - Borne Detectors in 1962 and 1963

Part A to C, Text; Part D, Figures and Diagrams.

Nr. 19 (I) Hartmann: Bestimmung wichtiger Satellitenpositionen mit Hilfe graphischer

Darstellungen.

Nr. 20 (5) Keppler: Ober die Eigenschaften von Zahlrohren und lonisationskammern

in verschiedenartigen Strahlungsfeldern. - Zur Interpretation von

R6ntgenstrahlungsmessungen in Ballonh6he in der Nordlicht­

zone.

Nr. 21 (5) Siebert: Zur Theorie erdmagnetischer Pulsationen mit breitenabhangi­

gen Period en.

Nr. 22 (5) Meyer: Zur 27 taglichen Wiederholungsneigung der erdmagnetischeri

Aktivitat, erschlossen aus den taglichen Charakterzahlen C 8 von 1884-1964

Nr. 23 (5) Frisius: Ober die Bestimmung von Langstwellen - Ausbreitungsparame­

tern aus Feldsfarkemessungen am Erdboden.

Nr. 24 (I) Ma: EinfluB der erdmagnetischen Unruhe auf den brauchbaren Fre­

quenzbereich im Kurzwellen-Weitverkehr am Rande der Nord­

lichtzone.