analysis of cap ~i rf - nasa

8 I 8 1 8 8 ~I 8 ,I I 1 8 8 I I 8 8 1 1

ANALYSIS OF POLAR CAP ABSORPTION EXZXTS 11. TIME RELATION OF M O R FLARES

AND RF EMISSIONS CENT-

By .IR Fred C. Jonah

LTV Astronautics Division

Report No. 00.802 ---HQasws6

LTV ASTRONAUTICS DMSION LTV AEROSPACE CORPORATION

F i r st Quarterly Report Prepared Under Contract NAS 9-4911

Supplemental Agreement 1 with National Aeronautics & Space Administration

Manned Spacecraft Center

1.0

1.1

1.2

1.3

1.4

1.5

2.0

2.1

2.2

2.3

2.4

3.0

3.1

3.2

3.3

4.0

4.1

4.2

RESULTS AND ccNcLus1oNs

Flares and RE' Peak M s s i o n s

Flares and Sunspot Areas on Flare Day

Flares and Sunspot Magnetic Class on Flare Day

Percentage of the Flares i n Each Classification

CLASSIFICATIm OF lElpoRTANcE 3 AND 3+ FLARES

All Flares of Importance 3 and 3+

Importance 3 and 3+ Fla res Followed by a PCA Event

Importance 3 and 3+ F l a r e s 'Followed by Very small PCA Events

Importance 3 and 3+ Flares Not Followed by a Known PCA Event

Flares Followed by Important PCA Events

Flares Followed by Very Smal l PCA Events

Flares of Importance 3 and 3+ Not Followed by PCA Events

Probability that an Importance 3 or 3+ Flare W i l l or Will not be Folluwed by a PCA Event

SUNSPOT GROUP AREA AND MAGNETIC CLASSIFICATION ONFWDAY

Sunspot Area on Flare Day

Sunspot Group Magnetic Classification on Flare Day

SOURCES

APPENDIX A i

Page 1

5

10

12

13

13

16

19

30

8

1

1.1

1.2

1.3

1.4

1.5

1.6

1.7

2

2.1

2.2

2.3

3

3.1

Master L i s t of All Importance 3 and 3+ Flsres 1%4=1963

Number of Importance 3 and 3+ Flares and Associated PCA Events

Page

21

6

Classification of a l l Importance 3 and 3+ Flares i n Terms of the Algebraic Sign of A t 12

Distribution of Sunspot Areas for a l l Importance 3 and 3+ FLarres and Those Followed by a PCA Event 13

Distribution by Years of Importance 3 and 3+ Flares w i t h the Area of the Sunspot G r o u p on Flare Day 14

Distribution of Importance 3 and 3+ Flares Followed by a PCA Event with the Area of the Sunspot Group on Flare Day 15

Distribution of Importance 3 and 3+ Flares with Sunspot Magnetic Classification an Flare Day 17

Distribution of Irrrportance 3 and 3+ Flares Followed by an Important PCA Event with Sunspot Magnetic Class 18

Importance 3 and 3+ F l a r e s Followed by Important PCA Events

23

Relation Between the Intensity of the PCA Events and t h e Algebraic Sign of A t 7

Relation Between the Peak Intensity of the RF Flux and the S i g n of A t 8

Relation Between the Intensity of the PCA Events and Peak Intensity of RF Emissions 9

Importance 3 and 3+ Fla.res with Reported S m a l l PCA Events

25

A t for Flares Followed by SnaU PCA Events 10

ii

I I 8 1 1

4

4.1

A-1

A-2

A-3

A-4

Page

Importance 3 and 3+ Flares with No Known 26 Associated PCA Event

Rela.tim Between the Intensity of the Rp Flux and bt u. Master L i s t of PCA Events with Associated Flazes and Sources

31

Sources Used for Polar Cap Absorption Data 33

S m a l l PCA's Reported by Two or More & m n d e n t - 14 Observers

PCA's During 1960 Reported by Gregory Only 35

iii

I c

R e p o r t No. 00.802 Page No. 1

1.0 RESULTS AND CONCLUSICNS

This sttlay has Seen devoted t o the analysis of 142 flares

tha t w e r e observed during the years 1954 thraugh 1963, and assigned an

importance of 3 or 3+ in the McMath-Hulbert Working L i s t .

studied the relationship of these flares t o all known radio frequency

emissions at 1500, 2000, 2800, 2980, 3000, and 3750 Mc/s, that occurred

at the time of the flare.

sunspot groups on flare &y, and the age of the associated plage region

i n solar rotations have been considered.

1.1

W e have +

The area and magnetic classification of the

TIME RELATION OF FLARES AND RF' EMISSIONS

We find that fo r flaxes followed by an important PCA event

the time of RF peak intensi ty coincided with or followed the time of

the f lare maximum intensity ( A t ? 0) i n 76.5% of the cases; while

A t < 0 fo r 92$ of the flares not followed by a PCA event.

1.2 FLARES AND RF' PEAK EMISSION

The FP peak intensity exceeded 500 x w (rn2c/s)-l for

87'$ of the flares that were followed by a PCA event while the f lux was

less than 500 x W (xn'c/s)-' for 7% of the flares not followed by

a PCA event (including cases where the flare occurred during the nonnal

observing time of at least one observatory and no flux was reported).

1.3 FUIRES AND SuNspoT AREAS CX? FLARE DAY

O f the major flares during 1954 through 1959, 71.s

occurred i n sunspot groups that on flare day had an area 3 500 millionths

8 Report No. 00.802 Page No. 2

of the solar hemisphere while

PCA event had areas greater than 500 millionths.

of the flares that were followed by a

1.4 FWSES AM, SUNSPOT M4-c CLASS (E? Fww3 DAY The magnetic classification of the associated sunspot group

is not known on flare! day f o r 21 spot groups.

occurred at ei ther the east or west limb of the sun.

cent of the f l a r e s tha t occurred on days when the sunspot magnetic classi-

f icat ion was known were classified as e i ther 'f or /3&' . Only 3 6 of the

8 orFr sunspots were followed by a PCA event. On the other hand, the

flare-day magnetic classification is known fo r 32 of the PCA-flares and

69$ occurred in ei ther t 'o rpd ' spots.

1.5 PERCENTAGE OF T€E F'LARES IN EACH CLASSIFICATION

Ten of these flares

Forty-seven per

The results of t h i s analysis may be expressed as follows:

7~ of all cases wherebt 6 0 were followed by a PCA

9@ of all cases whereht 5 0 were not followed by a

E A event

76.5% of the PCA f la re at2 0

929% of non PCA f lares at t o

8 6 of PCA f l a r e s the RF peak > 500 x looE W(m2c/s)-l

769 of non PCA f la res , the RF peak < 500 x 10'22W(m2c/s)-1

729% of t h e flare-sunspots had an area a 500 millionths of

the solar hemisphere on flare day

92$ of the PCA f la re sunspots had an area >, 500 millionths

of the solar hemisphere on f l a r e day

I I U I I 1 I I I I t I I 1 I

Report No. 00.802 Page No. 3

47$ of the flare sunspots had a or ,4'# classification

~n flare day

6 6 of the PCA flare sunspots had a r or f I y classification

on f W e thy

N m :

during a meeting of the Joint MSC-GSFC Working Group on Space Radiation.

Dr. Prince suggested that the time difference between the maximum of the

lU? emissions and the optical H-alpha maximum should be investigated.

This study was based on a suggestion by Dr. Helen Dodson-Prince

1 I I I I I I 1 1 I I 1 I t I 1 I I

Report No. 00,802 Page No. 4

2.0 CIASSIFICATIm OF IMPORTANCE 3 AND 3+ mAREs

The 142 flases with Lmpurtw-ce 3 or 3+ i n the MWth-Hulbert

working l ist of flares (Table 1 ) were placed i n three groups:

(1)

(2)

Flares followed by an important PCA event (Table 2).

Flares followed by a s m a l l or very small PCA event

(Table 3).

(3) Flares not followed by a known FCA event (Table 4).

ALL FLARES OF IMPORTANCE 3 AND 3+

Table 1 lists all flares of importance 3 or 3+ that occurred

2.1

during the years 1954 through 1963.

We have included the McMath Plage Number and plage age i n

rotations, the M t . Wilson sunspot number, the M t . Wilson magnetic classi-

f ication, the sunspot area based on the Royal Greenwich Observatory

photoheliographic results, and the Zurich classification are given for

flare day when the values are available.

2.2 IMPORTANCE 3 AM) 3+ FLARES FOLLOWED BY A PCA EVENT

Table 2 lists al l f lares of importance 3 or 3+ tha t were

This table in- followed by an important PCA event (from Table A-1).

cludes the flare, PCA, and shortwave fade data. It also includes a l l

known spectral emissions of Type II and Ill associated with the flare,

and single frequency data for frequencies 1500, 2000, 2800, 2980, 3000,

and 3750 Mc/s.

above lo$ of the peak flux in units of

We have also included the value of the RF burst energy

joules (m2c/s)” for 2800

and 375 Mc/s when a value is given i n the NAS

R e p o r t No. 00,802 Page No. 5

Program Apollo working

paper No. 1193 (January 28, 1w). is the time of the RJ? burst peakminus the t ime of flare maximum intensity.

2.3

The time difference i n minutes A t

3 " C E 3 AXD 3+ FIARES FOIUMED BY VERY SMALL PCA EVENTS

Table 3 lists the reported small PCA events that were not

included in Table 2 and those that were derived by Gregory based on the

use of high sensi t ivi ty ver t ica l incidence back sca t te r sounding of

the lower ionosphere at a frequency of 2.3 Mc/s.

2.4 IMPORTANCE 3 AND 3+ FLARES NOT Fy)LLcTwED BY A KNOWN PCA EVENT

Finally Table 4 l ists all importance 3 and 3+ flares that were

This table gives a l l of the reported not followed by a known PCA event.

radio emissions i n the frequency range f r a n 1500 t o 3750 Mc/s range as

we= as short wave radio fadeouts and reported spectral emssions of Type I1

and Type I V .

The number of importance 3 and 3+ flares for each year and

the number followed by PCA events is sunmaxized i n Table 1.1.

that approximately 2* of the flares were followed by a PCA event i f the

E A ' S reported by Gregory only are not included.

This shows

For the purpose of uur analysis of the difference (A t )

between the time of RF emission peak flux and the time of the flares

maximum intensi ty we have grouped the sma l l PCA events w i t h the flares

not followed by PCA's.

i 8 I I 8 U I I E t C I I I t 1 I t I

TOTAL

No. of Flares

CmP. 3, 3 + 4

21

32

20

32

19

10

2

2

142


PCA With S m a l l Gregory PCA PCA

0 0

2 0

ll 1

6 0

6 1

7 1 7

5 0

0 0

1 0

38 3 7

TABLE 1.1 Number of Importance 3 and 3+ Flares and Associated PCA Events

I 1 8 I 1 1

3.0


RELATIONSHIP OF FLARE MAXIMUM INTENSITY AND PEAK RADIO FLUX I"sm

3.1 FLARES FoJamED BY m m m PCA EMOTS

This list contains 38 PCA events, that w i t h one exception,

are included in one or more of the catalogues by Bailey, Modisette,

Malitson, and Warwick and Haurwitz (Table A-2). Four of the events

(Numbers 12, 17, 18, and 55, Table A-2, Flares Numbers 43, 47, 49,

and 156, Table 1) were reported with a weak absorption and the i r in-

clusion i n Table 2 rather than Table 3 is quite arbi t rary.

A l l of the flares in t h i s group were followed by a short

wave radio fadeout and radio emissicms at one or more of the frequencies

between 1500 and 3750 Mc/s.

the f l a r e and the RF' emission are reported f o r 34 of the events.

The time of the maximum in tens i ty of both

The time of the RF' maximum occurred simultaneiously wi th

or a f t e r the f l a r e maximum ( A t 5 0 , where 3t = time of RF maximum

minus the time of the flare maximum) fo r 26 of the events (76.58)

(Table 2.1). The eight cases where A t < 0 w i l l be discussed in de ta i l

l a t e r when other factors w i l l be considered.

I 1 I 1 Unknown Positive Zero Ne gat ive T o t a l I

6 t o f 10

0 6 2 2 3 6 0 3

0 2 0 1

10 I 2

3

TABLE 2.1 Relation Between the Intensity of the PCA Events and the Algebraic Sign of A t

I Report No. 00.802 Page NO. 8

This table does not indicate any good correlation between

the i n t e ~ s i t y of the PCA as,d algebraic si@ of t.

On the other hand Table 2.2 shows that the peak Rp flux

exceeds 500 x W(m2c/s)'' for of the PCA flares, and the A t 3 0

TOTAL

Jnknawn Positive Zero Ne gat i ve

1 0 0 1

1 1 0 1

0 4 1 2

1 13 1 3

1 5 1 1

4 23 3 8 -

TABU 2.2 Relation Between the Peak Intensity of the RJ? Flux and the Sign of At

Total

2

3

7

18

a

38

I

! @

rbs.db. x 5 3

>3 t o 6 6

> 6 t o 5 10

? 10

I

Report no. 00,802 Page No. 9

~ 2 5 0 t o >500 t o 310oO t o $250 < 500 5 1000 r' 5Ooo ,5000

1 2 3 4 0

1 1 3 7 0

0 0 0 3 0

0 0 1 4 0

2 3 7 18 0 I mAL

T a t d

10

12

-

3

13

TABLE 2.3 Relation Between the Intensity of the PCA Events and Peak Intensity of RF Emissions

Table 2.3 does not indicate any good correlation between the

intensi ty of the PCA absorpticm and the peak flux of the RF emission.

3.2 FLARES FOLLOWED BY VERY SMALL PCA EVEXITS

We have ten events i n this group of snaU or very small PCA

events including seven events derived by Gregory based on the use of high

sens i t iv i ty ver t ical incidence back sca t te r sounding of the lower ionosphere

at a frequency of 2.3 Mc/s.

The times of both f lare maxll~l * um and RFpeak flux at one or

m c r e of the f'requencies i n t h e range from 1500 t o 3750 Mc/s are known

f o r nine of the events.

RF maximum follows the flare maximum (At 2 0) while major RF bursts were

reported (flux 2500 x

At was negative.

I n th i s case w e f ind only two events where the

W n ~ - ~ ( c / s ) - ~ ) for three of the cases where

'I t 8 I


I Unknown Positive Zero Negative \Qt I Flux

t Total

1 , 5 0 0

>, 500 t o < ~ O O o

> lo00 0

T(TrAL

TABU 3.1 & t fo r Flares Followed by Small PCA Events

1 0 0 4 5

0 1 0 2 3

0 1 0 1 2

1 2 0 7 10

Because of the probable very low absorption during these

events we w i l l combine these flares with those not followed by PCA

events . 3.3 FLARES OF IMPORTANCE 3 AND 3+ NOT F0IJX)WED BY PCA EvENlls

Thirty-eight of the flares of importance 3 or 3+ were followed

by important PCA events and ten more have been assoicated with very

small events. I n addition three of the PCA events occurred within three

hours of the associated PCA f l a re and may have contributed t o the in-

tens i ty of the PCA event (flares s, 100, and 137) although i n two

cases (95 and loo), the start of t h e flare followed the reported start

time of t h e PCA.

not followed by a known PCA event (Table 4).

This leaves 91 importance 3 and 3+ fWes that were

We find that eleven f la res occurred during the normal ob-

serving times of two or more RF frequencies and eight during the normal

observing t h e of at least one RF' frequency w i t h no increase i n flux

reported .

I

Report 00.802 Fkge No. ll

t

I t I 1 I I I t 1 8 8 I

There was no known RF observations at the times of f ive

flares (ambers 7, 11, 26, 28, md 32).

The times of flare maximum and/or RF peak intensity is not

reported fo r 13 flares. The values of A t for the 54 flares fo r which

the times of flare maximum and RF peak intensity is negative f o r 49 of

the flares. If w e assume that a t l ea s t one observatory was observing

at the time of the II f la res that occurred dur ing the observing times

of two or more frequencies, we have 60 (and possible 68) cases where

A t was negative or no RF flux w a s emitted as shown in Table 4.1.

see that fo r the importance 3 and 3+ fWes tha t were not followed by

a PCA event there was probably no R F emissiagl from eleven (and possibly

l9) , and the RF emission was less than 500 x loo2* W (m*c/s)'l for 47

We

of the f lares .

lo known zn obs.

?o flux :eported

> 500 t o 4 lo00

No Flux Unlslown Positive Zero Negative

5

19

10 4 1 32

2 0 0 5

1 0 0 I 2

!WAL I 19 18 4 1 49

Total

5

19

47

7

13

91

TABLE 4.1 Relation Between the Intensity of the RF Flux and b t


Others * Three of d e PCA events may have been influenced by two major f la res , 4 64 ll, 0 3 29 c 23

7%- 90$ b!AL 1 ACCURACY ,PRowuITy

We also f ind thatetwas negative (the time of the RF f l u

maximum preceded the time of f lare maximum) in 92$ of the cases where

the times of both maxima were knawn,

The fwr cases (Flares 34, 48, 54, 48) where At > 0 and the

one case of d t = 0 riii be &ned in Getail later.

If we include the nine cases where (Table 3 and 3.1) very

smaJ.l or doubtful PCA events were reported with the 65 cases f’rm

Table 4 and 4.1, we find that i n 9U$ of the cases the time of RE’ emis-

sion peak precedes the time of flare maximum.

3.4 PROBABILITY !I!HAT AN IMPORTAMX 3 OR 3+ FLARE WILL CB WILL NOT BE FOU(MED BY A P C A EVENT

Table 1.2 shows that if we include all cases where A t 3 0,

Similarly, the

when A t < 0, o r no flux is reported when the flare occurs during the

normal operating time of two or more frequencies (ll flares), the flare

w a s not followed by a PCA event in 90$ of the cases.

f l a r e w a s followed by a PCA event i n 7s of the cases.

Non-PCA Flaxes

Important PCA

Total Number

91

10

38

No Flux Unknown Positive Zero Negative Reported

18 4 1 49 1 1 8

1 2 0 7 0

4 23 3 8 0

Report 00.802 F%ge No, 13

unknm EL, WL sunspot 500 t o 1000 t o 1500 t o or Not Area < 5 0 0 (lo00 (1500 42000 a2000 Observed

I

4.0

4.1

SUNSPOT GROUP AREA AND MAGXEZIC CLASSIE'ICATION ON FLARE DAY

SUNSPm AREA ON FLARE DAY

FFZS

The 142 flares of importance 3 or 3+ were observed i n 101

30 33 22 14 5 5

2 12 7 3 1 0

different sunspot groups. O f the lOg flares reported during 1 9 5

area equal t o or greater than 500 millionths of the solar hemisphere.

The distribution wi th sunspot mea is shown i n Table 1.3.

Twenty-three of the 25 major flares that were followed by

a PCA event occurred i n a sunspot w i t h an mea greater than 500 millionths.

TABJX 1 .3 Distribution of Sunspot Areas for A l l Enportance 3 and 3+ Flares

and Those Followed by a PCA Event

During t h i s period 23 of the sunspot groups were the source

of two or more major flares. In eleven cases at least one of the f h e s

w a s followed by a PCA event.

We have limited the correlation of flares t o sunspot mea

t o the period through 1959 f o r which w e have Greenwich Observatory d a i l y

sunspot area data.

MYI'AL

FCA

500 t o lo00 t o 1500 t o c 500 41OoO (1500 42000 a2000

0 3 1 0 0

6 5 4 5 0

Il* 10 4 2 3

4 9 3 4 0

9 6 10 3 2

2 1 1 1 0

1 0 1 0 0

0 1 0 0 0

33" 35 24 15 5

3 14 a 4 1


unknown

0

1

2

0

2

3 2

1

* One flare (No. 57, Table 1) occurred in a region with no known sunspot groups .

* Flare day sunspot area dah not available for 1960.

Flare day sunspot area data after July I, 1961, taken from U. S. N a v a l Observatory daily reports.

TABLE 1.4 Distribution by Years of Importance 3 and 3+ Flares

with the Area of the Sunspot G r o u p on Flare Day

If w e use the U. S. Naval Observatory area data fo r the

years 1961 through 1963, we f ind that 79 of the 112 flares (appraximately

Report No. 00.802 Page Bo. 15

71$) for which the sunspot area is known on flare df~y have an area a 500

millionths of the solar hemisphere. The distribution of the importance

3 and 3+ flares that were followed by a PCA event is given in Table 1.5.

500 t o lo00 t o 1500 t o < 500 <lo00 41500 42000 32000

No PCA Events

0 2 0 0 0

2 6 1 1 1

0 3 1 2 0

0 1 4 1 0

1 1

No PCA Events

0 1

1 1 0

0 0 0

3 14 7 5 1

* Daily sunspot areas not available.

* Flare day sunspot area data af'ter July 1, 1961, is taken from US. N a v a l Observatory daily reports.

!l%BIZ 1.5 Distribution of Importance 3 and 3+ Flares Followed by a PCA Event

w i t h the Area of the Sunspot Group on Flare -Day

I .

Report N o . 00.802 Page N o . 16

4.2 SUNSPOT GROUP MAGNE2IC CLASSIFICATION ON FLARe DAY

The magnetic classification on flare day of the sunspot groups

associated with the importance 3 and 3+ flares is known for 121 of the 142

flares as shown i n Table 1.6.

Twenty-seven of the 30 PCA flare sunspot groups for which an

area on flare day is known had an area greater than 500 millionths of

the solar hemisphere.

sunspot area are known for 27 o f t h e PCA flares.

an area greater than 500 millionths and a 75 o r f l u magnetic classificaticn.

Both the sunspot magnetic classification and the

Nineteen of these had

Both the flare day magnetic classification and area are

known for 93 of t h e importance 3 and 3+ flares.

had a

millionths.

large and magnetically complex sunspot groups were followed by PCA events.

Forty-three of these

or /Sfmagnetic classification and an mea greater than 500

Only 4.4 per cent of the importance 3 and 3+ flares from 1

.

1

5

2

1

11

5

0

0

0

0

2

ll

4

7

3

3

1

1

3

10

6

14

8

4

3

1

1

0

2

3

1

1

5

2

0

0

25 32 50 14


UnlmaWn WL EL Not Rep

0

2

2

0

0

1

2

0

0

0 0

0 0

1 7*

0 0

2 3

0 1

0 0

0 0

0 0

7 3 11

* One flare (No. 57, Table 1) occurred in a region with no known sunspot group.

TABLE 1.6 Distribution of Importance 3 and 3+ Flares with Sunspot Magnetic Classification on Flare Day

t

8 I I I

TOTAL

m, All Major Flares Percent with PCA S m a l l PCA

1

2

0

4

2

0

None

0

none

0

5

2

1

1

3

1 0 0

9 13 8 2

25 32 50 14

36 41 16 14

2 3 2 2 - JTable 3) .

i l l 16 10 4 A l l PCA


Not WL EL Reported

0

0

0

0

0

0

0 0 0

2 0 3

7 3 11

28 0 27

0 0 1

2 0 4

TABLF, 1.7 Distribution of Importance 3 and 3+ Flares

Followed by an Important PCA Event with Sunspot Magnetic Class

The sunspot magnetic classification on fhre day is knuwn

for 121 of the importance 3 and 3+ flares.

ated with sunspots that on flare day had a 4 or f l l f magnetic classification.

Only 22 (39$) were followed by a PCA event.

Fifty-seven (47$) were associ-

8 1 1 I 8 1 1:

8 8 I 8 1 1 t 1 I 8 I


SOURCES

-. 1 Catdwies of Polar Cag Absorption Events

Bailey, D. K., "Polar Cap Absorption," Planet. Space Sci,, E ( 5 ) (1964) 9 495-541

( 1 w i t s o n , H a r r i e t m., "Tabie of Solar h-oton Events, i n - Solar Proton Manual, Ed. Frank B. McDonald, NASA TR-R-169 {Dee. l963), 109-117.

Modisette, J. L., T. M. Vinson, and A. C. Hardy, Model Solar Proton Environment for Manned Spacecraft Design, NASA, TND-2746, April 1965.

Warwick, C. S., and M, W. Haurwitz, "A Study of Solar Activity Associated with Polar-Cap Absorption," J. Geaphys. Res., 67(4) (1962) 9 1317-1332s

Other sources l i s t e d i n Table A-2, page 33.

2. Daily sunspot areas fo r the years 1954 through 1959 were obtained from the Royal Greenwich Observatory Bulletins - Photoheliographic Results

1955 - Published in 1958 1956 - Bulletin No. 14 1957 - Bulletin No. 26 1958 - Bulletin No. 60 1959 - Bulletin N o , 103

3. Solar Flare Data

Dodson, Helen W., and E. Ruth Hedeman, McMath Hulbert Observatory, Working L i s t of Flares.

IGY Flares, Solar Activity Report Series 12 (June 25, 1960) 1959 Flares, Solar Activity Report Se r i e sy5 (June 26, 1961) 1960 Flares, Solar Activity Report Series i8 (May 17, 1962) 1961 Flares, Solar Activity Report Series 21 (March 15, 1963) 1962 Flares, Solar Activity Report Series 5 - (April 1, 1964) Polax Cap and Related Data 4.

Jonah, F. C., Analysis of Polar Cap Absorption Events. I Effects of Solar and Solar Induced Conditions Prior t o the PCA Event, LTV Astronautics Division Report No. 00.740, 17 December 165 .

Report No. oO.802 Page No. 20

Jonah, F. C., Helen Dodson-Prince, and E. Ruth Hedeman, Solar Activity Catalogue for the 19th Solar Cycle, in 5 Volumes,

1 1954-1956, LTV Report 00.594 2 Year 2957, LTV Report 00.538 3 Year 1958, L W Report 00.503 4 Year 199, LTV Report 00.650 5 Years i960-l963, LTV Report 00.654

R e p o r t Iio. 00.802 Page No. 21

r c

R e p o r t No. 00,802 Page No. 22

-. r S F . .

1 I I - I 8 I 1

a

R e p o r t 100. 00.8Oe Page No. 23

II I I I I I I I I I I I I I I I I I I


1 Report No. 00.8@ Page No. 25

I I I 1 il I 8 I I 1 1 I I 1 I I I I

N N N m N N m N + .-.

D N f ' R e t w L3 8 2 n *

N

f F: i? 6 8 : 2 N 4 4 3

8 X

m m I c L L c I E L

9-05 lh5 22

9-lb 0813 5b

10-01 0756 bo

.l%W lloD 62

12-6 lbo3 9

12-17 m

12-zz Eqs5 63

4-11 1- R 1(pz I* R6 6 h

Report No. 00.802 Page NO. 26

1.

3

3

3

2

2

3

3

2

3

3

3

Lxllo l lo 1

l a I 3

Imr 79 3

1937 163 E

. .

5 9 61-

15W moo 1W

1W

9m cn CUI -3.5 5.0 m m OM6 -7 6.0 363 3?% W 0 3 0 --_- 2.3 (9)

ZBm BD 1336 1339.5 6.0 Ur i* 95.0 10

1 ~ 5 100.0 50 ZBX, SD 1538.5 15b5.5 l6.5 (335)

15m

jm, 3750

jm, m * * 3 5 > M . O w 1 3m

Report No. 00.8W Page No. 27

ZD

u 7

195

37

3"l

125

3

10

1-

3 5

(lU71

M 10313

10850s

Ip)

12

Iu

15m m 0857 09* 61.0 (251) rpes m a 5 9 kv.0 4 jmo m ' 6 . 5 aa6.5 m9.0 -- xn: 3 w 3750

+ I 8

*17

a 4 a

-7.6 .4 A e . 3

15.m en wll Wlb 21.0 2Ei * SD 0913.5 2.0 rss )am

raa w ~ ~ 7 . 9 2 1 5 7 > w . n Y m . 9 d . 5 5.0 Jg]

I Report No. 00.802 Page No. 28

I

18 13

5 3 I3

20 13.

16 '13

2.

3-

1

3

1.

3

I.

3-

2.

2

3-

2

2.

2.

1-

-' I

.2

1

1% SD a32 * 12.0 232 29% 3x0 CD W a32 c830 WQ 13.5 16.7 282 3lb

pm 15m


i n 9 u 3

752 108 3

ue 8.2

xu7 IXP I ) 7013

1741 1739 W E 35113

r m ) * W.311 RP-

1533 50/3

Iy.i lB39 ,612 6312-3

2Luo -- 15.E

1m.s _- ln.0 174S.B 60.0

135l.L 1355.L 50.0 1353.5 13% 20.0

1.6 N.O 9u1, r t . 153.8 m, 59.8 u.. -1. 0 I kl T1.U 155. .* . -1.4

i5m 2Bw . 1U.O hirilv -2 oMrrir.8 t U Qr M

m.0 Imp 23L 5 3 -5 A.2 Imo c tEo5 zw 8.0 110

3750 c ZZWl zxrp 6.0 Bo A

1500 s 1M.L 1420.1 1.5 3

28m L 2432 lbj6.3 1b.O 9 -14.7 A a n l b p , u 162). P5Wn.n-

Al.0 w M 10311 -1. bo . zzm zw.e 9.0

-92.1 Also 111435. u 1MD.7, ,240 .In., IlE 2 9 6 . a t - k . l

*,At=. 4.5 W3 E 1433 lLji.5 -79.7

1 I I 1 U I

I


AFTENDM A

For the sake of convenience we have included Tables 1, 2,

7, and 8 fran Source 4, as Tables A-1, A-2, A-3, and A-4.

F i

Report NO. 00.802 Page No. 33

1 I

- YO -

1

2

3

4

5

6

7

8

9

1s

11

12

.3

.4.

.5,

.6.

.7.

.8.

9.

io.

'1.

'2.

'3.

'4.

!j

35

'7

'8

'9,

IO.

:1,

12.

:3.

;4.

-

FCA Rise h u a t i o n Ahs. Flare Date Beg. Tia.e,hrs. hrs. db. Cmset Mnx. XmP . . Position dt Rnnqe Start Times

LZzi Feb. 23

War. 10

Rug. 31

Nsv. 13

195z Jan. 20

Rpr. 3

June 19

June 22

July 3

July 24

kw. 9

R u g . 28

U . 29

LW. 29

Lug. 31

kpt. 02

iept. 12

kpt . 18

sept. 21

tept. 26

k t . 20

22E 'eb. 10

lar. 23

!ar. 25

lune 06

ruly 07

ruly 29

Lw. 16

Lug. 21

'U?. 22

LUG. 26

mept. 22

9.22 'eb. 13

iay 10

0400

1430

2000

1503

1330

2215

0500

ogoo

2015

1600

1300

oooo

1300

1415

1700

0200

2000

1703

2103

2100

3500

1500

1530

o600

0130

0400

0600

1400

1530

3100

1403

o800

2300

18

38

14

27

16

14

44

12

10

7

12

12

9

13

18

22

14

34

13

22

16 (2

0.2 19

11 %

a b

1 dh/hr 89

22 80

12 74

3 dh/hr 170

123

160

69

63

86

65

u 5

52

27

50

27

58

46

46

57

63

31

64

37

53

E2

'36

30

71

13.0

3.5

4.9

5.4

4.1

3.9

Weak

5.0

9.2

2.0

3-1

Wemk

3.2

8.2

4.9

7.2

0.5

5.1

2.0

7.8

3.2

3.2

10.0

Weak

23.7

1.5

715.0

3.0

10.6

16.6

5.0

2.6

22.0

0334 -- 0515 -- l226 l246

1430 1501

0617 6 2 9

0810 0955

28/2010 2m4

a 1052

1257 1 9 3

1313

=/E36 0303

18 1658 174 {818 14

1330 1335

1907 1952

1637 16bz

9/2108 21b2

0947 1035

0557

0436 0448

we0 CLZO

0259 0304

0433 0440

20/0042 0045

1417 1450

5225 CQ27

0738 mjo

l2/2301 2325

2055 2110

3

2

3+(3)

2

3

3

2+(2)

2

3+ 3+

3

2

3+(3)

3(2+)

3(2)

3+(3)

3(2+)

3

3+

3

3

3+

2+

3'

2

3(2)

3+

3

3+

3(2+)

3

3

2+(2)

3+(3)

3+

N23 ii&

N16 E%

N15 E15

N16 W 1 0

S30 Wl8

514 w60

N 2 0 EA5

1123 EU

N14 W40 N 1 0 W42

524 w27

so9 ~ 7 6

S30 E35

S28 E30

S25 E20

N25 Yo2

534 w36

n i 3 wo2

N23 E08

til0 w c 4

N 2 2 E15

s26 w45

512 v14

S14 E78

515 E50

N16 W8

N25 w08

S14 W 4 4

S14 W50

Nl6 El?

Nl8 wlo

N 2 0 W54

s i 9 ,ab2

n i 3 ~ 4 8

Nl9 E47

lhlp 31/1415-31/1530

3h 3@ 21/1200-21/2ll5

l h 53h 26/2100-26/2315

4h 2? 20/1700-21/1400

eh 5 P 10/0500-10/2400

1p19" 2l/14W-21/1730

lh 2r 22/1500-22/1745

oh 55" 26/0100-26/db00

Sh 2? 22/0530-22/1730

OriKirl.%l Ssurces

Be, Bo, DLP, HG, HAS, E, 0% =, s

Bi, B2, Be, Bo, CJn, DIP,=, HNS, JP, K, Rh, L, O H , €5, RL, S

B1, E, DLP, HNS, K, L, RL, S

5. Be, Jc, JP

:hers

, nc, IX

, Mc. WH

, Me, w

>, !!, Ma, VH

>, M , Mt, UH 3

3 , K, 'JH

3, E, KO, -ai

3 , 1.;. I.:=, w

3 , 1:

3 , ).:o

I , I<, KO, irx

I , x , UH

), K, KO, .m

I , n, MG, w

1, M, KO,

1

I , I:, MO, w

1, 14, WH

BO, I.!, KO, i

3 , It, Mo, kW

3 , M, MO, m

3 , M, no, w

0, K, w

0, I, KO, w

0, K, NO, WH

0, K, No,

3, x , WH

3 , K, ko, WH

BO, M, KO, 1

BO, M, Mo, 1

Bo

BO, K, Mo, I


- No.

35.

-

36.

37.

38.

39.

40.

41.

42.

43.

44.

45.

46.

47.

48.

49.

50.

51.

52.

53.

54.

55.

56.

57.

58.

59. -

FtA'S U r n ASSDClATED PIARes AND SCURCES (cont.1

FCA Rise k t i o n Aba. P l a E Date Beg. Time,bra. bra. db. h a e t Hax. Imp. Position t Range Sta r t Times

July 10

July 14

July 16

Aug. 18

s?s hr. 29

War. 30

Apr. 01

Apr. 05

Apr. 28

AT. 29

k Y * r y r 6

MY 13

Sept. 03

mov. v

R X . is

Ne,. . 21

J u l y 11

Jilly 12

July 18

J u l y 20

Sept. 10

Sept. 28

s?3 Sept. 20

Sept. 26

0'445 27 72

CU50 10 168

lloc 60

C&X 50 73

Zoo0 >36

1003 6 73

040€ '16 55

0230 12 30

o400 0.4 114 db h

1030 3.2 8 ab/-

1600 0.15-0.33 103 db/hr

1400 16

0430 15

0200 15

2ooo 18

2245 1.7 d b h pre-sac 3.3 db/h pst-fisc

2400 15

0745 8

65

E?

73

7Q

51

72

55

79

54

89

20.0

23.7

21.2

3.0

2.6

5.0

3.6

3.1

3.5

14.0

3.4

16.0

4.5

2.7

21.2

20.0

3.0

1.3

17.0

10.0

Weak

-30

0349 0527

2 2 8

1030

0710

1540

0859

0245

0137

0210 0359 0554 1016

1448

0532

0108

1330

x 2 1

1615 1659 i n o 1025

2.9 1555 1610

3.3 2223

3.1 2403

4.6 0638 o n 7

3+ N20 E60

3+ m 7 ~ 0 4

3+ A16 0 0

3 SO7 E31

1 mowgo

3 m 3 p29

lh 5@ 9/2000-10/1000

lh 2dc 14/Wbi-lk/C&X

lh 3@ 16/22CG-17/600

oh WP 1 8 / 1 1 0 0 - 1 9 / 1 ~

gh 4$: l l /22Wll /2400

sh Id" 12/1300-l2/2115

9 1 9 18/ll30-18/1200

L, K, Sat

Xhera

BO, Y.. KO, W i

BO, I:, Mo, 'UH

BO, Mo, YH

BO

BO, No

BO, r.: , I.:O , UH

Bo, I., C O , mi

BO, l:, I'o, "4

BO. b!, 1.10, Mi

BG, X, Lo, Wn

Bo, !.!, no, UH

BO, M, Yo, UH

Bo, K, LO, 'W

Bo, K, 610, an

BO, r4, LO,

30, t.:, !?>, 'a

BO, L, YO, mi

BO, M , Mo

BO, H, Lo, UH

BO, PI, I:o,

I, No

BO, M, Io, UH

R

A

Bi

B;I 3e

Bo

Bo

m

DH

DLP

M O

Fd

GO

c

w,

3

H3

mis

J C

JF

K

Ktl

L1

L. I ’

f Y

1*:0

OH

Pa

x S

SL

iJH

Anderson

Pailey

Bailey

Besprorvkmayc

Bookin

Basler b Ouren

Collins, J e l ly h Natthcrs

Dodsm b Hedemn

Dvoryashin, Levitakii b Prnlnatov

%geland, Hultw-ist & Ortner

Freier & Webber

3osl i iy

OreCory

;reensta*t & !bretx

:e11

iiainva & Goh

Hakura, Ragai & Sam

Je l l / & Collins

Jenkins k Panhis

Kahle

Ktlocholava

kinbach

Leinbach

Ynlitson

Malitson k Webber

I h i i s e t :e

Obayash ?r Hakura

Pil;eott k Shapley

Reid k Leinbfich

Sinno

Snapley b Lincoln

i larvick h Haurwitz

T A B L E A-2

SOURCES USED m m m CAP R B S ~ I D R DATA

J. Ceophys. Res.

Planet. Space Sei.

J. Pnys. SOC. Jam

J. E % p . 3nr. ?*pan

3. Pnys. SOC. Japan

U. AlMaba CeophYB. -St.

Can. J. Fbys.

Ark. Geofyaik

Soviet Astron. A.J .

Ark. Geofysik

J . Geophys. Res.

J. Ceopbys. Res.

J. Geophys. Res.

J. jeophys. Res.

J. E y s . Scc. Japan

J. Rsdio Iles. lab. Japm

Rep. Ionnsph. Space Res. Japm Can. J. Pnys.

Can. J. Phys.

U. A l s g l a Seophys. Inst.

Ce5az. Aeroncny .

U. Alaska Geophys. Inst.

U. Alaska Geophys. Inst .

1ASA Til

NASA w

9 lz

17 A-1

17 A-1

17 A - l

R-152

- - - -

3.2 1 2 7 s

63

22

-

a 6 i

- - 17 A - 1

5

- - Y 4

41

R - l z ?

- -

2 - 1 A- 3.27

R - 1 2 6

R-160

R-169

Mamed Spacecraft Center Erq. Des. k Oper, Ed.Purser, e t .a l .

J. rmophp. Res. g Antarctica Res. Geophys. Mon.

7 - 6A J. Geophys. Res. - 11 J. Gemag. Cecelect.

AM. IGY 16

67 J. Geophys. Res. - -

3113-3148

u1-120

1801-laOj

1-10

280 pp.

1317-1332

Report NO. o0.802 Page NO. 34

:I-"< 003c

12-1: 1310

12-29 2300

1-3

3-11 ?4Y

- 3-14 2295

3-31 15%

i-l? - ix

1-26 liy.

- - I ? 1233

?-e2 *;:

1-11 2 2 3

;-25 31m

I&

* 11-13 ;iio

2-31 203':

k-15 1230

4 0 2

a

7 2 - 6

12 66

74

1s 46

30

63

2

-d

123

j.2

Jeak

2.6

Wemk

ileak

Yenk

4.4

i.i

very S-al

-1.5

E

2 db

2 db

1-26

I

134- 1132 2

0134 0137 2

2229 2230 2

0330 c&2 1

1454 1507 2

3113035 W14 2 3Of2345 2 3 7 1 31/153" KJ52 2 31fWXKi 9-31 2

I

2041 2 1 3 3

X25 -37 1+

14% 1U l+

w1 OgaT 2

1034 1125 2

A20 E41 17/03ml7/16CC H , E, FS N25 di0 28/2300-28/2400 H, Jc. 2

N l l EO2 11/03oO-ll/lOxI Be, J'. €5, 5

s21 USL 14/1503-14/22w Be, E, Tp&s,s

31/nc -3l/l6oC J C , 'Tp

Bi. BP. Be, WH JP, K, L i r €5, 1

s10 uy Sa? W 2 3 A31 E57

A16 U6l JC, Jp

817 E78 13/MXX-13/133> Be, JC. 5 ll? €53 S12 i i 2 NW yli N17 E21

9. M O . c 1 N22 E03 11/22W-l2/07CO B1. 4

13/16m-13/2030 J C , S

S22 U64 25/2100-26/2303 G, J C . E. K

3 6 5 1 2 1 8 61

yIn ~ 5 % 324

3 6 6 l2140 10

3101 1???5 2 l l

11314 12855 313

UYl l2874 263

4449 13016

1 3 6 3

44% !fi%l WIRL

S

W6q 13878

14211

-354 14414 5340 5344 734r

+527 lUOb0

5858 15043

6261, 15461

6 9 6 15507

67% 15714

N36

Sl'i

ni'

Sli

s72

s13

n23

S24

AIS

N22

R11

SI5

S13

N17

N17

l a 2

Klo

SlO

am

N 1 0

s1;

w -.. G2 1-15 03

C3 2-7 07

C 4 2-15 10

Gj 2-29 16

00 3-10 18

G7 3-17 18

w

Cll 4-15 10

...I

C16 5 4 9 OB

u

Gl8 5-1, 15

Glg i-20 10

W'3 6-Ol 14

C2l 0-15 10

622 -25 17

023 6-21 23

2 4 6-28 19

325 8-11 24

326 9-26 10

UI

Y

1

4

4

8

2.5

3

4

> 3

2

3

6

2

> 2

>1

1.5

7

5

10

E

> 1

>1

> 1

>2

6

R e p o r t No. 00.802 Page no- 35

T A B L E A - 4

P U ' S B? (RlgMRI aar IuRm lgbo

134

1546

1-0

1620

0719 0957

0734

dl25 1418

W8

ogoo

0653

1215

2156

1217 l & 5

1 9 9

08y

1030

lCe3

0340

2 V O

1059

1839

2

1 2

1 2

1

1

1 1

3

l+ 1-

2+

?.+

2

3

3

1 1

2+

1

3

3

2

1+

1

3*

- * 4 v AaP.

14

17-5

<1

1

1

2.5

1

ll

2

6

4

6

1.5

7

5

1

1.3

8

1

1

2

ll

-

snvee Strtim

818

swtt B.

SCOtt i).

5525

5551

5585

5592

5597

5627

5657

5663

5669

56eo

5695

5 n 3

5791,

5-

5903

5%

5959

l e Y 5

1423-3

1424-21

1&4-39

1125-1

l&ll

lkzl-ll

1427-28

1&7*

1428-cp

1426-27

1428-39

1430-3

1430-23

1433-19

1433-39

1434-33

14657

l47Ol

14738

14751

14796

1483

14840

lW 14867

14885

1W

11981 149%

l 5 W

lSu4

15l51

analysis of cap ~i rf - nasa

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