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DISCLAIMER NOTICE

THIS DOCUMENT IS BEST QUALITYPRACTICABLE. THE COPY FURNISHEDTO DTIC CONTAINED A SIGNIFICANTNUMBER OF PAGES WHICH DO NOTREPRODUCE LEG'BLY.

LMSC B0069e6

Rev. A

DASA- 1926

5 $7ARFIS!H Wi-5PENING

R,. A. Vcrj

). H. Hollarndw. I. ruttermrn

repared by LockhecJ Research IWhoratory

Lockheed Misslles & Space Ccmpany

A Group Livislon of Lockheed Aircrort Corporaluon

Contract DA ,1-140-X,- 268

Thin Reccarch has becn sponsored by the

Defen:;u Atornrc Support Agency under NWER Subtask 07.003

LOCKHrEED MISSILES & SPACE COMPANY

B

L.MSC BOOM9g.

FORTNA ORD

This is the third in a series of reports prepared u.-,dcr Contract

DA-49-146-XZ-268 dealinrg with results and interp-ctation cf thc hiqh-

ltitude rn:vlm'r r.t:,:-itircs irin C) irat__on Pishb.v.'1 . "iightrope was

discussed in DASA 1638, Bluegill in DASA 1645 and this report Is con-

cerned with Starfish.

17.

9 A '

1INANNOUNC-Ii'

LOCKHECD PAL.O ALTO RTESEARCOP LAIJORArORY

A ( f' * K - I * I V # I % 1 1 LAC CM• V A 6•,a t 1(b' O tO,

LMSC 8006988

"Thc (-xpcrii;,c:;t3] ,.,ta obtained during, tlre Starfish detonationl are

;cusd, w,.ith co;ph3sis on the. phenumenology and c1ccirom;3r.etic

propagation. Various models of use for explaining the phenomena

observed during Stdrfish are considered. Modcls ;re formulated

whmch ctn be uncd t precdict elfects of othcr detor.ations , SiMlir to

Str! in yield dnd al.1tud.

LOCKHCED MISSILES & S$AC'.E COMPANY

LMSC-flOQG9SS

Con t cn ts

Ab..b tract

TabirP o! CGotcntb

2. De.crip:xcn of Veapon, Crricr and Envircnrment

3. Er.crgy Oiupu-t

4. rfC,;'tý o Entrty COtput on Environmer[

5. Flor•y Debris MI'Aon Phein-on.,nokogy

6. Beta Poitches and Lzte-Time Ucbri• Distribution

7. fe:ts on £Iectromagnetic Prcpagtiun

8. Conclusions and Summary

I

'i!

LOChHE&•.) ;MI3-•LE.S & ST';,CE COM-PANY(

9 9

-- I

Chapter 1. INTRODUCTMON

1.1 Purpose Of Report 1-1

1.2 Suzv:!y of Report 1-1

1..3 Pu~pose ard Results of the Starfish Experimenet1-

Rcfrcnces 1-3

LOCKP-ltA"D PA LO ALTO RESEARCH LABORATORY

1 C S II - I SSI tI S L S 14C I C (IN fA k

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L MSC-B0O6988

Chaptcr 2. DFZCRIPTIO.': OF \VWrAPON, CARRILR AND ENVIRONMENT

Page

2.1 Details of the Starhsh W\epon 2-1

2.1 .1 Introductio.i 2-1

2.2 Coordr'nes ar.d Geometry of Starhsh 2-7

2.2.1 Csorijnates 2-7

Z .2 .2 CZ u':.-tiy I w " ', T , 2-7

2.3 The Armbient Environment 2-16

2.3.1 Ambient Denstr" 2-1r

2 .3.2 Ambieat Atmosphere Compos'.t;o at Starfish, Altitude 2-21

2.4 -,ý-;mn.tic Field 2-22

2.5 S',i .,oary 2-23

S-, erc n cc s 2-24

xl

LOCKHEED P'ALO ALTO R.SLARCH LABORATORYI I SI S & A C I ( tQ W P A V

LMSC-LOO 6'3*

Figules

Page

Fig. 2.1 Geometry of Starfish 2-10

Fig. 2.2 Camera Plate Coordinates 2-13

Fig. 2 .1 Flat Earth Geomety of Starfish 2-15

Table 2 .1 Constitvents of Starfish (DASA Telegram) 2-2

Table 2 .2 Cornstitucnts of Starfish (Lokke LTL Calculation) ?-3

Tablce 2 .3 Starfish Constituerts (HE::RE C-1culaticn) 2-4

Table 2.4 Assum•nd Starfiih Constituents 2-ý

Table 2 .3 Numbers of Atoms in Starfish 2-6

Table 2.6 Distances from Ground Zero and Southern Conjugato Point 2-17

Table 2 .7 Starfish Density Comparisons 2-20

Table 2.8 Model Atmosphere Composition 2-21

latle 2 .0 Assumud Starfish Ambient Atmosphere Composition 2-22

xli

LOCKHtEO PALO ALTO RCSEARCH LABOFRATORYt O Cz u MI" I S I I ( S 4 A C I C C M V 4 1U 4 V

A B U .1 11 0 of i c I o? Ic# l 1 0 4 .0

C.cr3. TPiE CUTPUT OF TUEZ \VEAPCN

3 3.1 Gi.'2ocraI Charpc~crititcs

i

Enr.crqy Yield rotlo

h3 Int*Itai X-R.oy Puke 3-

3 .~ netrzn Output

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VAMSC- BOO693

Figures

riq. 3.1 X-Ray Yield and Tenperature ot Starfish 3-

F'ig 3 .2 Starfish Energy Output 3-7

Fig. 3.3 Starfish Lo*kc CZalculat'..:n 3-13

Fig. 3 .4 Appv,)xvrate Initial Mass & MNomentum 3-GC

Distbutiticn of Starfish

Tables

rzL.I-e 3.1 .eosulls of Starfish 1iE'.E Cal 1.-io 3-5

T,bla 3. &tnrf:.h ZVisible Outp3-

Ta•Lle 3 .3 St-.rfish N4cutron. Our',p -?

Talo 1 .4 Starfish Velocity-Masc Distribut~cn .- 5

LOCK•NtrD P'ALO ALTO PEStARPCH LA8O0lAIORYf P fI t iS$- % -~ A( I k Ut. Pakr

LlMSC-b3OCSC8

Chnpter 4. ErFiCTS Or R'ADIANT ENERGY OUTPUT

CI T}ZE t 'V(ONMENT

Pare c

4. I I:ntroduction 4-1

4.2 X-FPay Energy Deposlt' 4-2

4 .3 The IrJitlal !adlation Pulzt 4-5

4-5

4-9

S..... • [,.I I .... . th A .c nn Durln9 FCxp3nsion.

4.5 kjdizitýn fr:m the Dcbri-Air Pistcn 4-19

4 .c Lif -Is of ,l,:'sphirlc 1!cating 4-32

4 .9 Sum:7:-ry ond. C.nclusinns 4-33

Pc erC rCeCS 4-Jb

LCC.HRECV) PALO ALIV REb-AR'CH LABORATORY

* * * r.' .. C~l I •' . '' • e . I. ! - , .r

LMSC-V•06988

rigures

Paqc

Fig. 4.1 Enegy Distribution from Prompt X-Ray Pulse (hv > EK 4-10

Fig. 4.2 Absorption Coefficient 4-12

Fig. 4 .3 Blackbody Temperatute as a Functcrin of Time for 4-15

Expanding Weapon Debris

Fig. 4.4 Spectrum 4-17

F's. 4.5 Enermy Deposition per Unit r,-x 4-20

for Several Values of ;4 .

i . 4. c, Initin ,1iectrcn Density and Tempcraturc Rise 4-23

4.

rig 4.7 I.11! l 0 Density 4-30

Tables

Table 4.1 Number of >:-Ray Photons Above thn K-Ldce Absorbcd 4-8

Per Atom

"Taile 4,2 Characteristic Times for Electron Cooling and 04 4-28

Charge Exchange

x-v'i

LOCKH£E1O PALO ALTO RESEARCH LAOORATORY

C F 6. 11U I 1 , &4 4 ACI C 0 0 $ A 4 T

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Ch.npter 5. UARLY DEBRIS ',.40TION P-l1HOM.ENOLOGY

rage

5 .1 Introduction 5-1

5.2 Initial State and Movement of Starfish Debris 5-'.

5.2 .1 Initial Debris Ionization 5-6

5.2 Debris Stopping Mechanisms 5-8

5.4 >pailding Debris Model S-

5.4.1 Mignetlc BubpolL. Ccnsiderations S-12

S. 4.2 ̂ 7',,e ý,uLe•c ,•L lv Bou•,dla:. Lzjyu- ; - i

5 .4.3 %13gnetic Pick;up L.echonisn 5-20

5.5 M,.'anetic bubble Exp3nslon Models b-28

S .5.1 :¶.c.n e'ic •ubblc! E£.p-nsion - udel : 5-.28

5.5.' !,3gnetic Bubble Expansion - Mcdel II 5-24

5.6 4;,c Snowplow Approximation 5-37

5.C.1 Justification f)r Sno%, plow Thchniques

S C ? Snowplow In Varyin) A,,os;hre -9

5.6.3 Application of Snowplow to St'?:ish 5-41

5.7 Porous Snowplow Model B-.16

xvi

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5.8 A De-ailcd $tarlish Model S-S7

5.8.1 Density %todel-

5.8.2 Asymmetry Mudel .- 58

5S. .3 Geometrical Detail3 and Magnetic Field 5-58

S.8 .4 Details of the Model 5-60

5.e. 5 Input Parameters and Output Results 5-63

5.8 .6 Results for Starfiuh S- 64

. .8.7 Results fzr Other Bursts S-CS

.9 DifusZ-1 o :-gneuc Fiel into 5ubble

5.10 Debris In the i,/drcrragqnt.c Eubble 5-6E

5.11 Surrm-ry 5-7^

Rc fi 'rc nces 5- 79

xviii

LOCKHC•O PALO ALTO RESEARCH LAOORA-ORY

0 C.. a , I I v 0 1' % I IC e Ill ,0e(.AIt LI 1 (• tAP 0.l

I

I . . . .. . ..... ... .I 1Q

LMSC-D1O06988

Figures -

Page

Fig. 5.1 Hydromagnetlc Shock Structure 5-23

Fig. 5.2 Magnetic Bubble Model - 1 5-33

Fig. S.3 Equal Mass Contours. 5-42

Fig. S.4 Simple Starfish Snowplow Model 5-44

Fig. 5.S. Porous Pickup Model (a = 0) 6-S0

Fig S.S9 Porous Pickup Model (c = 1) 5-SI

Fi r. .5C Porots Pickup Model (x m 0) S-S2

Fig 5.6 Hydrrmangnctic Shock Bubble 5-$6

Fig .5.7 Geometry of Hydromagnetic - Debris Subble 5-70

rig. 5.8 Geometry o! Detailed Starfish Mod-el 5-7!

Tables

Table 5.1 Starfish Asymmetry Distrib'tion 5-59

xix

LOCKI4C•D PALO ALTO RESEARCH LAOORATORY1 0¢ C k t j 0 Atl I S a S 0 A ( I C a " p 0• A Nl IA gl it i ii&& l leCd O0 IA~d?

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LMSC-B006988

]

Chapter 6. BETA PATCHES AND LATE-TIME DIBRIS DISTRIBUTION

Page

6.1 Introducti on 6-1

6.2 Beta Patch Formation in the Northern Conjugate Region 6-3

6.2.1 LASL Data 6-4

6.2.2 EGG Data 6-12

C,.2.3 Analysi5 arnd irnterpre.aion. ý' NCR Cpt.ical Dato

6.3 Beta Patch Formation in the Southern Conjugate Rogion 6-26

6.4 Deiayed Neuwron ;.,easurernents in the SCR

6.5 Delayed y-Ray M,;,-3urement in the SCR 6-34

6.5 ;,irglow Measurements in ihc S-R G-35

6.7 Riometcr MWasurerenLs 6-36

6.8 Sunmear and Conclusions 6-3V

References 6-42

LOCKHE-- VALO ALTO tYr-rAPCH LA.-M.'?ORYC , C a f. II "$$ II * ' $ut. . (I M ISSL , M f

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LMSC-B006983

Figures

page

Fig. 6.1 Beta Patch Formation 6-2

Fig. 6.2 Aircratt Locations in NCR 6-5

Fig. 6.3 Debris and Aurora Dimensions 6-7

Fig. 6.4 Visible Power arnd Energy from the NCR 6-11

Measured by LASL

Fig. 6.5 Visible Rad-rce at Early Times 6-15Measured by EGG

ig . 6.6 Late Time Radiance Measured by EGG 6-16

Fig. 6.7 Field Geometry for A/C 53144 6-24

Fig. 6.8 Map of the Southern Conjugate Region 6-27

rig. 6.9 LGG Radiance Measurements at Six Points 6-29

Along the SCR Auro-a

Fig. 6.10 SCR Radiance and Calculated 0 Energy 6-30

Deposition Profiles

Fig. 6.11 Debris Density Inferred from Riometer 6-37

Measurements

Tables

Table 6. 1 Aircralt Positions in NCR At Shot Time 6-4

Table 6.2 • Fluorescent Efficiency Implied by LASL Power Data 6-20

I,

),di -d

LOCKHEED PALO ALTO RESEARCH LABORATOPYSOC 9 Is • M* 5IgS I S AtI A O PAN?a (.oup C.1.1d O I# ýC OCf 1 0 &-sc I@A €01114#IA'ol

Cnapter 7. EFPECTS ON £LECTRON'MAGNETIC PROPAGATION

7.1 introrduction 7-1

7.2 Radar Attenuation 7-3

7.2.1 Sandia Rocket Data 7-3

7.2.2 Project 7.2 Radiometers 7-5

7.2.3 Project 6.7 Rocket Data 7-12

7.3 Radar Clutter 7-21

7.3.1 Introduction 7-21

7.? .2 Observations on BacKscatter 7-24

7 ,1 ystem m EIL- s 7-29

7.4.1 Angular Error and Jitter 7-29

7.4.2 Range Error and Jitter 7-35

7.4.3 Pulse Distortion Error 7-36

7.4.4 VelocIty Measurement Error

7.4.5 Attenuation 7-41

7.4 .6 Systc.ns Effects of Starfish-Like Bursts 7-42

7. S Cc.mn'unications Effects 7-49

7.6 Summary 7-50

References 7-51

0 CiI

xadii

LOCKHrrED PALO ALTO RESEARCM LABORATORYtOC € wt'fB M zI %i E) $ 1 PA .' (,OMUPaN,I C. iOu. SPO!I|O 0$ i$Q I"IeI aectam ceII ,eOaltl~i a. .

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L1ASC-B90 69 88

Figures

F ag-e

r'ig. 7.1 Sandia Telemetry Signal Strength Record 7-4

Fig. 7.2 Project 7.2 Radiometer Results

Fig. 7.3 Project 6.7 Rocket Trajectories in the 7-14

IMagnetic Meridian Plane

Fi,;. 7.4 Altitudes of ProJcct 6 .7 Rockets 7-15

Fig. 7.5 Projection of Project 6.7 Rocket Trajectories 7-16

on Ground Plane

t* r. - . ..tzrn,:a.tion o( Prcif-ct 6.7 Telemetry Signals t U 7-17

Johnston island

Fig. 7.7 Ra~dar Ang-lar Error 7-31

TaMes

Tublo 7.1 Project 6.7 Rccket Parameters 7-18

Table 7.2 Pro-Shot Signal to Noise Ra3ic (db) and Duratiun o: 7-18

Complete Plackout on Project 6.7 TWM Links

Iv

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LOCKME-cO: PALO ALTO RESEARHC LAP1ORATORY

0 O I4 1 mi s l s 6 5w 1c : 8V "

(,to - D V.S.". , #, i - it 'oot#AF, C 0 ,044 Q.

LMSC-BW0698H

C;Ltpter 8. CONCLUSIONS AND SU'A?,ARY

8.1 Systems Effects 8-2

8.1.1 Introduction 0-2

8.1 .2 R/V Destruction Mechanisms 8-4

8.1 .3 ?,:u~dbur:t E-fects 8-6

8. i .4 ElcCtr)n Trzil;pig Effects 8-7

8.2 Sca'ing Tstimrtes 8-7

5.3 .3 u:-r ry

LOCKHEcD PALO ALTO RESEARCH LABORATORYS0 ¢ C 9 1 f v' I, I I k, I t. 0 A C I C,..0 A A # A

• i eOC. e .I ,)C CI a 4, CI- I

,0 T• . L:~.,¶SC - p2 C .,=

S.i 1 •rp; 01 Report

The. pjarpvsC o0 thts repot is to sl'in-irize brtefl[, the phuno-nol '.;y

C ,i tho ..uz.i.t . 3t S arf n to e 'r.clu ptud;ztiý'.; tc e .:) r1- mj:t.

t-he c:'•e•ts of e-hcr yiol:! an. altijtude in the Star'lli! rzvje. This Isan

.I S. the lOe .'t U:'ersto*" , : '.

.nc.;r, -!In cr a-blruous, V.e s:ýII howv: eve. r at .i.'.t to icsc;IbI: Some rz.np'c

-:': iq -. " ;;et:u."'e•olD, iy ch iro oi j•, -zr- : c i,-.::%- the Sta:}j I A vo

4 .i i. txcy C-,l L-') e>;t :I• 3 i \ni- ý : ,- i - -, .,

! .2 .. r.:vvy~ of { ;: r

,. Lric' sur.cy of tho r( port is -,it follows:

Ch,.'it•'r 2 c• siCes ,.h, S'~rfsh weoapon itsel., its crnstlutcnts 31d

Chapte..r 3 e\arn -,n s the cii,(')jy output of t!.c wcipon th, el tho,, rctC.!-il

A bmsl izi lit" csti:.;tet .

(. .• 3cr 4 ?,zmblcu:rs th; cfit•c.s olit enc rgy oltlut on, the £urofl ., . .Iotnc-;,phtrc (.,-ui ir. nsi; L.rv) znd the distorb.ince ci,.-.)tcd by 1his iw..,.yr 'rat :

L(3C..m!Li:n PALO ALIO !415I.Al#CH LAIJ.-j.!CRY

• *.* s - i . a" i *. . • • .

0 '•9;,i• , ,t I, •t t " I ,#, i i "II i lI

Cktcr ~S ConslQSts tht harh' 5tages Of Starfsh event, the •iread of the

deris, (formatio~n of j fnacgnetlc bubbl%, hydromagnetic shocks and Nyavcs

-!,d othcr relatcd phenomcena

Chaptcr 6 considurs the late time effects of Starfish and the ultirnate fale of

the debris.

Chapter 7 ccnsiaers th'! effect of Starfish on radar and communicatlon.s with

aor eye :cward the effects on systems.

Ch•'*,•: 8 gives a bric-1 survey cý: systers effects and a s•.T.azry of -

SIOr.s :-C2chc. in t•,o rep,--

Delet .e

1-2

LOCKHL. . PALO ALTO , JEANZ . .AO'rOHA44Y

ý- . 0 J - 1 Ii~ itS 6.1 cP~ 08-oos

L.•SC- B0069C8

rlcterem.c ior Ch-.•ptcr I

. Hcncrick, R. . et. l. ,'tc,.'J P~cenor."::a icr Operation ,hbw,.

1-3

LCCKHFCD PALO ALTO REbEARCH LAUDRATORRY

1 C. C a a I I a A I s i A I u a & I 1 C I (O S0 a 0 sv

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I

Ch',:: . DLSC!,IP,?.' OrF V.F'..PON, C%7,1IER AND ENVIRONM.ENT

In th~s ch3pter we consider tile weight anid constituent characteristics

o! th v we3pn,'- the %.eapon ca.rrier and the burst envronrrent.

2.1 DetolIs •z the Sta.rish Wccpon

2.1 .1 P..t t.duction

V. , shll c-r.sider in tlis section s~:me of the pertmnent d.tails of

v.ap;),n output hill he corsid-:rcd in the next ch3p"cr. We shall also consider

the • .- z.ri~.. ;,tr.• pn.m-r, :it •-t•rItsh 3 It!,ud.

71e do.alls o', t ,,• of Stc--:fth aiffcr depending

oC *,%Ir oI Ises as a t..ircnce s'urce * '7o .scrcp3ncies are s!7131 3r.d

cr,2 ! ;• - ..-. ce th,_ ph0:;ro: to y Strf. sA:-r is ,u..lc.•.. .• ,

uncr- urt a -., ,• e th.,._ difUerk,,ac !s insigniltcB.-Il.

A t.prIC- sLt of vIMues is that ,',en by i DASA telegram o-. filc at

D.'SzCcenter at Santa -3•rbjra:

2-i

LOC•HIEED PALO ALTCJ RESEARCH LA•BRATOY0O C a Nl f 1 0 UI I %I II 1 6 1 01 & C I €C ~ 0 0 0 6

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LMISC- DO30 69 88

A rep e bp i,,ke 1,) on the thcoretica1 (CORONLT-codc) calculatio-ns

of the Starfish cxp'osion gives for ,-om(.. of the weights,

Deleted

Table 2.2

Ccznsttucnts of Storfish (1.okkc LTRL C31culation)

2-3

LOCKHEED PALO ALTO RESEARCH LABORATORYc, c t k f 1 0 0 it s I 1 1 $, & %) p 1 ( I c 0 NOl r A W T

Cl w F -IOG. V,1 1 19O .40( @O6-440t { lP ~ tl )

LMSC-BJOg9B881

The report of Cowan et al. (2) used the numbers in Table 2 .3 for a

code computation (in a spherical mock-up) of yield (HENRI code):

Table 2 .3

Starfish Constituents (HENRr Calculation)

2-4

I

LCI••HEE. PALO ALTO FnESEARCH LACOfATORY

IsN I 1O I % 5 1 I # S f 1 6 - C I C (0M All I0 •eo.. &'VIO h o0 IVCSet *d(**l' 1 dC fOvIo

* .-.-- . * -'-.

LMSC.- 0069 8 8

Tnorc irc some s:r,.1 discrpancie in these variouz values, but we may

tae',. thc! co,- s.'ticn of Starfi.h to be that given in Table 2.4.

LDe eted

To|blo 2.4

ksumd Stnrfi;zh Con tlien:s

2-5

LOCKMREO PALO ALTO RESEARCH LABORATORY

| 0 C .11 1 0 .55 1 1 S IC 1 , 0 . A Id -&~ ~ . a0 "e 0l q 1 0 C O I .O I I I a t 4e 1 Cm 1 4 1 a 0 . 1 t0

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Del(c '

Table 2 .5

I.ti7C.bets of Atoms in Starfish

2-6

L.OCKW.LEC PALO ALTO RCSEARCM LABOI-ATOkY

* LeO ¥# bI 1| 0' *~I eE Slf £ ~L '''•W K et,oca tlip most l 1$ a PAC LOO ~ f-

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S.2 ~C rd •'- .'. .. F"'.z f ifIsh

2 .2 1 Co, rcln; tn-;t

Accordlrn to DASA-1'i78 (SR-19) (R~ef. D7), Starfish occurred at 2200.090

iccal time on S July 192: (iccrding to the SF-Fl.IG report (Ref. M3) the time

was 0900:09.2-.i('Z.) Cc'orair~atcs .ec 16.4,( N and 19 .37 0 E and an altitude

De~et•F

2 .2.2 C; rccmu:trv ovf !t'r. f:sh

Since the phen.rnena of Starfish took place ovcr vast regicn: of tme

Pacific, photographs taken hundrcd. of kilomete:s from the burst pint will

show strorg elfects of the eath's curvature. ror this rea4on we shall

consider the geometry of Starfish In various aspect:,,.

(a) Thy projection of a portion of space on the local p!3r:e of a c ým.ra 'jhcn the

curvature of the earth is and Is not takon Into account.

(b) The geo'rwtr, of the Pacific area Including thL curvature of thu varlh.

We ars? intetested in these aspects of Starfish geometry, sinre )i is

necessary to save rn idea of the way the veor large scale ;.eophysicz!

2-7

LOCKHLED PALO ALTO RLS*EARCN LAOOI(ATCJP.YIC C• 9 1 1 1 D 61 *l S 1$ $ '. SFA ( I ( r, & I V A 6 V

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LVASC-BOO 696B

phenomena of Starfish appear on phottogr-,phs taken from vario'uS positlon.s

C:onsider Fig. 2.1. in the plane of the camera, c , a:'d the shot point,

s , we ha,,e as gt,'.'n quantities, h the altitude of the shot, h_, the

altitude of the camera, D the great-circle range of the grour.d zero point

of the shot to the camera and P the angle of elevation of the camera. Then

consideration of the geometry shows that (Ro = radius of eartl)

d r (Ro + h c) sin (D/R ),/cos(D/R 4, )

h H •altitude of horizon (tro. '.; ra) over GZ =

R + ( ,h* 2 h R R

h= altitude ,f horizontBl line from c. mera r + Rc C/ -os C/R 0 - R

(h S +ro)cos (D'/Rf.) - (hc.Ro)tan (h+R)sin (D/i%)

Applying this to the Maui-J.I. problem, we have that D = 14.'^ kn., hc = 3 km

hI =153 km; hH = 1 1 3 km and 0-9.3 0

_imern-Coordinates

Consideration of the geometry of Fig. 2.1 shows that in the coordinate

system X'YZ centered on the camera, with Z axis pointed toward the detonation

point, Y axis parallel to the earth's surface, we have for the coordinates of

the point P

2-8

LOCKHEID PALO ALTO RCS.LARCH LABORATORYI % C a H I 1IJ 1) " % I t 1 $ 4 1 # A C I C C1 A '.IA (CIOl•U1 * -S'Ok C, *C-1 IiO A1 i iS ! A.&( .O i 0IQ.

LMSC-B006988

1" D(.0 + +. 2

r .o

x=r Lcos n esing +sin -cos ro Cos (? ).c

y = r [sin ý sin (C -o

z = d + r [cos q cos -'o sin P sin 9 cos ( )- )

CCos GS = Cos P. Cos 4.. -Sin. a Sin Ao Cos ( 0. -C)

Here L- Is the angi= oetween SP and SC. The position of the point

xyz on the camera plate xc, Yc is g~ven by:

xSc xT -z

YC= y

T z

where f is the focal length of the camera.

If the geometry of the burst area is cylindrically symmetric, we can find

the image on the photographic plate of a horizontel ring (r = const, 9 = const,

t = 0 to 21?), and this will in general turn out to be a distortec. ellipse.

The horizon e.5 seen from the camera coordinate system has the

coordln3teS

h (- Cos0sin T 2-CosP sin0 tcos o1

2-9

LOCKHEED PALO ALTO RESEARCH LABORATORYk 0 C I2 04 ( 1 M•I t S I% 1 & aS F a I , O"vr &N W

A G.6QvI & .I IOgG& i0to( - 40A l( I oilto

1 1

'1

I \

t xI

/ /

i /'/' I-/

• " 2' X€

r~g. .1 Geomertry oi Starfish

2-10

L.•CNLCL- P.A.O AI.TO) R[,.EAS4C' LABORaT~rY

* *. O!.V **. *C*.au

11

LMSZ- B.% 0& •3S

' :" h +hc (7:0S sin-;

2- h +1'Cs o

"2Rh+ h (- sin H sin + cos 1os cos ~.)

where Is the a:imuthal angle of the horizon as seen from the vertical3 -x.p,:z

throu;h the camerra po.nr.', and z, is the dip anglc of the h;ri-on:

c~s rn = (Ro + h

Tho horizon coordin3te-•, n3p onto thc camera plate giving fcr the inage of

t _e hwrl:on

= (:tn in( * Cos O. S.,1

winch is a section f nn eillipse.

C,•...o,• o,•dln te f.:,", F!,%t rnmh

Consider ri' . 2 .ZA. .Wo have for the coordinates of the point P in

the camera coordinate systcm.:

x r (sin sin 0 cos 4 cos c,:s

y ,r isin sin )

-"d - r(cosp sin.* cost - sing cos

?-11

LOCKNELD PALO ALW% REf.rARCH L.0.',CRATORY

1 OCa I r a I S' S 1 0 % & I t A,.t I f 0• A At

A e ,4. 464, I( @Ali

Lii:n Ingb- IF \re bvc thc.t

(N -r cý-z :ý cr z,:wi sinp G r/"

The camera plate coordinates are given by

Y V

vhcre f is the lo~l lec:th of the c,•..-.cra, WVe see tat lines of cylindrii-al

camerr pi.ne if d :.- r If d is ci-nparable to r we have fc-r tho equ.3ion

in tvc c3mera pl:tc c, j hori,:on:*31 rini* et some angle - and ra3,.us ircý:.

the shot poirt

"The coordin3tCS - f are related to xC , •y a Inear trnntcr:,n.or,

d c1r -Cos $c-)s v.

r o .; sin ,' ( -in - sin ')- S.n ; : - (1 c s ; C '

d - r 5 ." "i

2-12

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LMSC-B30 6968

r7 c

....... ......

\

Ix.

, -x

r•3 2 . Camera Plato Coordin~ates l

2-13

Ln-•CKMf'CD PALO AL'TO RCSCARC1)4 i.A:!OIATURY

r C I I I D 1 4 t * & C I c 0 aO f a, "* t

I I# I I - I .

and the coe.!iclentt a , , , and a are giv'en by complicated functicnS

of ,' , 0 , and r/d e V ee th3t if the camera it, suifcier.tiy close to

the burst point, the image ol a horizontal ring !s a distorted ellipse instead

o! a regular one, with the amount of distortion proportional to r,'d .

The proJections of the field lines on the c~amera plate can be obtalned

by taking the field lines as a simple dipole approxint.i,cr

h = F.(Lcos 2-1)

Thenr from the eo.-etry o, Frig. 2 .1 we seu that

Sin2 ) sin 2 (P: + sin 2 (k - Ar) (,pherical tria.-.le)

where A is the magnetic latitude, and our coc:dinr,te system. ... ,, the

magnetic coorinate system (A is the magnetic aut••;de be:e-ath tre shc't

point); and

C! (hh/1r sin X -

COS P sinaiT s sin -l .'sinka/sain ka._-rQ

2 2 2 2 4(hs + R) + R L cos 4 - 2RL (h + R) cos'A cos (.I"F

sin '~*RL cros 2 sin)

gives the coordinates of the line of force (as a furctio-. of X ) which passes

6 puipondicular distance b away from the shot point.

2-14

LOCIHC( PALO ALTO RESEARCH L&UORATORY

• ,• P.., .~e• O l l • LI & "* '",l t.1

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2--S

/3i

i i/

/Z/1

/J/

/I

F1lj. 2 .3 Fla3t •arth Geomcetry of Starfish

f

LOCHEEO PALO ALTO RESEARCH LADORAI.ON

I 4- . ... .... .# t.

From r , z;,, as a function cf X % we can determine xyz and

Y' y and get thv procctorin of the magnetic line o! torce determined by b

and L on the photographic plate.

2 .3 The Ambient Environment

The main characteristic of the Starfish environment is its extreme vari-

ability in density as a function of solar activity, hour of the day, etcc. Ths

variability is important for the purposes of scaling the results of Starfish to

other yields and altitudes at these great heights. For this reason, above 2.00

kcr -or, the yield-altitude ph.xrwen-a2 .-- sh',il•i be in terms rather of yieki-

density. Even this type of scaling may be too crude kor certair, oPplicaLl.-'s

since the way the dens-ty varies with altitude Is A function of solar actw-ivty

and lOcal time.

2.3 .1 A.,bicnt Density

For altitudes above about 120 km the solar sunspot activity and the

time of day are important parameters In determining the density. Thus

p - p [h . S , tQ

where h - he,ght , S = solar activity (measured in units of 10 wattt/

meter - cycle-soc of the 10.7 cm solar flux) and t- local timo. In

Wneral

p(minimum) - p Cb ,270 1 400)

2-16

LOCKHEEO PALO ALTO RESEARCH LA1ORATORYr

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r.,stancef •'rorn Groond Zero

_ C'It_____ km

31

S-i 575

S-2 275

S-3 575

S-4 275

S-S 575

DAM', P 359

FrS 893

Oahu 1353

PaImyra 1433

Midway 1535

Xmas 2087

Canton 2156

Wake 2532

Dikttnce rrom Southern Conjugate Point

Acanla 100 to 200 km

West Samoa 300

Samoa 596

Tonga 527

FiJi 732

Rarotonga 1758

Table 2 .6 Distances From Ground Zero and Southern Conjugate Point

2-17

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LMSC-B006988 8,

The Harris-Priester atmosohere (NASA T."I D-1444) can vary nearly two

orders of magnitude at 400 km. :he Starfish event occurred near a solar

mini-num and at a locil time not too far from its minimum, and we may conclude

Xthat the Starfish ambient density -:'.s at the lower end of the density variation.

The variations can be ver/ large for these high altitudes, for example

at 400 km we can have variation of frozi 6 x 10 -16 (g/cmr2 ) at night, solar

minimum, to 2 x 10 14 (q/cm 2) at d3y, :solar maximum.

Various values for the density at 400 km are available:

1959 ARDC = 9.00 x 101is gr/cc

1966 USA-Standard - 6.50 x 10"1i gr/cc

Since at heights greater than 200 km the diurnal and sunspot cycle variations

are important, we shall examine for example the values given by King-Hele

and Quinn (J. Atmos. and Terr. Physics 27, 197 (1965)). For the period

1962-64 (night) they give 5.7 x 10"1G gr/cc as the density at 400 kmn, This

13 less than the values above by an urder of magnitude, and is due to the

decreased solar activity from 19S8-59.

A fit to the values of the 1962/night densities (as given by King-Hole

and Quinn) can be given as

p -p (200 km) (200/h)8.3 (h> 150 kin)

where h is the height in km and p(200) 1 1.7x 10

2-18

LOCKHEEO PALO ALTO NHSEARCH LABORATORYt 0 C % I I I I0 I I I t I I ACI C I JA P A I I IA 000VO ft tiOf ~CI 010 &IICIADI COOIOIAItlý.

VMSC- BO006988

Another estimate of the ambient density at the time of the

Starfish burst can be obtained from the atmospheric properties model of

Anderson and Francis (Lockheed Report 6-75-65-19). They give values of

N and K as a function of altitude and local time, where

p =K.SN

and S is the solar activity index for the data in question. Using the

value tabulated for the date of Starfish (S = 45) we find for 2200 hours and

for other times the densities given in Table 2.7. For comparison wa also

give U.S. Standard 1962 Satellite Handbook Night-Minimum, Harris-Priester

and CIRA values of the density.

We shall assume that the Starfish ambient density is given by the 2200

hours value:

pj 8.5 x 1 6 g/cc

Thc Harris-Priester Atmosphere (J. Geophys. Res. 68, 5891 (1961)) is also

given for comparison, as is the CIRA-196S atmosphere for low solar activity

and 2200 hours.

For estimation purposes we find that an approximate analytical estimate

of the density we have assumed for Starfish is given by

8.5 16 (40)0V h > 400 km

S0.5 1 6 1420 6.67 400 > h > 160 km

2-19

LOCKHEED PALO ALTO RESEARCH LABORATORYI1CINISa0 MSA It( & aPAC I COMPANY

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14 1-1 14 14 -4 U-4 r-4 c

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14 -t -4 •4 -4 • I

1% 1-7, ;.. .

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) -4 ,4 14 14 - ,- '4

-40N

.- •L. %o, ;I D r. - t•,D. .,' " •

~ .4 4 -4 -4 t\~

i in . .. ,• t^ --CS I

4-. a .x a - _ - o,"0& CU 1-4 el .e

. t ' L% '3 3 'N •, '0 .ý U

'Q J'• ") c

P--4 4 9 4 4

4 4o

t: 'o,, 'i .1 -g ' • ' . ...L. 0

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.4 0 . I0 Hl l$1t -t .& 'l3•. -~l I

o,. UN -4 N ' H -ý Hco

Li , ,.m...j

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5~.II

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LMSC-B006988

This fit is given in the eighth column of Table 2.7 to be compared with the

density of the 2200 iocal t!rne Starftsh atmosphere. As can be seen the

igreement Ls good enough -go we can use this sV:nple analytical fit for

Starfish analysis purposes.

Since the density at Starfish altitudes can vary so much as a function

of local time and sunspot activity, it is important for scaling purposes to

have an expression for tha density as a function of altitude, solar activity

and local time.

2.3 .2 Ambient Atmosphere Composition at Starfish Altitude

The r'.sults of Anderson indicate the following approximate composi-

tion tot 400 Km (:or zorce ti.me and sunspot activity):

C 298.0 x 10 / cc

N2 24.60

He 7.41

N 3.69

0 2 0.08

H 0.65

p 4.7 x 10= 1 6 g/cc

Table 2.8

Model Atmosphere Compo3ltion

Thus atomic oxygen is the most important constituent at the burst point.

2-21

LOCKHEED PALO ALTO RESEARCH LABORATORY

0 C iN IO 1 II I I I I I a S ! A C i ( 0Q " 0 M A

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~ ..--.- ,.-..---..- . . .. --. . . .

LMSC- 5,'u'3963

We normalize the compositic.n above to our assumed densLty of 8.5 x i0

and obtain for our model StZifish ambient composition:

0 270 x li3 / cc

N2 22

lie 7

N 6 "

O1 1

Totl 7x 105

Table 2.9

Assumed Starfish Ambient Atmosphere Composition

2 .4 Magnetic Fiold

The magnetic field had a dip angle of about 280 rt burst peioat. The

magnetic field line through the burst point intersected the magnetic e.uator

at an altitude of 900 km (L.- l.1S).

For our purposes, we shall assume a simple dipole modal for the

magnetic f.eld of the earth for which

" 0o.315 1 J 7- 3 Co2 n

2-22

LOCKHL90 PALO ALT0 RESEARCH LABORATORYtOc "wIio 6aI$611 S 6 SPAgl (oft# &"N. cJaoueDlrlll Iv )~a .e ,j.g g.iJ ljla li gee toa i~loeeg l

.a1

LMSC- 800698tl

n= \ .3eos c-sX)

where h - altitude ,R w radius of earth and X - magnetic latitude.

The dip anglo • Is given by

co.• , tan = 2 tanX• 4 - 3 c s 'k

\ •'..

Delelcd

2-23

LOC.I•4CU FALO ALTO f .,CAnCI4 LABOQRATORY

4 ,.er,. I ,.t,, U* *i~t. A € I..11f to ol • a a ,&

'0

S.. I

Rclrences for Chapter 2

1 Lokkc, N,'. A., L.lL-UCIC-4551, Rad,,ýt,.;cj Flux ard Debiris Anqul*,ir

D)stribution r.o,, Starfih, Lawrcnce Ra.oton Laboratory, 6Berkeley,

California, jin. 1963

2. C.owan, R., Lazarus, R., and Longmire, C., L.%SL-WT-131Z, ris ,z-

.!•,;re.cter1stls fot S' h, Los Ala-os S!ertAifc Lab., Los Alamos,

Me kexico, :,irc". 1952

3. R-.S.A .eview Symposi•u,., Nov. 1?63, SR-19, t'ASA-14q9).

4. .cCormac, 6., et. al. , ,-,•.i't"Fr R. r ({•SA-SR-, 'Au. 19v.

5. Grorg#e, G. F'., ýta , )rris -r.x,'znF .-'n (EGG-B-28 17), June 1¢v4.

PAGES 3-1 Sj/ DELETED

2-24

LOCKNULLO PALO ALTO R$SrARCH LADOHATORY

* t. t . 0i . .... tIt a

-LMSG- B006988

Reference for Qhapte.r 3

1. Lokke, W. A., LRL-UCIf)-4551, 8.3diation riux and Debrls.Ancular

D3stribution C'rom Stdrfihh, Lawrence Radlation Laboratory, Berkeley,

C.ahdornis, jan. 1963

2. Mr.Corrmac, B., et. al. , ,...rfish Fr,"_ Rjeport, (DASA-SR-2', Aug. 1962),

P.C ;a . ,, La%:,,,• R .,and Lo, - Jr., C. , LASL-\V'O013 12, Pr _ t t•

Characteristic•s for Starfish, Los Alamos Scientific Lab., Los Alamos,

Now Mexico, March 1952,

4. DASA-SR-12. (MASA 1370), DL bris \lotiorn and Ionospheric Effects.

(reb. 1963).

5. Gcorgc, G. P., Starfi.•h Debris Uxpanslon, (EGG-B- 2817), June 1964,

6. \Wing, P., X-R3Y Spectra of Starfish, DASA 1604, Allied Res. Assoc.,

June 1965.

7. Hamlin, D., et al., Analysis of Coeration Fishbowl Data for Mhtion of

Bomb Debris DASA-1478, Feb. 1964, Gen. Dynamics.

8. A. Kinch, DASA Review 6G-3, p. 32.

3-18

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LMSC-B0069e8"

Number of Photons AbsorbedRkm per Atrmn

0.53 5

0.59 4

0.68 3

0.84 2

1.2 1

Table 4.1 Number of X-Ray Photons

Above the K-Edge Absorbed Per Atom

4

PAG3ES 4-i le'-Z7 DELETED -

'i

4-8

LOCKNEEO PALO ALTO RESEARCH LABORATORY

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LMSC-B006988

h 0 23 [N 2 )c t v

kn) (cm"3) (cm3) ,.(sec _ (sec) (sec)

100 1.0212 8.0012 2.1-2 3.0-2 3.8-4

120 6.7810 4.0411 4.1- 1 6.4"1 7.5"3

140 5.689 4.4010 3.80 40 6.8"2

160 9.478 8.799 1.91 11 3.1-1

180 2.548 2.709 6.21 41 1.0200 9.01 1.079 1.62 12 2.80

240 1.737 2.488 6.72 32 1.21

300 2.046 3.827 4,43 33 7.91

Table 4.2 Characteristic Times for Electron

Cooling and 0+ Charge Exchange

PAGES -v4 qy

DELETED

4-28

LOCKHEED PALO ALTO RESEAPCH LABORATORY1OCCEHI O 9 1 I A 5 t a S & 1 ACI C O0pANv

t 01O ,0 DIVISION of lOCta to Aleclap (I ollPOtAlson

LMSC-S006988

Reference for Chapter 4

1. Engelman, A., et. al., Integratcd Analysis of Lorn Term Debris Motion,

(GCA Reports 1964, 1965).

2. DASA-SR-14, Optical Measurements Symposium, (DASA-1380).

3. Hamlin, D. A., et. al., •Ludies of Debris Motion, (General Dynamics

Report, 1966).

4. Whitten, H., osnphere Above 100 kn,., (DAMSA-1539).

5. Anderson and Francis, Atmospheric Density Model, (lockheed Report

6-75-65-19).

6. lac-kout Handbook, DASA-15U0, (GE-RM 64 TMP 44).

7. Magee, J.L. (ed.) Thermal Radiation Phenomena (DASA-1917) (1.ay, 1967

Lockheed Palo Alto Research 1.iboratory).

./

4-35

LOCK-IE-* PALO ALTO RESFARCH LABORATORYL 0 C I O M I I lI I tI & $ P A C t C O AP A ? T

A 941OUP DIVISION o0 IOCINII& hltS(A#I COSOIOSASION

POI

L NSC--B-90998

Chapter 5. UkRLY DEEMS MOTION PHENOMENOLOGY

S . 1 Introduction

"In this chapter we shall be concerned with the phenomenology of the

early debris motion of Starfish, up to a few hundred milliseconds, when the

debris has reached distances of the order of hundreds of kilometers away

fromr the burst point. The state o. ionization of the debris is considered

and .t is concluded that it probably rer-ains Ionized during the early stages of

expansionr. Consideration of crcss-sections, ionization processes, etc. ir, dicate

that the debris cannot appreciably interact with the ambient atmosphere after

the first few kilometers of motion. The tenuous nature of the atmosphere at

Starfish altitudes prevents direct rnteractlon of the debris with the amnbent

atmosphere. The interaction which takes place is assumed to be indirect, in

the form of a magnetic pickup mechanism. The mechanism for this magnetic

pickup is considered. Next the snowplow model is discussed, and the

combination snowplow-magnetic interaction is used for developing a detailed

snowplow model, which can be used for altitude-yield-time regimes other

than Starfish. Lastly the problem of the diffusion of the magnetic field

.. back into the debris region is considered, and a model is developed for the

"effects on the conjugate region of a debris-hydromagnetic bubble. In formulating

the model the possible effects of instabilities and turbulence are

neglected. These effects may well be of importance fo- detonations in the

Strrfish altitude range, but we shall presume that their importance Is minor

--- , 5-1 S-

LOCKHEEO PALO ALTO RESCARCH LABORATORY"t OCaHIED 1 i ' 0 M , I t A IPAC I COMPANY

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LMSC-BO06988

""rfor the first few hundred milliseconds, when the debris is expanding rapidly.

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LMSC-B006988

The

ionization electrons are preeumably what is measured, and one must have a

mechanism which will slow down the ions faster than the electrons. We

expect the opposite effect: the electrrns to be slowed down faster then the

ions (neglectirg charge separation).

Other items of experimental data regarding the size and movemerit of the

debris include the appearance of the bright spots in the conjugate regions.

Since these are attributed to electrons and debris fcoIlowing the field lines to

the conjugate regions, they give an estinmae of the size of the deb.:- .....

The most sriking fact about the regions is their large size, which indicates

that the debris is apparently mixed with the field lines out to the edge of the

magnetic bubble which is presumably formed. This is plausible if we have a

hydromagnetic shock situation, where the magnetic lines can enter the regqin

where debris may be located. For example, charge excharnge effects may

allow charged debris to be neutralized and then to move ahead of the debris/

field Interface into the shocked region, where they may decay to produce

electrons to spiral along thr field lines to the conjugate regions. This model

will be discus:ed in section 5.4, and shown in Fig. 5.6.

I ,

5-4

LOCKHEED PALO ALTO RESLARCH LABORATORY&I CC | I 10 MI S1 |It & SI ACt C O M )AkVA QeoCU 0.VIIOk 0 tOt 9 Ito a.9C I.-I C O§Peo ,&IIOa

LMSC- B006988

A tentative explanation for the differences in the size anc movement of the

North and South beta patches is given by Stubbs (Ref. 12) in terms of a

distorted magnetic bubble.

The early auroral effects of Starfish are usually interpreted as being

due to early ari.val of th- electrons frorn Ine eegion around the detonation,

"*1

tr-4

LOCKHEED PALO ALTO RESEARCH LAWORATORY1 0 C I t 0 A ID I %•I~ I I ( & A 6 0A C I C 0OM P A N V

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...... C- B--Ob9

:'I *,! - ctic n !',' shali c'ss, s .11r a detallcl:i Starfish mcdel using the

v,-ri,%us concepts d.'vcjlpcd In the pre\,i.xat sections . The nrodcl i. bascci o0:

( r) .-. ei:c-fnduccJ pic;,up of the ionlzcd atmosphere, both the ambient

i:es,,.cre and thi icn:z:ticn c.iused by absorption of 'I, lniti3l radiat1(.n

!r':- 1 ,: w'',. ; (2) th', ,r-du.l pickup in a downwards direction of

,'•:'::., ::•'r~ldue t* t;D rapidly increa•sing donskty; (3) incrvi,'-iod

Sr':!.': z;, r:in~tlt fizi- l hc.• thc hy:'drc-ma'anotc shock situ-li:;n pr-vails

.i : !i, 'r.du i'. d,_ 2 rcisII.., tc., 3:a*;nit 'Is th• vcloclty of',., , .' .:''. '1r. 7l, Cl,, .z . ~ ,J VI2. ~ ; ~~. " c• ( 2 ""

!,, r t,?' r- Dsphre 0 ,ich ca)n Le vcri.:d betv,'ecn solar-mlninmin, nigh:-

t'.., : :.: ' l.' 1 !>:I1:'A " , "-tv". c').ditlo'i. , SincO "'ose virlatl ,,S C n L-

V.... :' l•.'t i• 1, z rulln.; l . "'101o : (5) inclý.slo.", .M{ Welpon

in '!I,' X-r:Y cn_'rr:y output, tceiperaturo, voicity .. r~d .iniss

Ci b'; 'S (',.e tJ (: Ithe r sults o! l.c,;ku (1) tis our input for the

I'. ,- thcc;- Ideis %,.e havu devised a computer program for the one-

dic,..-,' snowpIv.' :n,,el, \\hlch cin be applied to Starfish and to other

1clas, 311it.ide . UtC. (,-u: 'n. *h,t the asymmetries scae sir•nlarly

ti 1::;c cI'I• in•;n ci ;. ' .) Dv-il., v'1il L2, owvon below,

:' c,'.. the ,'.1,ieo anr thce b,21hvior of the densiltis atove 120 km :r,

:..•t ttt, tu iýn.t oi tht' solir flu;x and the local time, we h3ve used two

d vr.sity d, -,I g v t -i n I'.. [coa er ("t a , I for conJ;tlons of fight, low

5-57

toCt- ,4, r.0 PALO AL.I Ri. 'AA'CH I AfCOWIA1OPY

• I 1 ., . ,- Ii 0'I & - I" I• i I A ,.1 1 I

L:MSC- &3 069 Q9

eleted

5 S 2

-.S. A.-v:-.'-'Ctrv \:,dcz eetdfC

\,, hivc assued the results of Lokke to hold, and have divided

th.•n ssvm-'- axi~s'!'.ytric woapcn into seCVn angular intervals with. respect

to'h oni o. the verticail. Th:. assumed values are shown .n Table S-.

In ýdditic-, "or c,-,m-npriscn pjurposes , we tIso have used a sphcrizoed Starfish.

v.h3' v3?s alet:;o .how., in Tahl. 5-i.

dcucimin:;;.0 t70 extent and r..gnitude of the Froonizat•on of the ambient

atmnsphrc w•lcn %',III Le pIC.c er up by Ihe m3z.nctic-fic•ld pick:up mechanI;r,&.

Th' dbrs a1i , ie.,v and r.i-.s/Gtcr3J-an distributions are 0i Importance

,u Input .ta c..r thc. 51uowVlow C. deC.

:,. .3 (,, t ,,,..,i D,',.•i- ,':d ti,V~qn0¶1tc__.'i!d

rcr compIlter.nss tno computer program has mncludvd the e.f!cts ot

i non-t•,t earth (in oid-r to determine the dcnsity and magnetic eld strengths

as :. 'nct.on of location). ror the rragnetic iIS. , wo have assu-vd a simple

- ' dei t or thc enrih h• tield, with the magnetic latitude of the burst

p..i.: 's an input pnrimeter. The orientati¢cn o: th: wcuprc -wls with re:,pcet

to the ve-rticJl is also included as an inpoit p3rncmtero

L.C.HNCEO PALO ALTO IiLS.A.RMH LACORATORY1 0 C I^ I If U I t o t II t # PpA C e I 'IN t h t k

A Glove *'',,0 C1 ,I.44.1b 4 *.•S.9.i 40"0648 1.O

II

, MAGNMTC UNl'.

_ -- - _- -

\\

\0

"rig. 5.7 Geormotry of Hydrzmvinelc - Lw.rjv BublAe

"5..-71

LOCKELD P'ALO AL.0 RIGNE1'C L.A;ORATO F

17 1' 1• 1• U \ 1J

LMSC-W'C069t3E'

* I-. I " •,

rig. s.B Gcomcti-,' of Detailed Starfish Mlodul

5-71

LOCKHE.ED PALO ALTO NESI:ARCH LABORATORY1 0 C I N I I u I a I- A , 4 C 4) a N v

• ' . , , , . A

LMSC-•BOOCS8 E

- iir *•.i •,ýh, v.'hcre the C•iZUI IO.S cf " , ,, , ,ic te that the fis"'tcn

d tri .. s cc:)cer,tr,'ted in a is;c nt .. , ;C would tlurefo-a e::c; t

oi th,'. b1 sis of th• onalysi. abc.ve a :-0re ur,0,o: initensity at the coniupate

rugion as a furctnz,n of x in'.i y than \.we w-,'-uld get if the fission dctrisc

were unliormly distribjted throuihout the hydromnagnctic shock layer. T7nre

cýnsidcrations will hold only cs long as we can speak of a hydromagnct.c

shock region suirrouding the expndcing dcbris. Oncc the dcbrit vclccily.

hac slowed dwr.., the simple pic:uro above will no longer hold.

5.1 1 •ui.r.c,. :

rn,,;ch3ni.m Svcrn" to exist th3t can slov': d!,cvn tre cxpinding shell o, C'br.I

sih' Z1c.-vation thit the Ccb:is w..as in .c".. slcv'ed dov.-, and hat G

mz,dcl v. ' an apprecazble irt:ction (c~bout l.,£) of the detris bcing p-c'.vn up

. to fit thc d ,:,i fr t';r first !vv. hun. red .'n.libeconds itndcnttn th.it ,

,:c-:_,3rnisni mus" o'Peate to piz'-. up *e a.,c;'.t at•,ospihere. Th( mes plrsibie

.ourcC c: this picup mecnanism is th.e mngnctIc held.

Using tni'; mechanism, eo:nbined with a self-consistent methcd I[r

considering the i,;craction b.tween the debits and the ambient atmosper.cle,

,-:d; to n !r.oiel vi.tch can be usc.d fur dccrxbing the early debris enotioa of

Sorfih:h, ahid wn~: can be uýcu for pfd:ti;n for other 'ititudus , da-'-,s.

S.:'eral ci these cases which m'ny be of future interest are considered in deta:l.

5-73 £ -7 --+-4.

I.0CCHC,:D IIAL'. ALTO RCSCA14CH LAV'3'::4.fORY

£ **Cv * V • , Ittn• C* ,, }: I-.tt i, 1 * . ! , ,.' , .&,jii •

LMSC-BOOG688

.. !

S • : ' " i I ............ ......" , : : :... :• ' "-.......... .. ---. .. ........ ... ..... O.. .... ..... •...

.... .. I •.. ..S. †.. . .... . .... ...... ]: .. .. . .................... : :. .

.: ... .. . . . . . . . . . . .

.: .':: ... " . ...... . . .. .. . . .. . " ...': ::: .: ::::: : ... .': .".. ..

S......... ... . . .. .... .............................. .: .- .-..'. . .. . . . .....

...... I . ............... .

S. .. ... ' .. ... .. ..... . ..... .. . ........... . . ..

7- 7-NA I 2

.. ... ...... .-. .....

S.. .. .. . . . .. i . .: . : .. .. . . .... ... .. . -: :.:... --.

. . . . . . •. .: ... .. . . .

.. . .. .. .. .... . ...... . . 1 ( ,.)0:. : ' 2" : : : : ... ..: " , .. :....... ..

S. . . . ; .: : . . ' . . . ' " 1 " " " " : : " ! " : . . . . . . . . . . . ..

:: : " : " .: ', -: :~ ~ ~. .: .. ' ". " " .' ... ..i ' : .. { : .. .: .: 1 . ....".

.:! .... ]: : .. .. .... .~ .... .7 ..::]: i ........:]i~ ::] :i : ::~ ]:~~~~~~~~~~~~~~. .. .? ' - :. . ' ' : . . . . . . . - " . ./ . . . ;. ...': ... . . .. .. .' " :- ' " .- " " .. .... ". ; ';. :".. .. ...........

• " . .. ..... ..... ...... . .. M AG. N ,:::

FigJ. 5-11 Starfish Un~der Da3y-Solar Maximum Conditions

5-77

LOCKHECO PALO ALTO RCSARC LAORAd,L . 0 .... I 'I * U I " .I I sI¶ 11 1, .I -A.rI0 IA :- " ' AT U AW 4/.

3Jo :: i'T~ a CTT. :'::t - W#T- 't -- :TT. :-I .T IQ l t'l~ t t• T :m,6 00 1 14E iT ::! ) .2 ! T7 !

LISC -B0039.z5

.... . .. .. ..* .. . .. .. .. . . . . . .. . . . .. . . . . . . ..

.... . . ... ..... lo;..

I. " , ' .-. - .-S. .. .. .: ... : .I . ....... ... .I : : . : , / , , -j . .. : .: ? '> , • o o :• l .-: ..! .... • .. ... .

, , ., - , /.I -I

S .... .. - : .. . . .. . ..

If X•) k m .. ______._

..... .......

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" "".. ...... . . .... ...... ............

I/ / ' , . " ; . :

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... . .... .. . . . --

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..............

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"" " ' . " . A " l;u": .

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I. I . ."• . . 7.., • . .

I -. .• • • i... . .

• 13"10 1,t•l" .r. : .u.:

D'p :.olcjk - 32?Y Iay-,%A~jxir.m Con.d'tions

1&OiCKHErV PALo. AL.TO Rc[.•lf:A CiI LAtJO RATORY '

C , ; I i'* , l5 jI Li5S%.% 5 * es *. S.. *' I '"*. A I.t IJII

ad4

9i

Best Available Copy

. , A., LRL- UCID-4,51. , . ; '!ux: ,: Dei . A(,._Lr

... l ... loll'l•m •t.r • •]w cn 1%R,idjotion lil.oratory L.r6.,

4 [,ire. .lr: :trJaCl. jllu

":1 :;. 'c':': , ""T. P. ond Shu.lct . I,, * -:t.•.: -h.i".rt l L. n .. Iela n-

"- . .• "*, (Junr, 1c W)

•'.LJ.. O ... ..I.:.... . .

b ~ ~ ~ ~ ~ %n s"/'' l.[•":: .::".son E::-'c':¢ , nt ........t F. Oi-2026)~. i': . ........ * ;* V¾1 .... cL- 7:.,~ ~ L;, ' .-\ S'- 1?, I"

L..:. A. • -n ', iw, c. xcx1 co, N 1w c . 196 2

7. ~ ~ i e....:=r. C., PM!,.;ma' P h %!,i : r.e

A. ~~• ....... Of. (DP. 6 5 S v G 11 2"U. l'Jts |: ,,: * . A., * e. l.1., *Stu.J•,,. of t 'bcr:s ,, :~.-.._ , * . , SS 1 S

Jill. 5P61.,) .

9. Topc, p¢t, * . I., , ~t. *:l1. j.i:rly'-T=r;'.' T i ',r .'. • •:;,_ "', oo f;c [:"

10. Cv-. v, G. P.. id,..h I)br ,"i '. ti' ,,t cr, (n clG-B-.•'17) , Ju'w 196(4

LOCK04tCD PAL.O ALTO RISE ARCH LAiORAlORYI # toU I I% III % & t &A I 1Oe* &A%

*. '. O * t 8 I* * I= t o t @ * @ al*I e . . f16*.' S a . % t

* .. ... l2~. 2'I'. I~ zt~i.r,. , ,-

* .. ; DL "''r 'tiz* (D s;,; I747).. . .

;*. ".,- .l d ¢ 1t~ . .. rofn'.' :-"i 1zur•'.' 1. *. ,479, 4'J1 (19C5) *

I& u

FDCt . PALO ,.LTIO AL.SE.An'C.I L~nr:oRATORY

2,101",0- P 9 A9 ,

C,.. Cr E.I'TA FATCHES AND LATE-T1MC D•IPRIS DISTRIBUTICN

~.'

Tht ',,trs re:.J i,-.J b.v. 1!Q .?C CTCjfnC_`C 1101d, so the hor'zont3i u-xte'nt

dei.1.m...... , by the extunt of the debris distrib-ition froem

.- , h'o bevt':s mrv. .,ittc . Vf tO.c debris i!, confincd tgo a d finte volu:c.

tbe 1(,n-i.;e rcic in.L v.'Il co',,r "i c:.rrcspcndingly dcflni:e area . This disc-hi kc

Icn.zed •hycr is frcqu,.ntly cailed tho Lict' patch or beta pancake. "h~e b~tas

eIt:,'d nm tho u;AcrdJ cr,•.'oi will folaiow thi' ivId over the equator 311ý ir,31e

,'•nother bL:3 p3tch mr. th;e oppos;tv h!rnaspncrc. 'ilhc loc"icns el the Octa

p.itchez aru called the cor-':g•ct r(jions. 'To Afrat apnp:ommtOn, neglecting

both n.itu:cil and bomb prod%;ced asymmctrles in thi magnctic 1hed, the bet,'i

paitch,_-, in thu northern and southern conjugteo togions w,.ould be identi cal,

The q.omctiy In the con)ugate region nearest the detonauon point 1s repre-

se-'t.c Sc.hl|maiitIcally in rc.q 6. i.

LCO,'KIHtUO ALO ALTO nL5LARC14 LAB1ORA.)rjY

* '.. ?.t...% ,* 11 ,I.:,I CO P&.,

L.'SC'-B90698I

/ MAGNETIC

/ FIEtLD

//

/// /

////

/ // /

/ // //

'A /loo7

Fig. G.1 I-eta Patch rormation

6-2

LOCKHILD PALO ALTO RESCARCH LA13ORATOFAY* i u ll c a a * .ID iY . t I I .bk IA t 1 . n I v

LN¶LC- r.)O 5988

rcr :! r. . dc -ri s c i strt)u..':,n. the i 'iza:z n at rnu&it:..j att '.UjLAU 1i;

, , th hb..'toa rxich can be w:,aied with a f3ir d~gjrce of c. r.ty,

.ct tD the asbu-lpt., t);' t tlne b,%tas move irdepcndcntly ol one Can.-t!*r

,'IJ losU oneiJy onIly 1y ,Aulcnntr'y int.eractions with air atom.s . Qustions

:,s to the acciC'rcy of the c. lcujiatios arc raised by uncertainrtiS I. the rnodCC

It~c3f, nac in. )-reuinr zne',nistr., p:rticul~rly under the pOrturbid condituons

Ic Lo expcctca iollowing a nucicar dctonation. for Starfish the cistriLution '& ;

•.•r f~ - v-ii ):,z',',, arnd Lhis raises iurmncr questions as to the appticabilit) 0.

th.2 ui::'t,1 ".zu,'l cutlincJ abc'.' .In tl h cih ptor the expenr:-,ental dat.3 L'e.ri:•-

, I. Si' -i ,i i ,1r' . ;Xa•tP.lC, patchc.% ore e: 'ni.ed t3 Ge t::::;'c

* :.k. > .':t& L . ,,Yli Li:, s• ::pi ::;c~d.l p:Ovides 1 de'•cri' .ti't ¢, p LC:' '

.: c- , . o o !his it is ail•o -.,ccssnry to Jiscubs th,, dwia on I.' t-

. " i,: ch Fcr.".:'.•t io n 2' tho Nc'rt horn Gc•'.)uq3t. IKoicn

..- :," .'il1 I d."', Onl or t.. ' 0' I hc Staf'ish -'01a patch il tn .e

_:. I A c'.:• ;, , ", . , C: t) !;,c :-n miven bv 1.;%$ (RFc, . . 5. ,

(.) EGJ G (rlcf. 7, 9. 0, 11 , 12). Photoaraphs were takcon Irom. the.

!•I Ir, lslbr.-;i .n, d fro-n a Ircralt in tne nes1hbor'nhod of the CI•. Since

,. • t-tuj:. rC e pun-,tt : is bel w. tlhi ho.-ILon fro:n lLt v..-1, , ..31 4i•ac:

;.• , ; 'r evldcr t1I•C itA, 0 r " 11.1011 r.I'qaoa I {O''iu .' :, lh ,

JG I't-lr, hs v.•.were t3;*.: Ly cnineras abo.ird 1\-.o tn -i.15 .i.crift,

A/,'C .31.14 unrj %/C 531210. A/C 53144 was due inignctic north of :*.ý zuio.t

at , horl:'ental distnc,- of about "75' k,, while P/C 53123 w3s rrm,''tg c ei't

LOCKHLI:'O PALO ALTO FItbAHCAH LAEIORAI4OtYr (" L i t,, t ;, - - I I • I1 % A 1 0 & - , 1 , 0 , ,

-.S.S .C V .

Se

L.MSC-BJ069&8

t~t hc ,zc l rzi._, of iLxout 350 ., (Ref, 10). T;c. LA3L cameras were

d a OKC-135 ot 3,ott 1J. km h i•,zo:;.ti ran:.c from the burst and Is°

t~zt ',f r.',{-.ctc ncrth (Ref. 2, 3). Posizlln d3u, !or thc three aircraft at

!h.Xh timv arc glv'-n in Tl,,lc 6.1 (Rot. 2, 3, 10). Also given are the coordinmtes

of the intersection with the 103 km altitude layer of the field linc through the

burst point as calculated from the Jensen-Cain field model (Ref. 13). Tho

irt, : ,nferratlon Is shown graphically in Fig. 6.2, together with the location.-

cf ,. zero, Jo.'hn-ton Island, and French Frigate Shoals

r'3 SO 1. ," on j'vC 53 3 1Z0 -1 -p.-'.t at

r; I 6.35U C 6 3 1r A8. ri

i': r.rt r- n,: c ,23 :.34 i 3-, (,:c l i,. :,

7 r -. irn t:.-.,i ;,tion 2 . 44 .9 1H ._

1'bblc 6.1 ;,Ircrift Po$itlons in NOfR at Shot Timr

6 . Z..1 LA ý.L D.it a

1h._- LASL uircraft •is. abouut 50tO km from tho conjugate rejgion

.-t ,hot t;, . 1.hic,t'.Ox,,aph.• %,':(:re tl)kcr Wv.ith a 1)oo ,,l : 0'e a h,-M r,,1 M'

,r.inm'r r3tc .if 3(10 pur -,cc, and two Ni:.chell ca:n ,ra! w frlinin; rnte- of

24 pr .rc, f.lack rind white films wero .eposcd cui tho Phctosonics tnd one

of the MtcheIl cnm,,rns, and a color record wis obtained with the zccond

MI Itcl|m. I

G-4

LOC~kirwi VALO A'.' ASACHLnRAj.

S..~~~~............................... I. ... "

S. ... ...... .. ................- - .- . ..-.. . . .... : -. I

i ,-.. . . ... , ...."•' -.. ... . .... . I.

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:' . . .. . . . .. . . . .... . . . - I.. . . .

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-: . . .. .. .... .. . .. .. .... ... .... . .......... .. . .. . .

I I

... . ..... . .. -... .. I. ... " .;.''r -. , '" -. .i .. .... . . . ..4

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:" ,...... PAL ...... fl , AI Ij . . . .. TOS . . . . . .. ....... . ... # AI . . . . . . . . .

LM SC- .0069 8

Prints of the first eight fran.es (- 0-3C' msec) ano frames 19 through 26

(A (,-93 resec) of the ilhtosonic5 film ore chonvm in R-f. 1 . The first frame

ovuexposeJ anc shov'.- no structure. C-% tre second frame a br .- spot

-has appeared in the neighborho,>d of tihe NCR. The spot appears to be a r3,

colir.-:.ted along a direction con!--.,'nt with the direction of the field proiecuou

onto theo plane of the photograph (Ref. 2. 3). The ray extends to tho b:ttom

-f the frame, and hv'nce thre ýcit.d rcgion probably wxtends down to ailt'iuos

outs.ide the fidJ of v,,,cyw of the carrura. This is consistent with the stotc,,gnt

of tioerlir. (RLf. 1) t;>t the stoppiv altit;ies for averzge fission betas are

Let5,' : e c •'e•,l • : * :. ' ..• , ..-% , .z;:.tc , tr" t!. •:tL~".• 9~ the c'1:rei3

hRrizon at the NC' is F.S ý.m, Lut this vl.:e i- questionble because o' uncc.t-

-. n e in a .,r p-intirnq 3n7lus (,Ief . i{'1).

In subsequent frames thu. i.umincus t , c-r C , r te Ccn ..- ,t,

point ',s hcrizonillyi .

e c..t ,Liter o';.; t;- , o,

jr''Y..'h aof thu auror) ciucrLa:•es, -i,,antinin.g god corr ,latlon with the hO ri;:ntcl

r.te of growth of the dubris cloud. .F - 25 mec tGhc aurora extcnds b-cr,

the right-)zinw cdTe of tho film. Di:',ensl,ýi.al d.ota ol hoth EGG anI L;SL i.re

shD'\-,n in Tim . P.3. :m it. I ,, ::' i ci - 3%' ir, .t •,' m.,c (K.T. ý', 3) 7:'d

a nnaxi!nunm Eenuwhat ~ tin Y ,. .) havu also Lucn giVun b,, "nn.

At about 65 mrcc (frame Ij) the P.Iotozunics film shows th ap p;r:,jn e

of a small bright spot near tlhe pzint where th.e rig inil. rx, hrA . .pi..,rJ i!,

the sc-cond fran,., ThiL brigh, rpot is seen against the much larger b-t ics les

A4L -7 7?i~rLOC'HILLI) F'At 0 A.t•w fnlsZ"ARCH LAUOIhATOWYI 0 •. I " -" i $ & f I CI S P 4 1 p* .p,: I ' , ' t Cl,{N ,a. . 11- II .S I I I (*I*-l&tl,t l b

S

S P

LS- Bn 0 69 98

i::t .--c lria,•s area to wh~ch the orlairal spot h3.s now qro',il . Drom the

. J I:uts it Is difficult tD tLll ruc: 1-,, thu r chavior oi the ro.. spot

In J:ct ,t is not obvious from these prints that the spot was not present prior

to 65 - r.d ,n ecamc apparent at that tume only b~ecause v! the decrease In

b~chgro]-d ir~tensty. On the basls of Inspection of the original films, however,

}{Berlin han stateo (Ref. 2, 3) th3t the ,:ew patch appears at 90-100 km, that it

f-,rt cxpan•s with little increase in br~gh*,.ess, and that beginning at aboot

120 ms,: t-.ere is a rapd expansi.on anr a very sharp iticrease in brightness o.

this costr. a'lrt'.

2it.a .,l. c-i-.cra ýield: of view extended to lower altitudes, and

lncuck t1*~ ~ 11'. I the NCý- %vn.rQ rnxirmum '-1 e ncrgy'v~o. c,,'-tteil. 1hcz: !rRmni,) rzte of 24 pýrr acc correspondý to in trferv3i of

42 -i.ec between irz,.es. The shutter sectcr of 1700 and the frar.itn rate

i ::ij 2r, exr:;s-jre tme cf zibut 20 msc.c. Thus the Urst frarie could be a ý-70

'. ei xc2-posure 4- ma--oc (xposure, or anything In bctwcen. A:. appr:.';-x•taZ

;,_,;o tt.' .fýr tIne M.itc-.eil !ilr..s has been es1ablished by co'iparIson with tvi.'

r".'t•z:,i. rc:orCs ( it). ! 0). Presumobly the time Libels givc.. these photos

(ReA. 2, 3, 5) :rc bakcd on this comparlson and refe: to the time at which tho

shutter closed

T7.-. publiuhe= Mitchell phctos comprise frames 1, 2, 4 and 6 of both the

color :n bEack and white films. .All cf these show a largo luminous region

whose d:nensions increase with timo. In frames one and two of bath rrucids

a luminous re-,aIon which is somewhit s;nallcr And much less intcrso is app3tent

bcneath the :,Iin bo.rce 0• light. The bright spot which appeared on the

Photosonics film at abnut E5 rns$c is not visible in any Hi these prints.

6-8

LOCKHELO PALO ALTO RESEARCH LAOORATORYO k til. I I, I IIII I;- * (* (1 OSI$ AC 0 a aN I

r - .9 ofvl ifk - 4 4l| g l | { I I 101 6.1 (0101)4611011~ll

LM-SC-E p6968

.. . . .... .... •: ,. ..P•' • ' •

*p.: ,. t;ne haap c-.

t e C.r-.e I c 1 S.~ s u m r. V* C 7 1 1:z~ r t.1'y t -0(

. .: ,re " ab." "-. 53. .e ) hA:Cs -.. ".s 75-1 , km (..of. 2, 3),

='.4 1..:• ('. . -, ) .." 95 p,.u .,t. . "), - .... l 'e• c:. .. • .. r..erred valu.2

r3-::' • r .- .7 ! . -".c""l..-.' *-' " Z'3 I A : ' " n Ct'-.5 • an

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i:. . s S C. . *: ",.1 Cf GG (

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.•:.,.-:~ ,! ... 4 .'. A c "" dn t• hc , o ~ roduced 12

~~~~~~h .... ;.- n• ,.-, .. t . .':im : plc . .Z. • ,..h ap;o-red at - km-.• ,,• ..

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films. c:!.. I-, .-.-n 0 c.n l '.ic t*a'cu. ,.-.t.t ;6'0 S3,142% w•-.. chqht!l ,. ,,.,y •.. . . -

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-.! :2: " r., t over ro .ses a',' I ,. s'lh..-ek. '. a.i t .

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• -'3 2 - " "" ;', , :: •'. ••... .,, ." •,: ,*~ " r [.":"• I'. "..*. *; ,..'.1.. A

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II.,r .'z':t i~r ,', •" I ::, ',•• to }'. ,•h•,, 3 ') ::' a ~ th , l' .•. -'• .,• '•t• S .5.ls t,

,,

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a:.c,._tt dt h ýh PIt LAQ, and ntIlI other strcdm,,rs appear at l11rt t ti es j(;',2f. 1),.

6,2.1 EGG Datd J

NG photographs of the NCR from the eastern A/C 53120 were

obtaincd, co the only useful NCR films of EGG were taken from the norther,,

./, $31-4 (lef. 9). Pubhshed photos comprise several early frames from a

rh~tosonics 1'ýB camera running at 3G0 frames per sec and a Traid at 16

fra.mes pe- sac (Ref. 7, 10). An unidentified photo at 15 msec (probably

'ro;' t'e , -h .csoriiz; i,:•) • cw In Flef. S. Useful rccords were also

n•_I- ze; oU11 u~" 7q,-vi; ' Ruhai,: c-nera d!.:cus.ed !I n lhe pr,, c~r:::

section. The POR (0a-'. 10) indicates tnat aurcral photographs were obtainLd

3r, several cameras with framing rates of 16 per sec, and also on a Photc.sonies

4C framing at 2309I pc: sec as well as several Robot cdmeras taking one frame

per second.

The earliest exposures published are those from the Fhotosonics 10B

cam.era (Film. 93227, framJng rate 360 per sac, exposure time 67 psoc) . The

first frame of the record is denoted frame zero by EGG. It was overexposed

and contairns no useful information for the NCR. The next frame, frame 1, was

exposed at 4.1 rnsec. The expanding debris is clearly visible in this frame,

but there is no detectable luminosity ftom the NC. (th!L contr:.dict.; the p-o-

liminary report in Ref. 7 that the "A aurora" appeared in all frame of this

serien, but was cropped out in preparing the enlargements for publication).

T'ram( 2 (6.9 rnsec) shows the beginning of a lurninous'patch in the fore-

ground at a position consistent with the Intersection of ti.e burst-point field

6-12

LOCKHEC• PALO ALTO RESEARCH LAPORATORYLOC Itga 6 IIS1 1 ACt C 4)•( s M A h I

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t I .e r L -'..I s of t lI s s e rie s w e re g iv e n a s 1 .4 i ;sec lite r In IR c f . 7 . P re -u In a biyv/

the dillef rnce it labellir.i .results from a more accurate zero time dutermination

s in c e t h ,, p u bi:1c at io n o i R1 1 . 7 .) In s u b s e q u e n t fr a she s t h e p a tc h c o n t in u e s Itc ' or e ,.', v.h i le t h e p e a k in te n s ity v a r ie s o n ly s lig h t ly . b y fra m e 8 (2 3 .4 in s e c )

the ,'e cf thc upp er edge of the p3tch has Just rcached the burst- lcirt

imcv a. on the hl' :: p ' fram .e 14 (-•- 0 ,rms ..c) trie patch covers the Cntrc plotei(flci. 1 7).

T h .e c u a l lta : ,'.'c ! •.jt - ,r e s o : tif c d e b r i s x ,ra "s i o n e x h i b it e d L y t n - r5C ,0

fil: ". 'r . X.'."•una Lc . .ti -s:l ,r to t h-ifr.c se n in tnc L.;SL ','i i~lt:. .

Deleted

A I t c ue : ' . , E G C :r v .' ( r . .i . " r 3 i n r i g . 6 . 3 ) a g r c e s r a t h er w e l l w i t h t h e

LA .ýL curve. T i-n d:sc ro p T.ac'.., botv. 'c,.n the tv..o EG G curvcs has not beencxplaircd.

The end point of the initial aurora (6 msvc) was observed at 21.6 °N,

1 C ,. C, , T -.c auroia extendcd in altitude from 70 km to the bottom of the

frarn e, v..hich corrcspnnds to 5. ;.!n. Thus the Init~al altitude range was from

< S0 kmn to 70 km (r~ef. 9, 11) . The nltitude ot maximum radiance was initially

66 kmn, but iiicrossiA rapidly with tiimc, while the altitude of m3xiinium pi.ntrationi

varied Slowly (Wet. 11) . The initi.)1 aurora was observed to expand symminatrically

6-13

LOCKHEED PALO ALTO RCSEARCH LAGC'V4ATORYa aI 1 0 14 , S I i I S A I ACI C 0 A %•

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in 'ý 1iz,,itudi:'aI diruction- obo~ut a- 1:\cQd Ccrnit .Asubsc-4u~n..tamimI1r aurural

e!:'ctw~ -.. :vrcdto occur at asorn3what hiqh:r aititude h-gqnnrunq at aiout

De~e~~ . ~ a-~,e Cu krit iitudc.a c. fuicticn of

trime Is sh'own in Figs. 6.5 aind 6.6.

612,2.3 Analysis and Interpretation of NCR~ Optical Data

The dist~-e ~'-.m the burst ooint to the N'CR wvas - bOO )km.

Th C t r 3ntr, i-r .1:2rtackCS movin, ot the speed of light is 2msec for this

di.;t Dell-,: -~11~ f'ssion bc-tas have vrnergles in the Mc-V ran;e, arid hence

trav.el ~t'ryc ir ly the spc-uj -Ai lich: . If thv b ta;.re abie to leave thc

hur-st rcyicnr znho if-!~ to reach t:nc NCR without losing m-,cr-' of

their energy', as t swnple ntJCi !-upposes. a beta aurora shouild be obser-'ed

to bc-ii: a.t zibc~ut 2 zc:

Tb~ u~jr~niýq f 6n au~riat a)-pro:um-nteiy the expected position

is olrr(ývud in th-e earliest urz:Ilo frame, the secon~d tra me of the Photo-

sonvic;ý rt .:crd, 7ý;:- f-,rinc'v. exposed somcwhure in the " 7 rmscc intcr.'al,

,,nd hernce shows that the onset urne was prior to 6.7 rn,.; This is consistent

with the simple model, but dcus not, confirm it. The first usable frame In the

EGG Plhctosonics fi was exposed at 4 .1 ms2c aind shows no evidence of

luminonfity In the NC",. The nuxt framec, 3t 6.9 mscc, shows the begin~nings

of a lurr,-riý.us paý.7n. Thus it !ýecms that the aurora first appeared between 4.1

and G.7 rn'cc, ar~d rict ajt 2 rmsec as direct moction of relativistic betas would

lead one to expect.

6-14

LDCKMIýALV PAL.O A-TOc IMSE AtCH LXLIORATORtY

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dc1-r ~ ~ ~ ~ ~ C , v ti.c L c..\itho !lghc :,,,c: vit thos -)t t hvi.

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0ý0r.s ncl-icng v'imbic iirht wi, n zi f ixL.. fluoreŽscenc 2 effizierncy, t.hen dut ing

the firs, ý.c-corn the *viszitb- rnov.lur fromn 5 Etnumultion thould be zon'suint.

whIch in tj-: sn:wld iays~ tho square~ of th,. horizon,1 rdi

Nn-;tlic.r tim! power n-303zurAnd b% I.AS1. nor thc radimn~c macoured by

ECbl:hiv~us in thc prcd.-:,,-d.rnc.

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6-2

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LMSC-B0069H6 ji

6.3 Eeta Patch Forrnation ir. the Sou,.hern Conjugate Regic;.

Ph.,tcgraphic data wvrc aiso obtained b-, EGG In the southern conjugate

region Rc. (7, 9, 10, 11, 12, 141). Camera sites were located on Samoa and I7oncga.epu. The fastest fra,!ing rate of any of thc cameras was 100 per sac. =

Cbser-a3tions were hnmpcred somewhat by cloud cover. Ry triangulation from.

these two sites the lower end of the end of the initial aurora was found to be

zit 17.220 S, 175.S95oV. The Jensen-Cain projection of this point gives an

altit.de of 3LS kn over yohrnston Islard. A map of the SCR ts sho\•tn in

Fig 6.8.

S• IV

Er C1I

I

¶1

6-26

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6-27

LOCI-HErD PALO0 ALTO RE~if-ARCt LARORATOf'

c 0:,

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6-2 '

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1-f

While the cun•,ez are similar, a larger traction

of the hight appears to corem, from hkgher altitudes thz, n th'_ j depo~itlon

curve; woulci indic3to.

Mleasurements of the growth of the aurora, both In latitude and longitude, ,

were also rn:de from the films (Ref. 14). The latitudinal expansion of the initial .I

(8) aurora was symmetric, with an initial expci.sion velocity of about .

6-28 I

LOCKHEED PALO ALTO RESF,.RCM LASOKAIORY "

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i, 6urnimr;, tho beh\Jcr of the • rora r lh,, SC .z Scem. 'o ha',u cc:',- . •f•.,d

to thsootic•.1 e.l ct-ti.'nr ,mere closeclh-n the .XCI ýuror, Thisc lends

some: !upr.'rt to the h'.pth¢c-i that tho betas bch",,,.cd as cx:pceted in !he

nfrLh, but th.t interp.-r'tt;on of the northern dc ta is coniued b% th.e arrival

o! cb... so O .ifter the n onsct,

Dv V! ,te C4

N 8 in-i;gntic pi.;ton .v;hic) soopcpd a large fraction of

the arnb.ent oit ape1 ars to have fornucd for these ptiticles initially moving

I parllcl to the field.

1

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Tl. d.r~cns~onq of v.'hat Zrc assumed to be Leta patches co:relate well

\'ith mensurcd dirne:'sions of the c>:1paning debris. This appears to indicate

either tiat dubris (in particular, the fi!sion frsginnts) Crossed i:el lines,

or if a mo-gnetzr piston ws formei, that the debris wa-i well mixed with the

fieid ,n the piston. The dimensiors of tne southern beta patch were smaller

then those of the ncrthern patch. This is probably a result of asymmetries of

the magnetic bubble, as suggested by Murphy et al . (Ref. 15)

E. .4 Dclayc-d Neutro'n Nleasurvmc-nts in the SCR

Dc .. n --', .u'.rons v.-ert! zi' bsu, d A s pzrt of .r!ojict G .5B h%' c',,nters

•I'k.:rd tv.wz o., 1,,s,F316 ! ar. bib , A ltt ooe Z2 ,.- :a.ttou. : -'n z, tic

two m~~eo~ shot ti:me are shown irs. Fig . 6 .8,. Tho e surc r-cints and their

intcrpret-ttic:; h--',e L,:cn discussed by the iITI group of Stinzhcomb .

(Ref. 2t, 29). Interpret tion of tnt dta is- hampered by' uncertainte in

cco1ibr:,ti,-:. : t.hc coun.terts, both nbsollute calibrations and thce relzi\'e

calibratio:; o,: the two counters,

In spite of the cahi,ration unc.:rtair.ties, the data leave no doubt that

declciyed ncutrons were counted in sizc-able numbcrrs, and hcn,:c th.3 a con-

sidernbil r i:iount of fission debris was transportcd to the SCR . In an atter:PL

to ?cc,.junt for thv r,?ltWve countiln rAte! obser.ved at the two stations,

SztlnchcQ2,:'b eL 11. hctvuc doe,~ or, appr~xivlcttý ilQ :'.; transis-ct coi~culotioC;i

from a poi:it source o "-ons. F,,,:jure ot the rather.iarg- dt•:taca bctvceen

the t. , bailloons, they find thit the relative !:ount~ic rate cannot be lit with

a point source unless it is abov'! 20, ni

6-32

LOCKI.i'r r PAL U ALTO, RESLARCH.-4 LALDDATOr4Y.1 .t I I) - I t 1 a s - A I I ( C. . 6 . 1. 1

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I.MSC-Bo06988

The most favorable location of the -imt source rcquires Df the

fission fragments for consistency with their best estimate of absolute

counting rates. A point source in the neighborhood of the region of maximum

) counting rate found by D'Arcy (Ref. 30) requires an altitude of 250 km and

of the debris for cons'stency with the neutron counter data.

The neutron data have also beer, analyzed by Hamlin et al. (Ref. 13).

In this analysis an extended source was considered, and neutron fluxes at the

counters estimated by a multiple scatterina calculation.

1 .. '

V

6-33

LOCKHEED PALO ALTO RESEARCH LASORATORY0I O I C M It IC. 1 1 1 0 1 1 1 & I PA C I C OMlD A k 4

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LMSC- DO 06988

6.5 Delayci ý -Ray Nme;.surernent in the SCR

!M.Iasurements of )-ray intensities in several different energy channels

were rrade with equipment aboard thý- Pro)ect 6.10 KC-135 flying from the

Fiji 1,lands. The flight pattern of this aircraft is indicated in Fig. 6.8.

Analyses of these data have been published by D'Arcy and Colgate (Ref. 30)

and by Manley and Carpenter (Ref. 31, 32).

V.•

e I e ted

The 6tbris distribution given by D'Arcy and Colgate seems highly

questionable, since the ert.re aircraft flight path lay west of the magnetnc

m-r:diar. . Estinates of debris dens. y were based on a simple attenuation

calculation, although photons reaching the courtcr after one or more scatters

nrob•.blv m;,oe a sianificant contribution to the ccunting rate.

Deleted

6-34

LOCKN•IF, PALO ALTO RESEARCH AIiORATCAY TIt.Lfadtst..' 0~~.11-. of '310 1 '9 -oIf 0.4 t 0 .0A*Og O..

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'he I:os. r.:.-ent analysis, and the definitive one, is that of Johnso.n

(!eff. 2 ). In hi 2rnalysi.,, Johnson attenipted to corrcct for synchrotr',n

noisc:, E and F rec'on .býr:.tio"o, 3nd antenna patterns. He found a minimu,n

of unc.e-taiity in the St-3ifish cato at 10 mii. By con'p-.rrg the obberved

att8uu-V*r, v.'wth- p,%dictier, s of the \V'EPH III code, it was posstble to infer

an areal delwis density over the various r~ometer statioýnr '. r.

Deleted

6-36

LOCKHEErD PALO AVVC RESFAfCH LAnonPATORY

1. 1.O 0 . I . ' 1~. .1 1 11~P6 £S' :14. C 1110gtI, a: t(1

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I

6.8 £Summany an~d Conclusions

'Therc: is no reason, either theoretical or ..,xpcriment'il, to do-.Ibt that

betas followed the magnetic field to tho conjugate regions, and maniy reasons

6-38

L.OCKH4EED) PALO ALTO flESCAfCH LAeonATORY1 0C ANJIftHIf A 1 5 S I 1 £ 1 AC k COM 0AM T

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I

LMSC-BOO6988

to believe they did. The LASL photographs do give some indication that

th h.otas deposited their energy at anomalously high altitudes in the NCR.

Interpretation of these photographs is rather difficult, however, becauseof the near-simultaneous arrival of the debris and the relatively slow framing

rate of the camera with which tho photographs were taken. The EGG photos

offer some substantiation of the !ASL data, but they also are Inconclusive

because of the unfavorabla line of sight of the camera relative to the field

lines.

Arrival of betas and debris in the SCR were further separated in time.

The EGG photos in the SCR Indicate a behavior of the betas more nearly in

jgrvt.-.:-nIt wiih L•Ov'cci¢cal expeczations. " c-, , c.;ecte densitý%net--,, of the

SCR films to provide total visible power versuo time would be desirable.

Deleted

6-39

LOCKHEED PALO ALTO RESEARCH LABORATORY -4". 1. , ,1 0 C Ia I 1 0 M 1 % I I I S & $ | A NCI CO .0AN ,'A.

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LMSC-BD06968

.1

I, is h,,J te reconcile these f3cts with statenmcnts tc the effect that

th:, e effects ".' nucn less than expected, since the cxpectations

worep un~ ly b-zied or: the pancake model vh!ch assumed spherical expansion

an.d ) 2C kr.; depe•siticn. The basis "Sr such staternents was probably the

rr;eativcly sr.all attenuation over johnston Island as measured by the Project

6.7 ard Sandia rockets (see Chapter 7), and the lack of obvious evidence

for the targe effects in the conjugate regions.

It is ui.:ortunate that no radio propagation 7neasurements other than

riometer measurements were made thiough the conjugate regionb. There is a

hint of large Offects on the two northern Project 6 .7 rockets, but they were

near the orPds of their traj*ctories and zhe data are h-rd to interprcet. In spite

of th. lack of direct evidenc., o

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-I

LMSC- B,06989

R,. ferences

1. H. M-eoerlin i. Lcn,. D'rtI,)n D.-tbrs Elistorv and lonosphere EffectslPe.-ultnrig from St~ri ")ASA 1 33. Proceedings ofSymposium at Sa'i

2. J. Zinn and H. Hoerlin, OptIc3i Measuremeants (U), __ASA 1380.Prnceedir.gs of S','mposiu:m held at EGG 6/63

3. H. Hoerlin and J. Zinn reprints of oapers iron'. Rof. 2, In1.A.:-; Pzoters Presented at DASA Symposium on Optical Measure- Jmt n , L•MS z1, "

4. H. hoeY1in, 1. Bennett, M,. Pec'k, D. Sappenfield, S.N . Stone,nr.d J. Zinn, ".,%" Rf,''.ew Svimpaiu' (Fishbowl) Vol. 1 ofCAS;. 1449. P, zCj-Cdmns of Sympc5sium, h(-Id a, IITRI 12/6Z,

'.. . L~it.2. ii . ' ! z rlin, ,... Pc. ":c~ "" . . . . . .~i~ .. .c r t,-,• • "

~.tni F~l. rocc.,dmcjs uo Az-vanced Stud%, Institute atEerGen, Nor..'v 8/65. D. R2.l Publishing Co., Dortrecht, TheNetherl~r~ds

6. -. lioerlim, Tonmt AZC-DOD Optical V,'.r;:shop at Los Alamo! 1/67.Proc.eecinqs to be pubishecd.

7, D. F. H1ansen and V,'. Fcoquist ii; _,ptic-fl :Ncasureme,.-ts DASA !3 L, 1Prozeedins of Symposium held 6t £2G 6/63..

S . M. Shuler in DASA ReviewS.'mposium (r-hno;,') Vol. I ofDASA 144w, Proceedings of Symposium heiu at lITRI iZ/6Y

9. W. P. Boquist, 4r.N. all, T. Pascoe, S.H. Dohorty, .Fishb,%w! Auro-al ,Measurements in the Northern Coniugate .Reao_!.n

LGG Rcport B-Z33 6/64

i0 . D. F. 1lansen .;t al. Onti=-nl Phqnomenologv of Hi-3h Altitude Nutloar -,

11 . W,. P. Boquist, DASA Review 64-3

.Z. W'. P. Boquist, DASA rview 66-1 I

6-42 '1

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LMSC-B006988

13. D.A. Ha,Iin, R.V. Loywcn, R. Mlarr.ott, and D.H. Sowle,r-,i•i'5s of Or-hrati',. Psh-z.-] Data for Motion of Bomb Deb:isD.4D SA 1476 -,i.

14 N*V P. Bc-quist, W.N. Ha . r. P-scoe, anC S.H. Doherty,Fi s:bnwl Auroral Me. , --- t r tr '8outhern Conjugate Reo.ic,

MCG Report E2.i,

B15. .,. u:K, .:, Ii .1 Stub-s. J.A. V.,halen, i-iigh Altitude (Starfish).. ,!.•, hMt. Auburn Research Associates,

16. John Z.r•:,, Los Alamos Scientific Laboratory, private communication.

17 E. Marton, priv.,ate commuicatic.n based on inspection of EGG filmson !ile at DASIAC.

1i .J. Grifin, Re-£,•ah-ticn of Cptirr.nal Perameters for Post-Pssio' .,LDec.', LiSL LA-2bll, ;,zencdum II, 6/64

19. J. J. Griffin, Phys. Roy.

20. H1.I. WVest, Trons. Am. Nuc. Socc. 3, 537, (1960).

j 21. P. Armbrusto.r and H. Nleister, Z. Physi,, 170, 274 (1962).

22. W,-. Kr.na and G.E. Putnam A--448 (1956).

23. B. MlcCcrmac et al., Intecrat.cn and Synthesis of Fishbow. SCR rInti

24. P.L. Hart:nan, M' ensurements of the Absolute Fluorescence 7ff:'-ic.... ofA~r Under Electron Borz;b.rdment, LASL, LA-314/-%MS, 1,

25. E.W. Bennett and M.W . Hane, Spectrographic Air Fluorescence M.53sure-

"merts cn ctarish, Kingfish, and Pluerill, LASL, L.AMS-30-4.,,

26. W. Bccquist nnd6 . S;)yder, Ccii~gaste Aurcrijl Measurements trcm t.'oec C '.2. Halo Altituc(e Nuclenr lest Series, EGG B3435,

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2', D. A. Hamlin, R.W. Lov,'en, D.N. Sowle, 6nd R. C. Vi.',F'udic's cf 11t1h Z1,Itit'lie Nucle*ir Fxrioslon Phenornen-DA A 16 :3 , C''.

2ý. T.G. Stlnchcomb, C.W. Te.-r'Jn, M..crhir.s, -, w. C. Proston,Pc'r r.t 6.5 B Project Officers' Report, DASA >.,C.'i

29. r.G . Stinchco,.b zond C.W. "r•c-.i. in T.hbris Motion and Related

To-".,, UiA 1747, 2/,6

30. R.G. D'Arcy and S.A,. Colgate, )GR 70, 3147 (1965).

31. 0. Manley and 1. C!.:tt rn Debris Motion and Related Tz..,DASA 1747, 2/,.

32. 0. Ma.iac r.nd J. C.krpentcr, Nuclear Weapons Effects Revi ew 66-2,..• 1793, 6/66

33. TB. Barreit and ý,-;.3. . in Debris Mction and Rclated T:plcs*\SA 1747,10.'$5

34. J.R. lo: -r.d G .J. Gas.mrann, Nuclear Weapons Effects Review bn-jL•

35. H.A. B the, Radar Blackout for Starlish, LASL T-1351, 8/62.

36. R.L. Bgusch and ".. . Cc'rrelbti%-. " r..• .-1.. Data Relatedto Radar .da"... 7 ASA 1439, .i.

37. G.L. Johnson, Analysis of Fishbowl Riometer DQ41P D;,SA 1696,/8/65

,'

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Chapter 7. EFFECTS ON ELECTROMA3NETIC PROPAGATION

7.] Introduction

The problem of analyzing the Starfish radar results is a difficult

one because of the lack of reliable models for calculation of the various

effects and because of the limited data. For low altitudes the formation and

growth of the fireball are reasonably well understood, and estimates can be

made of thc degree of ionization and the resultirng radar attenuation. Because

S. . ... . .... ...... e , l uie s are not available, and

the Analy!is (and OepecIalh' the predictions) must be reoarded with some

A major dl'tr'culty is that aetails of electromagnetic propagcticn and

absorption ire str ::gly dependent on electron density and average electrori

velucities (electrcn temperatures, where such can be meaningfully defined)

for altitudes above about 200 km. Because of the low ambient, air denalty it

this region, prompt thermalizatior, of the electrons cannot be assumed, and

rather high average electron energies may persist for a considerable tilme ater

the elevtrons were produced. Collisions between electrons and ions are the

dominant provess in deterainirng the collision frequency to ba used in 3ttenua-

tion calculations. The electron-ion collision frequency varies with electron

temperature T as T-3/2 so uncertainties in electron temperature cr

energy can produce large uncertainties In attenuation calculations. The

attenuation is also proportional to the square of the electron density N e

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rather than the first power as at low altitudes, so uncertainties in N C

Icead to correspondinglyv 1rger uncertainties in attenuation.

In the following pages, several catego:ies of radar effects %-ill be

discusscd:

(a) Absorption in the ionized region produced by Starfish. Since

th'e detonation occurred at such a high altitude this region extends over a

very wide area.

(b) The back-5catter ot radar energy (ciutte.-). Thl main niccnar.Zm

se'Jms to !,.- ari-tions in electron dEnsily, in particular l o n'genc.ties

(c) Refraction effects dua to thc presenco of lonized rc-gions,

(d) Scintillation and utter due to spatial fluctuations In the elocuTon

den ityv.

(,' The production of extraneous signals Which arc detectb'e by

the nidai sytcrn, i.e. noise., Dcteili of the radar receiver, antenna Ird

source-target geometry are neuded for analysis of noise effec's. Tw-o sc;rc; a

of noise are of potential importance for radar systems: (1) synchrotron

radiation of high-energy electrons in the earth's magnetic filCI, (2) tzier'sl

noise from hot fireball-debris recions.

(In additirn to the radar unta wiich ci.n be attribute& t. i.)nizzti1,n

caused Ly the Starfish weapon itnelf, there is also evidenc- [or rac,•r Cc.h'-s

due to the hoo.;ter cdebris. A survey of these unusual radar echoes is aivs,

in Rcf. 13. In consideratiun of eiiccts of zi Starfish-likc burst on a ;adnt systcm

the presence of these echoe,; should be n'oted.)

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7 .2 Ridar Attenuaticn

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Sandia rockets and the ive rockete, of the Proiect 6.7 debris expansion

experiment.

7.2.1 S3ndia Rocket D-nta

Information on the Sandia rockets is contained in the Project 32 PCIR

(Ref. 1 Five rockets were !n the air in t*e. neighborhood of Jhnston 1sian d

i.t short titre . Of thcse-, three were .r ..s..tttnq signl•s at abc 't 2$5^ MC All

"&he telz.etr'y record of one of th. rockets (SJL-153) is shown in l'i. 7.1 . Th!

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These extremely large. electron densities and attenuations are not

observed, and therefore a large portion of the downward kinetic energy is

not converted into ionization. Therefnre a more reasonable estimate for the

absorption of radar is given by using our first model: distributing the

magnetic bubble energy uniformly to give an electron density.

The major radar systems effect for Starfish may occur at the conjugate

region where the betas act to produce ionization and not In the vicinity of

the detonation itself. AMother effect is that of hard ultra-violet absorption

in the upper E-region where ionization effects may persist for long times.

I

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Communications Effects

Deleted \".

The measurements of the perturbation of VLF links followitng Starfish

r.,dicato that prompt neutron decay effects can affect the propagation over

paths at distances of thousands of kilometers from the event. There was

also evidence for drifting debris effects. The initial stages of disturbance

on paths to J.I. can be attributed to ionization from prompt y and x-rays.

(Ref. lu, 11.) Another effect of importance is the neutron-decay Inducna

perturbation of VLF signal paths. Ref. (11) gives a discussion of the effects

of the neutron decays on VLF signals.

Deleted

Communications effects of Starfish and similar typ.e bursts can bc

large and very significant. The exact prediction of the effects is difficult

and depends on the type of communirations network being considered, and

the availability of alternate communication paths.

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7.6 Summary

Hich altitude bursts such as Starfish can probably considerably

degrade the performance of presently contemplated radar systems. An

analysis of these effects has been given in Ref. 18,

The phenomunrology and the data for bur~stz in the Stnrf!Th altitude

regime are sufficiently uncertain that it seeohs difficult at the present tilme

to make any definitive statements as to the system effects of Starfish and

related bursts on VHF radar systems. It is posslblo that for Starfish we were

just at the edge of producing strong effects In the VF lregion. All the rough

estimates that we have given for Starfish electron densities indicate large enough

valucs so that VHF effec: may xvcll be important, and tcir seening absence

in Starfish an accident of the data for this part:cular event,

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References for Chaprer 7

I. Miller, C. R., .High Altitude Measurements , (Sandia Report

SC-I TR-2046)

2. Fischer, P. G. , Starfish Revisited, (GE-6STMP-81, DASA-1730)

3. Towle, D. M. , Radiometer NMeasurements, (MI T3 14-ESD-TDR64-375,

Sept. 1964).

.,. Towle, D. MA..

5. Dyal, P., ,.,bris £xpansion ,E'perimcnt, (Project 6.7, PCR-2026)

6. Dyal, P. , Pcc Measurcrments o; Proei 6.7, (AWWL-TR-66-74 and

AFWL-TR-66-7S).

7. Horowitz, S., R iorrter Meaturernents, (Project 6.8) ,(POR-2027,

AFCRU,

8. Johnson, G. L. , Nuclear Radar Clutter, Vol. VI, (SRI, June 1966).

9. Jayc, W.E. C., Airbcrre R!d'r ObZervations Diring Fisthowj (SRI-4-

1767, Project 6.9).

10. Carpenter, G. B., VLf Prcoaaatlon During High Altitude INucledr

Events.(SRI-5-1407, DASA 1618).

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11. Wclthng, W. ., et. al., Etfects of Nucloar Detonations on the

r-Rvnion (AVC0-ArCRL-65-b24)

12. Maeda, H., T. Geophys. Res. 6S, 917 (1964).

13. DASA Review 64-3 (11,/64).

14, rlshbowi R0.dar Data Analysis (MCA-MO-4234), (DASA-1673-.1) (June 196S).

15. Optical Symposiur (DADC-SR-3, DASA 1337)(Sept. 196Z).

16. Bowles, K., Raaoo Wave Scattering in the Ionosphe,,e p. 133.

17. DASA SR-50, Sympoium on Eh, ctromagnmic Effects, (DAS,\-1826) (Oct. 19CGCA.

18. Bowusch, Stanton, GE £LMPO-6S-TMP-54.

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Chapter 8. CONOLUSICGNS AND SUMM',RY

Deleted

For these reasons on

analysis of the effccts of Starilsh-li14e bursts on radar systems is of great

imnrcortarice.

In passing it may be noted that Starfish is probably an atypical even-

as far as an ABM system is conccrned. The yield was lower ano the altitude

was higher than might be expected in a typical ABM defense situation. Thus

conclusions reached about radar effects from Starfich may not be of direct

relevance to the actual ABM situation and corresponding care must be taken

in drawing ABM conclusions frcm the Starfish data.

8-1

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8.1 Sys~ems Effects 4

6.1 . 1 Introdu,"tion

The major question in analysis of the sys~ems effects of Starfish,

is one of debr!s !ocation. The effect of a Starfiý-h-likc burst on a long rarge

high-altituoe defense system v

peis very important in

dctcrmlning the fasiillity of such a system. For this reason the analysis

of Deletedf results is of importance. If wo can; detei"mine a reliable

model fcr the debris spread and the extent of theD eleted dar effects,

thz.i we may have a useful tool in analy•is DeletedIn parti,.ular it is important to find out if one can set up a reliable

model for estimatus of the time of the radar blackout: if this tit . is short,

thcn the distErnt. high-altitude intercept system may be a useful concept

from tha di-fensive point of viewi.

'A. -"-.•

Deleted

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An unresolved uncertainty is the effect of multi-bursts: the

environment will presumably be very different for bursts of the Starfish-type

after one or a serieb of bursts. This question we do not attempt to answer.

8.3 Summary

Starfish was an event unusual in the great variety and extont of the

phenomena which developed. We have been concerned in this report with a

survey of some of the phenomena which characterized Starfish, with a view

towards developing an understanding of the mechanisms involved, so that it

would be possible to make some estimates for other yields and ambient

conditions in the same altitude regime. Major regions of uncertainty are the

values of the electron density which result and the distribution of electrons

in space. The snowplow model developed here can give some estimate of the

possible extent of the debris expansion, but the step from debris extent to.

electron densities is not clear. A very crude estimate may be had by distri-

buting the kinetic yield throughout the debris-magnetic bubble end assuming

all this energy goes to creating electrons.

In conclusion, Starfish-like bursts may effectively degrade VHiF

systems.

8-8

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A Gro..p 1Jivis.1on of Lockheed Aircraft

A STARFISH HAPPLNING

a 095ac oviev No~as (TV"e &I vell. smo IAAct.I del..)

Final Report

Berg, R. A. , Holland, D. H. , Futtern-,zn, W1..

4 It 9.0 PT 0 J't 70 IToAt. . ev 0 PAGES 1 76 .40 op hap#

March_1967 ______________________

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Defense Atomic Support Ag~ercyWVashington 25, D.C.

11 ABITRACI

The experimental data obtained during the Stalfish detonation are discussed,

with emnphasis on the phenomenology a,... electromagnetic propagation. Vario..is

mocels of use !or explaining2 the phenomneria observed during Starfish are

con~idercd. M,'odels are formulated which can be use~d to predict Oftects of

other detonations similar to Starfish In yield and altitude.

DD . 1473

K9Y W0001 of I 064~ .

E1a:kowt, Radar, Weapons Effects

I. OP'. 11ATIING AC'T1VTTY: Entire the n~salo &Wu4dress lsposed by nWWUy d~o .icr~aoq "tag sedar ofUwcedmttci the coeiisc,91. Wixon~tiactor, gtantt@S. DirpamvlEWt o~f De. much ad;fen$# activity at Other orgArueauont (Corporate author) 990UsM&~ (1 "Qo'iie fict r wa 01 capivio att athe report report fre" DV..'.7. REPORT SECUW!VY CLASSIPICAT1O4t Entter the ovw (2) "'aeeilgia sarin e sad dispeatamse of. ILas

al uec~i!~ cla S.,"s n of llhq repe"I'. Indiceate oWheihe""R*tr itd Dat is imiteude4 blotting to to be in acevr6 totb Ci ea.wt.1n~e RWIth gpptmvnate aeditty re*ulatj91b1 (3) "U L Govememeas agscies may oh~s eage r(uo

this repor dwactly fto DOC. Otter QsmL~qd DOC2b. GROURP Automuaic dourn~radtng is specified in DOD Di- usr Sholl te,9ieSI tkrotsghnectiY. $20O0. 10 and Armoed Forces. lftduitia. Mantual. Enter4 4 grovjp numbirt. Also. wien applicable. %how that options'.______________________sfainwiivli have baee used for Group 3 and Group 4 asat iilhr (4) "U. L. maiitar? &Cowitse May ablaj" w'ipes of L%.6

1. RUIONT TIrtE. L~eav the votrpiteto report title lit 1 Shall #04maes ibrasocapita~l lvtrnis Titles in all coo&@ should be unclassified.Ut a invorioAglut ittli cannot be selected without classilic&.tiovN show titie clossalfcotbos in gall c&PLzalS In Illatuheois (3) "A1 diel~bwa @4' ilus room epis ciSewtvalO'.1 Q"-alaine,4dis1.0l following the title. dieid DDC US~aalsers h u fe 'es rew4b

4. DESCRLPTXVE "OTES UI apropritsir enter the t~ys of________________in-rtcf. #l.g. itaefi., pteigoass. burnUmef 7 aruwal. or final. it the epr kl 6"M twotad ti the Oftfce of Te'tcbrcsGive the inclusivest4airs whent a specilic isyortifig poioid is Saitces. Doyensweum of commece. for sale tM thM rpktc. msdpcov ered. Cate hski fact on ots Lrao oncpe. .1 know%S. AVTI4OR(S): Erie the noev(s) of author(s) am shown* Im L SLPPL~dgtTAXV NOTI Utte far adiatuaesal eusplamat in the rrpnitL Lawte tast name, (usg nameau. eaddlo tial. t"e 201946If trot itery, stow rorit end tranch of iloivic*. The name ofthe principal .. the# to an absolute Shlnuous requireseeft 12. UOMQN1RjC. ~ZA`RYAC7TMI? Vine wwr-thuo~ f

6. REPORTI)ATt. Leiter the dote of the report as day, the d fee, th m reai " iidrc devse,.eborlacruplus.dberwa.l(pmioKh yearor feMN Tbsh ac. It vicie tham lans dete, appears Jew lot this ¶~ mwc sli dbete 4"84L, wiisef ddnfacta

on the report, use date of publicatio 3 8 Ae &r 64141ef M48Ww n eoo7. TTAL 1JVDR OPPAGE The~ waftebry of the, decmu.t i&Sias ttw1 of the eepse' ires ioe%417a TTALK~bMR O PAES. he oW age erit t may sa Iod opol..r eia.e " &M the 110-17 W tia e's IfIcac M.-

shou.4 filjow nrencal paier.aion proeodwus, ILe.. etir the Port. If ad"uosal upsett ta imUyqoov a costuftnelta ehet &M.UtmJnmierq af page* conisautaig Inflorn~ation, be attache",1b. NVIIIIsER OF RELMZKIECE* Later the tots iwembe of 11 is bgi%$ 41cousb~e LU ", sblc 44 P4'aosaw PerpetiWrratence# eiaed is the report. be WK1664410id. Eacb paogrphp of 60 obatract s"I*. "ud with 7As. CY4TRACT OR GRANT HUMULAR: It mpoeorlet. OWN so i-..4 totism of Wh aulitat, ieanilty elasasftmutse. & ta &&.the applicable smiber of the contircl or rpan saetdw skirt (eeticata is the perserpli. necassieute as (Tj,. fis, e.. of Mtt)the, tepon wue ecittebm ?1mam i soa LautcUoo e e tobelo 4 as e ahtsbt.tct Hy..Mh. 4k, 6 Is. PROJECT NMBUNS Enter thi upp"tepittst over. IMe ""acted Watgab is fumea k so t 2:5 S-Military doeywtsMe adeoUfatationf. such at ploejenomt abse *.KTVRS a ~sae uePpm~igu e

itahateject ~ ~ ~ ~ ~ ~ ~ o mset. 16t1m1111tc uaee 0 hutp ,09. that chorseftene a .eV"n said say be asued asgat. ORIGINATOR'S REPORT HUME3(S Eawer the o111. lades orntiare low £owetbg" the impot . Sel meicscasm t bacilt-n r-otwausba by othich the decusMi S~il he Ideatlified selected so owlatme seeuiratr ciealfiutieam is dquate&. deatu.and conifelled by Ithe otgiuating aMwitt. Thisu eameb best fiet". owe% as equiaeoest~ meidc des'sautafls. Mile maw, mAIasryfor fawvea to this topeft project coda, sasse. u.g'oaehac insucue WA1 be ine4 me key,96. 0TW REPORT MUMBERL5: If the raltf ha bseeds bot sllu ba gieli~wd bor "n sldwatletad l04 as trcuIte.sseigned env7 *test rstome numtbers (either &IF the Otlilmasr fal IMu ae86SWOt 1 *9 sM ruled. sai eRWA a emo~aa

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