1962 CIA Report Quick Look Technical Results of Starfish Prime
Data Furnished by: Col. Leo A. Kiley, Commawler Iloerlin, Deputy Commaner * Heraz= J. Scott, Deputy Ccander Dr. F. C. Gilbert, Deputy Commander F. Stre~bla, Comander
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[[pages 1–102 of 112]] August, __ I 1962 DTI1C SJLE D MAR 1.6 1985 P A QUICK DOOK!' AT TIFE TECIVICAL RESULTS OF STARlFISH PRME 4-. Data Furnished by: Col. Leo A. Kiley, Commawler Iloerlin, Deputy Commaner * Heraz= J. Scott, Deputy Ccander Dr. F. C. Gilbert, Deputy Commander F. Stre~bla, Comander DOD Task Unit LSL Task Unit Sandia Task Unit IRL Task Unit EG&G Task Unit Compiled by: MEA iApproved 101 Public reZeaJ4J Dim~ur U au1Inta Francis Naxin, Stafff "Member Appruved: Wil.liam E. Los Alaws Scientific laboratory Walter A. Dumas, Major -ge United States AryV Scientific D
Dates mentioned
19621985
Keywords
Entities
Extracted text (OCR)
August,
__
I
1962
DTI1C
SJLE D
MAR 1.6 1985
P
A QUICK DOOK!' AT TIFE
TECIVICAL RESULTS OF
STARlFISH PRME
4-.
Data Furnished by:
Col. Leo A. Kiley, Commawler
Iloerlin, Deputy Commaner
* Heraz=
J. Scott, Deputy Ccander
Dr. F. C. Gilbert, Deputy Commander
F. Stre~bla, Comander
DOD Task Unit
LSL Task Unit
Sandia Task Unit
IRL Task Unit
EG&G Task Unit
Compiled by:
MEA
iApproved 101 Public reZeaJ4J
Dim~ur U
au1Inta
Francis Naxin, Stafff "Member
Appruved:
Wil.liam E.
Los Alaws Scientific laboratory
Walter A. Dumas, Major
-ge
United States AryV
Scientific Deputy JTF-9
1
•'89
3 1,
05
The enclosed report is
a compilation of data available in the field
-within approximately 10 darys of the Starfish Prime event, together with
an introduction to the objectives of Starfish Prime and some tentative
conclusions about the data obtained.
As such, the reader is
cautioned
that all data are tentative and in most cases obtained by "quick look"
in particular all numbers quoted are subject to later
techniques:
correction.
Accesion For
NTIS
DTIC
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(", '-.;
CRA&I
TA3
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UNANNOUNCED
Abstract
The Starfish prime event (
altitude SSW of Juhnsto,
detonated at l00 1n
Islelid at 2300 hours, Honolulu time on July 8,
1962) significantly increased the understanding of high altitude nuclear
detonations and their effects.
As an aid to penetration for incoming
missiles by disrupting enem
anti-missile radars,
Starfish Prime was not
as effective as anticipated.
Detonation degradation of communications
and radar surveillance capabilities were found
to be appreciably less
than expected.
Some data were obtained on the direct effects of q bomb
÷
x rays on materials carried on pods near the burst;
most pod experiments
were not as successful as desired because of pod stabilization and
positioning difficulties.
O
VL
e
Beta ray and debris pancakes
were formed along magnetic field lines north of the burst at a distance
of 600 km at an altitude of 120 to 150 km. The effects of these pancakes
were of comparatively short durations.
A pancake was also formed to the
south of the burst along field lines, but a significant panceke did not
form under the burst. The major visible effects of these pancakes lasted
for a number of minutes; an auroral gýow was still in evidence four hours
after detonation in the north conjugate area;
ionospheric disturbances
in the south conjugate area lasted for many hours.
r
of debris were deposited along the manetic field lines intersecting the
bu-st location at altitudes vell above that of the burst. Rocket-borne
VI
I
Significant amounts
high altitude diagnostic techniques were tested; neutron, x ray, gamma
ray and time interva.l measurements were successfully made;
radiochemical
sampling and alpha measurements were unsuccessful. High altitude nuclear
detonation detection systems were tested with a very considerable degree
of success.
The small rocket weapons effects and phenomenology diagnostic
program from Johnston was quite successful.
4I
TABLE OF CONTENTS
Page
Abstract
L
3
I.
Introduction
6
II.
General Summary of Results
13
III.
Data Compilation
A.
Seismic and Pressure Measurements
B.
Neutron Measurements
24
24
26
C.
0 and 7 Ray Measurements
D.
X Ray Measurements and Direct X Ray Effects
Measurements
3
E.
Light and Thermal Measurements
-
F.
Measurements of Electromagnetic Signal Due to
the Weapon
42
G.
Biomedical Measurements
46
H.
I.
J.
Measurements of Effects on Radar
Direct Ionization Measurements
Communications and Ionospheric Disturbance
47
52
Measurements
Magnetic Field Measurements and Earth Current
Measurements
Miscellaneous Measurements
53
K.
L.
66
70
Appendix 1.
TVJ 8.1.1 Los Alamos Scientific laboratory 4eliminary
Field Report.
Status as of H + 5 days. H. Hoerlin,
1ASL
Al-i
Appendix 2.
Discussion of Riometer Data and its
R. Dyce, SMI. and W. Kna•;, GE
Appendix 3.
Miscellaneous Reference Data
1.
R/V and Pod Positions, and Time of Burst
2.
Small Rocket Data
3.
Ship, Aircraft, and Island Locations
4. References
5.
Orgaznizational Abbreviations
a
*
6.
Weather Sunmary
Distribution
1
30
Significance.
A2-1
A3-1
A3-1
A3-2
A3-4
A 3-7
A3-8
A3-9
last page
5
Introduction
The warhead for the Starfish Prime event of Dominic was launched
from Johnston Island on a Thor missile and detonated at 2300:09 hours
Honolulu time,
L
on 8 July 1962.
The warhead, contained in a spin-
stabilized re-entry vehicle, detonated at 400 km altitude 32 IM from its
launch pad with a nominal yield
P e
modified for the firing by the i
systems,
Three 1200 pound pods,
safety (destruct)
flywheels and it
(See Figure 1.)
resembling re-entry vehicles, were attached
to the missile at time of launch.
numerous small experiments.
r
lusion of telemetry,
and special external insulation to prevent excessive heating
of the after structural members.
a
The Thor missile was
The back plates of the pods held
The pods were stabilized by heavy internal
was hoped that after the pods were released from the
missile at about main engine burnout time they would remain in a near
vertical position.
I
Release times were progreamed so that the pods would
be below the burst with their backplates approximately normal to the lines
from the pods to the detonation.
Me podf contained transponders to assist
in determining actual position after the detonation and recovery gear so
that they could be located and recovered.
Scientific stations to obtain data from the various experiments were
estatlished throughout the Pacific area, with the most concentrated group
on Johnston IclrJd.
F6
From Johnston Island 27 rockets were fired in
support
Figure I
7bor missile wlth pods in
Prime is
Bluegill Prime configuration.
Starfish
essentiallv identical.
j
I
7t
J
-w
l
of experiments,
and a large array of optical and electromagnetic
instrumentation was operated.
In the area surrounding the island, a
fleet of ships and aircraft operated with technical stations aboard.
Stations were established in the Hawaiian area to observe the burst from
elevated areas and to observe the northern conjugate area.
A large
nuber of rocket-borne instruments were launched from a firing area at
Barking Sands,
Kauai.
The southern conjugate area was covered by
establishing stations in
the Fiji, Samoan and Cook groups and by
stationing ships and aircraft in the general area.
Other shipboard
stations were utilized througliout the Pacific to study t.le effects of
ionospheric disturbance on RF transmission and reception.
An unsuccess-
ful attempt was made to launch two rockets from Point Arguello in
California in
support of the TtJ 8.1.1 effort.
voluntarily in the event,
in
Many groups participated
generally invited by the Department of Defense,
order to take advantage of the substantial Interest in
the world's scientific community.
groups will,
It
is
the event by
hoped that the results Zrom these
in time, be reported to the scientific commiunity.
The operation was conducted by Joint Task Force 8, commanded by Maj.
Gen. A.
D. Starbird, which was resp
.,ible to both the Atomic Energy
Comission and the Department of Defense.
Task Force was Dr.
The Scientific Deputy of the
William E. Ogle of the Los Alamos Scientific Laboratory.
The scientific elements in the Task Force were organized into Task Units
as listed:
TU 8.1.1
Los Alamos Scientific Laboratory
TU 8.1.2
Lawrence Radiation Laboratory
-J 8.1.3
Field Co=-.ard,
"T-U8.1.4
3andic Corporation
TiU 8.1.6
Lager1on,
Defense Atomic Support Agency
Germeshausenr
and Grier
izurin£ the period that the Starfish Prime event was being prepared,
most of the Task Units were also involved with other events of Dcriinic
on Christmas Island.
4
The Starfish Prime h..gh altitude nuclear detonation had the following
L.
9
major scientific objectives:
1.
Evaluation of missile kill
mechanisms produced by a high altitude
nLcle•z detonatior.
2.
Eýluation. of the effects of a high altitude nuclear detonatior.
on electromagnetic surveillance capability.
3.
Evaluation of the effects of a high altitude nuclear detonation
on long range ca
4.
unications.
Investigation of the basic characteristics of a high altitude
nuclear detonation and the physical basis of the effects.
5.
Evaluation of high altitude nuclear detonation weapon diagnostic
techriques.
6.
Evaluation of high altitude nuclear detonation detection systems.
Electromagnetic surveillance capabilities after a high altitude
nuclear detonatioL were studied by a large number of experiments.
Attempts were made to track objects, in,
near, and at large distances
from the debris and to measure the attenuation and refraction of radar
signals.
Measurements were made of radar bcatter and clutter due to the
debris and ionospheric disturbances.
These experiments covered the radar
frequency spectrum, specifically including those frequencies of greatest
interest in anti-missile missions.
The period from before detonation
10
uitil
after detonation effects disappeared was covered.
Logr
and short rarZe c o_'•ications
wc.e tested t--roughout the wc-ld
bIy co=nunications
si=,Llation experi-ments. and b,"y nonitoring a large
number of existi:u
coz-unication nets.
Both gover-rnent
and private
cmmurications systems were exercised during the period of interest with
the aim of determininr
signal propagation condiitions as a f rct
of
frequency, path location, and time relative to burst.
The basic physical chs,•rcteristics
and effects of high altitude
nuclear detonations were studied both for applicability to the other five
objectives of Starfish Prime and "or their inherent scientific in*erest.
Two of the phenomena of prime importance were the debris expansion
history and the geomagnetic
effects.
Experiments to obtain data on these
phenomena included detesmination of the ionospheric corposition,
coszic
electromagnetic noise transmission through the ionosphere,
magnetic field
strength measurements,
earth current
measurements,
radiations.
various satellite-borne experiments,
sky brightness measurements,
Ultraviolet,
and measurements of rftclear
visible and infrared spectroscppic
and
photographic measurements were made near the point of burst and in
the
north and south magnetic conjugate areas.
Weapon test
diagnostic techniques were tested by considering both
the d.rect emission from the weapon Lnd the effect of these emissions on
their
surroundings.
The bomb energy emitted as x rays was determined by
direct measurement of the total
apperent bomb temperature.
x lay energy and measurements of the
X ray excited air fluorescence was studied.
Neutron flux and energy distributions were determined,
ray fluxes and time histories.
The behavior of the bomb debris was
studied and rocket-borne debris samplers were tested.
electromagnetic
as were ga
There were
and 9ptical measurements of the time interval between
the weapon primary and secondary,
as well as an attempted measurement
of bomb early alpha by high resolution telemetry techniques.
It
was
hoped that the yield could be determined by an analysis of the direct
thermal radiation, the x ray yield as inferred from air fluorescence,,
I.I
and the kinetic energy of the bomb debris.
Higa, &Atitudenuclear detonation detection systems were directly
tentef
in the Starfish Prime event throagh the use of the Vela Sierra
air fluorescence systers and direct optical systems.
Tne spectral
characteristics of the air fluorescence were studied to aid in distinguishiZ.g nrclear detonations from lightning flashes.
Optical and elecuro-
magnetic time interval measurements were of interest in
this area, as
were the verious measurements of the electromagnetic signal from the
weapon.
In addition many of the basic effects which were studied could
have applications in detection systems.
r
12
II
General Suary of Results
Unfortunately difficulties in pod stabilization arn
positioning
seriously degraded the acquisition of data on the direct effects of x
rays on materials.
Pod S-1, closest to burst, was essentially at its
desired location of 8 i• from air zero.
It
waz pointed toward, rather
than away from, the burst so that the experiments on the backplate of
the pod were not exposed to the burst;
therefore, no data on direct
x ray effects were obtained from this pod.
The pod did have a circum-
ferential crack and a dent in the lining, but these may have been c.wsed
by impact with the water or rough handling on recovery.
Pod S-3,
furthest from the burst, was 23 km from air zero rather
than the desired
14 km..-
Its backplate was slanted from normal to the burst (See Figure 2)
vith the axis of the pod forming an angle of 40° from a line thraugh the
burst point to the pod.
As a result the experiments were degraded both
by excessive distance and shadowing.
No data on direct x ray effects
were obtained from. this pod.
Pod S-2 was 12 km from air zero with the
axis of the pod forming an angle of 43 degrees from a line through the
burst:
owing to shadowing approximately 50% of the x ray effects
measurements were not obtained.
Some of the material samples and indenture
gauges were subject to the direct x rVy flux and are being analyzed;
these shcxald yield same useful x ray effects data when completed.
Rocket-borne detectors did successfully measure the x ray yield,
L
13
(
*
*
AIR ZERO
ACTUAL
POD S-3
POSITION
DESIRED
POD
POS. (ION
4.0
Figure 2
I14
-
Pod Position Diagram
AIR ZERO
the black bod.
temperature of the weapcn,
and the neutron flux; in
addition, foil! carried on the pods yielded useful neutron flux data.
Although there is
still
a fairly wide spread in the data,
15
ICBM
*400 km PRECURSOR SHOT
AS AN AID TO PENETRATIQN
EXPECTED
IONIZED REGION
TO DEGRADE ENEMY
-AICBM
AICBMI
Fig~ure 3
-Precursor
80km
Shot Tactical Cond-ition
17
RADARS
MAGNETIC FIELD LINE
EXPANDING D-RAY PANCAKE
EXPANDING DEBRIS PANCAK
BEGINNING TO•.FORM
400km
JOHNSON
ISLAND ý,,
L
120-15Okr
400mi
Figure
f
-.
NORTH
,
4 - Northern Pancake Location at + 70 Milliseconds
1
--
began to form in
the sasne area; eventually the debris pancake was
brighter than the beta pancake.
also deposited in
Ve,y large fractions of the debris were
a panca3ke to the south of the burst at intersections of
the magnetic field lines, through burst and through points above burst,
with the atmosphere.
burst.
A strong pancake did not develop directly wnder the
The injection of large amounts of debris into the geomagnetic
field above the burst,
and the mechanism of the subsequent debris
distribution are not fully understood.
complex.
The effects appear to be quite
(See Figure 5)
The visible phenomena due to the burst were widespread and quite
intense; a very large area of the Pacific was illuminated by the
auroral phenomena,
(Tongatapu)
from far south of the south magnetic conjugate area
through the burst area to far north of the north conjugate
area (French Frigate Shoals).
A large amolunt of spectroscopic data were
obtairKd-.
At twilights after the burst, resona~nt scattering of light
from lithium and other debris was observed at Johnston and Frenclr
Rrigate Shoals for many days confirming the long time proaence of debris
in the atmosphere.
An interesting side effect was that the Royal New
Zealand Air Force was aided in anti-submarine maneuvers by the light from
the bomb.
The next paragraph is an eye witness report of the detonation
by MaJ. C.
X. Mcllue,,
AOMC,
Kwajalein; the paragraph following that is
an
eye witness report from Johnston.
At Kwaialein,
1400 miles to the west,
a dense overcast extended the
length of the eastern horizon to a height of 5 or 8 degrees.
RC
At 0900
a brilliant white flash burned through the clouds rapidly changing
to an expandirg green ball of irradiance extending into the clear sky
above the overcast.
resembling
horizon in
From its
surface extruded great white finwgers,
cirro-stratus clouds,
which rose to 40 degrees above the
sweeping arcs turning downward toward the poles and disappear-
ing in seconds to be replaced by spectacular concentric cirrus like
rings moving out from the blast at tremendous initial velocity, finally
stopping when the outermost ring was 50 degrees overhead.
19
They did not
z JJ
M
0
z.
0
m
0
0-
00
0
Li
cZ
j
=
LL
-j
00
cr
M
0U
w
C
zZ
0 (n
w
IjJLL
0.
mw
20
0
disappear but persisted in a state of frozen stillness.
occrred, I would Judge,
within 45 seconds.
All this
As the greenish light
turned to purple and began to f.de at the point of burst,
a bright red
glow began to develop on the horizon at a direction 50 degrees north of
east and simultaneously 50 degrees south of east expanding inwaid and
upward until the whole eastern sky was a dull burning red semicircle
100 degrees north to south and halfway to the zenith obliterating sme
of the lesser stars.
This condition, interspersed with tremendous white
rainbows, persisted no less than seven minutes.
At zero time at Johnston,
one could remove his goggles,
a white flash occurred,
but as soon as
no intense light was present.
A second
after shot time a mottled red disc was observed directly overhead and
covered the sky down to about h5 degrees from the zenith.
Generally,
the red mottled region was more intense on the eastern portions.
Along
the magnetic north-south line through the burst, a white-yellow wtreak
extended and grew to the north from near zenith.
The wid,;h of the white
streaked region grew from a few degrees at a few seconds to about 5-10
d-6rees in
30 seconds.
Growth of the aurora.l region to the north was by
addition of new lines developing from west to east.
The white-yellow
auroral streamers receded upward from the horizon to the north and grew
to the south and at about 2 minutes the white-yellow bands were still
about 10 degrees wide and extended mainly from near zenith to the south.
By about two minutes, the red disc region had completed disappearance
in the west and was rapidly fading on the eastern portion of the overhead
disc.
At 400 seconds essentially all major visible phenomena had
disappeared except for possibly some faint red glow along the north-south
line and on the horizon to the north.
Vo soands were heard at Johnston
Island that could be definitely attributed to the detonation.
Strong electromagnetic signals were observed from the burst,
significant magnetic field disturbances and earth currents.
21
as were
A VLF signal
_D
some samples,
but the rocket-borne samplers were not recovered.
borne nuclear track e=alsions were not successful,
Balloon-
possibly due to a freak
te=perature inversion which prevented the balloons from reaching altitudes
geater than 50,000 feet, but rocket-borne
and are being analyzed.
emulsions have been recovered
Photographic and spectroscopic coverage of the
detonation was highly successful.
The short range rocket-borne
diagnostic program was highly successful.
Detection equipment of the Vela Sierra type was operated with good
success and the rangel'
and sensitivities of the method were found to be
at least as good as aredlicted.
The strong electromagnetic signals from
the detonation were observed under the sea,
airborne stations,
Microbarographic
at land stations and in
at many hundreds of kilometers from the burst.
signals from the detonation were obse1ved at Johnston
and Christzaz Islan"%s.
1-%gnetic field disturbances were measured
throughout the world.
1.
The detection range for a space detonation of yield Y kilotons was
calculated to be approximately given by
Range =
where range is
i
expressed in
1 0 5.\FY
kilometers.
23
-
III
DATA COMPILATION
A. Seismdc and Pressure Measurements
Project 1.1 (DASA).
Air Blast and Pressure Measurements.
Meazaros,
Julius
BRL.
Microbarograph at Johnston, on ships S-1, S-2.
Pressure gauges and
acceleromcters on the pods.
Results:
Preliminary data from pods S-1 and S-2 indicate no
discernible pressure or acceleretion.
Pressure and accel'eration gauges
in pod S-3 not operable.
Project 6 .5a (DASA).
Ionospheric Soundings and Magnetic Measurements.
Dr. Fhilip Newman, AFCRL.
NBS microbarographs at Midway,
Thutuila, Wake and Adak.
Corporation, at Palmyra, had 3 Hall Stars (HS-I)
Results:
Project 32.6
Mitre
4.5 cps seiemometers.
Data not yet available.
(Sandia).
Microbarography.
R. L. Eno, Sandia Corp.
Microbarographic measurements at French Frigate Shoals, Johnston
Island, Kauai,
and Christmas.
24
ResuJits:
25
B.
Neutron Measurements
Results:
Pod.
S-I
S-i
S-1
S-I
S-I
S-I
S-i
S-2
S-2
S-2
S-2
S-2
S-2
S-3
S-3
s-3
S-3
S-3
S-3
.- )
S-3
Cadmium shielded gold foils and bare gold foils gave essentialiy
the same neutron flux.
6
26
f
J.
Sandia Corporation Measurement.
J.
•iller,
Sandia Corp.
Fluor and photoznltiplier with log circuitry were rocket-borne fron.
Kauai (Rocket No.
SU-154).
Fluor and photomultiplier using H}ILRT (6 k)c
S1a-155).
telemetry) techniques (Pocket No.
Results:
stren th
Rocket SKI-154 gave preliminary 14-Mev neutron source
Deleted
Good gaena ray information should be
avý.alable from this recordý
Rocket SYa-155 gave a marginal strength signal but should give more
These data are not yet available.
c etails of the neutron spectram.
Project 6.•b-2 (DASA).
Balloon Measurements of Debris GCmnas.
BlO neutron counters at 100,000 feet carried by balloons launched
from South Conjugate Area.
OSO (Orbiting Sole- Observatory)
Satellite.
Dr. W. Hess., Goddard Spate
Flight Center.
Moderated BFO neutron counters.
Results:
No data; satellite not operating.
TRAAC Satellite.
Dr. J.
Solid state neutron detector,
further covered with polyethylene.
Results:
XPL
F. Kircher,
covered with 1 mscra2 of B 1 °,
Range:
Thermal to 2 Mev.
Data not *'t available.
Lawrence Radiation Laboratory Measurements.
The following were rocket-borne:
Dr.
F. C. Gilbert, LRL
a slow, neutron experiment from
Kauai and a Nal crystal activation experiment Irom Kauai.
tunnples were car-ied in the pods on the Thor missile.
Zr activation
Balloon-borne
NaI detectors, an.- neutron emulsions were launched f'rom Kauai.
r
and
27
Results:
Fission neutrons were seen from Kauai
in
the slow neutron
ex-eriment and a large flux of slow neutrons was seen from 1 to 10
seccniz afte-- detonation.
Kauai Na: results indicated
however-,
experiment.
pod angle may have degraded this
Balloons did not rise above 50,000 feet due to freak
te=perature inversion; therefore,
no data were obtained.
Los Alamos Scientific Laboratory Measurements.
Dr.
Two rockets from Kauai carried calibrated U'8
neutron time of flight measurements,
r
28
H. Hoerlin,
LASL
fission chambers for
and neutron emulsions.
Deleted
L
5
c.
r and y Ray :.easurerients
Oa.ra Radiation M4easurement.
Project 2.2 (DGw.).
Plz, badges,
glass microdosimeters,
activated borosilicate 6lass dosizeters,
John Kinch,
TIML.
formic acid dosimeters,
cobalt
and magnesium calcium fluoride
therioliuminescent dosimeters were carried on the pods.
Results:
Detectors have been removed frcm pods brut data are not
yet available.
Project 6.2 (DASA).
Rocket-Borne Gaema Rey Scanner.
Warren Berning,
BRL
Two Javelin rockets launched from Johnston gave gamma flux as a
ftuction of scan angle and position; total garma and total beta in analog
fcrm.
Results:
Ir• Lr.tar,'.antsd
Obser:vat ion
Launch time
Altitude
Gazmra scanner,
+20 minutes
below 125 krn
~125-325 a
p
525 km
325-600 km
Ge.=rr. scannerte
+hO minutes
Total gamia detector
+20 minutes
below 145 km
145-310 km
310 -•l
310-500 km
30
Instrument and
Launch Time
Altitude
Observation
Total Gamma Detector
+ 40 minutes
below 60 1,
Beta detector
+ 20 minutes
Deleted
60-175 km
Rest of
flight
Bet' Detector
+ 40 minutes
Project 6._
Warren Berning, ERL
(DASA).D Region Physical Chemistry.
Beta flux meter (i
100 key) and 2 channel pulse heigit analyzer
(2 0.5 flev and r 1.0 Mev)j similar gamma ray sensor.
Results:
Rocket launched at-4420 seconds got data which hav& not
yet been correlated with time, altitude,
Project 6.4 (DASA)
and orientation.
W. Pfister,
E and F Region Physical Chemistry.
AFCRL.
Beta and Gama flux meters similar to 6.-.
Results:
Most data lost due to telemetry failure.
at+4 8 0 and+960 seconds goT, data up to 100 km;
Rockets launched
counting rates increased
with payload altitude and appeared to level off at 50 to 70 km.
Rates
in +960 second rocket were perhaps lower than in the earlier rocket at
a given altitude.
Project 6.5b-lE (DASA).
of Iowa.
Satellite Data Acquisition.
State University
Dr. James Van Allen.
Injun I satellite recorded beta and g•nmna counting rates.
Besults:
(
Data not yet availablt.
Balloon Meesurement of Debris Gemnas.
Project 6.5b-2 (DASA).
C. Stone, ARF
NaI scintillation counters at 100,000 feet carried by balloons
launched from South Conjugate Area.
Deleted
Project 6.7 (DASA'
Debris Expansion Ecperiment.
Five rockets, each vith
6 beta counters and a gamma flux detector
were launched from Johnston Island prior to detonation.
recorded data for 27 seconds after detonation,
1000 km from burst point.
AFSWC.
Lt. W. Whitaker,
These rockets
from 100 to more than
Beta and gamma fluxes were measured both
along the magnetic field lines through the burst and perpendicult~
to
the field lines.
Results:
Data not ýet available.
Project 6.10 (DASA)
XF, VLF,
Loran-C Propagation.
Roger Whidden,
AFCPRL.
Nal scintillator in KE-135 at 44,000 feet with pul•se height analyzer.
Records in range 50-300 key and > 500 kev.
Results: Aircraft at 1770 47' W, 15* 22' S at 43,300 feet at H hour.
fp
Project 6.12 (DASA)
Piggyback Siatellite Packages.
Captain R. A. Bena,
AFCRL
0 and y flux meters on Discoverers U127 and 1128, recording DC
current aM 2-channel pulse height analysis (k 0.5 Mev, i 1.0 Mev).
Results:
No data.
Satellites not operating.
3
32
OSO (Orbiting Solar Observatory)
Dr. W. Hess, Goddard Space Flight
Center.
A number of gamma detectors.
Results:
No data.
Satellite not operating.
lIwrence Radiation Laboratory Measurements. Dr. F. C. Gilbert, LRL
Rocket-borne scintillator and photomultiplier (from Kaua.i) to
measure primary aLpha from the prompt gu"as.
photodiode to measure time intervul.
Resvuts:
Los
No data obtained :e
Also scintillator and
to improper circuit triggering.
os Scientific Laboratory Measurements.
Dr.
H. Hoerlin, LASL
Scintillation gamma ray detectors were rocket-borne from Kauai.
Results:
Sandia Corporation Measurements.
J. J. Miller, Sandia
Fluor and photodiode systems rocket-borne from Kauai to measure
time interval from gamma time history. (Rockets Nos. SKI-151, 152.)
Fluor and 5" photodiode system rocket-borne from Kauai to
measure alpha from gamma time history using HHRT (6 kme Telemetry)
techniques.
Results:
malfunction.
r
(Rocket No.
SKI-156).
No time interval data due to unknown instrument
No alpha information due to failure of payload to separate
from booster.
r
33
m11
ll
D.
X Ray Measurements and Direct X Ray Effects Measurements
6.; (T$ASA).
Prict
D Fegorn
nhynica71 Cemistry.
Warren Berning, BRL
Four rocket-borne sensors with thin Be windows; energy deposited
in 3 mlu
CsI crystal in I microsecond recorded in analog form.
Results:
Project
No data due to rocket failure.
6.4 (DASA)
E and F Region Physical Chemistry.
W. Pfister,
AFCRL
Six Ion chambers around Javelin rocket, i'th
filterb to select hard
x rays.
Results:
No data due to telemetry failure.
Project 8B (DASA)
Thermal Radiation :ui
Fifects.
Capt.
Gillespie,
AFSWC.
Indenture gauges,
metallurgical sanmpls,
materials carried on pods.
Results:
fracture gauges arn&.-ther
Also a K-edge detector.
See GenoraJ. Summary of Results.
Lawrence Radiation LaLnratory Measurements.
The following were rocket-borne:
F. C. Gilbert,
IRL
(1) an x ray bolameter from
Johnston (60-inch tantalum strip wound on a plate behind a beryllium
window) measuring the increase in resistance of the strip due to x ray
heating; (2)
a thin fluor scintillator from Kauai;
(3)
x ray photo-
electric diodes from Johnston.
Results:
Photo-electric diode data not yet
calibrated.
Los Alamos Scientific Laboratory Measurements.
Dr. H. Hoerlin, LASL
Rocket-borne scintillation x ray experiments (thin fluors over
photocells) and photo-electric x ray experiments from Kauai and Arguello.
34
Results:
No data from Arguello instrumentation due to rocket failure.
Sandia Corporation Measurement.
J.
J.
Miller and
J.
Scott, Sandia.
Fluor and photodliode system with subtraction of gamma contribution,
rocket-borne from Kauai (Rocket No. SKI-153).
Silicon solid state detector, with beryllium cone scatterer with
copper and titanium filters,
was rocket-borne from Kauai (Rocket No.
SKI-159).
Chromel constantan thermopiles to measure total x ray yield were
rocket-borne from Johnston (Rockets Nos. SJI-151, 152).
Thin foil calorimeter for total x ray yield was rocket-borneafrom
Johnston (Rocket No.
Results:
SJI-153).
Fluor and photodiode system failed because of a power
supply malfunction at launch.
Thin foil calorimeter failed due to telemetry malfunction.
I
35
E.
Light and Thermal Measurements
Note:
Snall scale optical measurements of limited interest (for
exi-A.e, rocket tracking) axe omitted from this ctmpilation.
Project 4.1 (DASA).
Investigation of Chbrio-Retinal Effects.
R. G. Allen, USAF, AND,
Lt. Col.
Brooks AFB.
Photovoltaic cells with filters and black body calorimeters were
carried in a number of planes as part of the chorio-retinal burns
investigation.
Deleted
Project 6.2 (DASA).
Rocket-Borne Gamma Ray Scanner.
Warren Berning,
ERL.
A photomultiplier tube with filters measuring the intensity and
duration
)peleted
i
Project 6 .2a.
Ionospheric Soundings and
rlagnetic
Measurements.
Dr.
Philip Newman, AFCRL.
Photometers measuring 3914, 5577 and 6300 A at Kona, Hawaii.
Results:
Record was initially saturated.
for 15 minutes.
36
Recordings were taken
C. Stone,
Photometric and Photographic Measurcments.
Project 6.5b-IA.
ARF.
Various photometers,
cameras,
and a 35O0-7400 A spectrometer.
Generally measuring over relatively long periods of time, with one
(Tonga and Tutuila).
millisecond time resolution photometer.
Results:
Photometer at
Tutuila saturated during initial phase of
phenomenon.
Deleted
C.
Tiros IV Satellite.
Project 6.5b-3R.
Stone, ARF
Boadband radiometer covering IR and visible; IR sensors with bands
7.0 - 30.0 microns,
at 6.0 - 6.5 microns,
8.0 - 12.0 microns.
NASA
will furnish data to ARF.
Results:
Data not yet available.
Radio Physics Laboratory (Australia).
Project 6.5b-30.
Camden,
CSIRO,
New South Wales,
Australia.
Birefringent airgIow photometer,
interferometers for measurement of
airglow auroraltemperatures by emission line widths,
meters,
Data not yet available.
University of Canterbury, New Zealand.
Project 6.5b-3 P.
Department of Physics,
All-sky camera,
Results:
sodium optical photometer,
C. Ellyott,
and auroral spectrograph.
National Bureau of Standards, CRPL
Airglow photometer at Mt. Haleakala,
Results:
Dr.
Christ Church.
Data not yet available.
Project 6.2B-3Q.
L3
two auroral spectro-
lead-sulfide detector for IR (cverhead),
Results:
I.
Dr. D. ?.rMartyn,
Data not yet available.
Hawaii.
of 700 km or greater.
Project 6.13b (DASA).
Optical Measurements.
John E. Hagefstration,
AOMC.
Measurements in UV, visible and IR from DAMP ship.
meters,
thermograph (IR scanner,
Results:
Very little
Cameras,
photo-
thermistor detector), radiometer (PbS).
data obtained at shot time because of weather.
Sunrise and sunset on D + 1 yielded no measurable effects.
Project 8A.1 (DASA).
Infrared Blackout and Sky Background.
Hervey
Gauvin, AYL.
Electronic scanning spectrometer in 0.35 to 0.60 micron range, 20 A
resolution, pointed at detonation (103 scans/sec).
meters 0.2 to 3.0 micron ranges.
Narrow-band spectro-
NBS slow scan spectrometer pointed 500
from horizontal, one radiometer, UV spectrometer,
and photometer packs.
All the above airborne in KC-135's in Northern Conjugate Area.
-friew
land based photometers and cameras.
Results:
Generally successful operation on 98 percent of instrumen-
tat.Lon, with some degradation at Maui due to clouds.
Northern aircraft
at 37,500 feet, 22* 43' N, 1680 24' W nt detonation.
Eastern aircraft
at 41,000 feet, 15" 53' N, 1660 23'
In general, all
equipment recorded (UV,
W at detonation.
visible, IR) strong signals, more intense and
persistent than expected.
Below is a table of results now available.
b
I
38
Long Term Debris History. Dr. Edward R. Manring, GCA.
Photometers looking at early time and long term debris history by
measuring resonant scattering of lithium, barium and zirconium lines.
Project 6.6 (DAsA).
Johnston Island, Ships 2 and 4 for early times; Tongatapu, Tutuila, and
French Frigate Shoals, Ships 1 and 2 for long term measurements.
Results: Unexpected signals were received at Johnston Island on all
four (44,54, 5535, 6130 and 6708 A) wavelengths when the instrument was
uncovered at + 30 seconds.
Suggested sources for the light are (1)
lithium, barium and zirconium debris, excited by electron or photochemical
strong euizzions due to atmospheric fluorescence which
excitation; or (2)
leaked through the filter edge.
Observation at First Twilight
Location
Johnston
D~eleted
French Frigate
Shoals
Project 6.10 (DASA).
HF, VLF, Loran-C Propagation.
Roger Whidden,
Akb2RL.
Scanning spectrometer with gratings for 3000 A, 3914 A sid 6708 A
and IR scanning spectrometers, 1 to 2 and 4 microns.
All carried in
KC-135 at 44,000 feet in South Conjugate Area.
Scanning photometers at
4278 A, 4861 A, 5577 A, 6300 A and 6479 A.
Results: No instrument results available.
Visual observation
center of aurora about 200 km west of theoretical
(160 Southern Conjugate calculated according to method of Vestine.
summarized as follows:
170 S,
1760 w).
Longest display was smoothly curved ray originating
beyond northern horizon and extending over aircraft "steady in position
and resembling a searchlight beam."
Geomagnetic field lines in same
apparent position as beam would pass Johnston Island latitude at a height
349
Results
Wavelength
Range,
Microns
Instrument
0.3-0.4
Unspecified
0.2-1.0
Broadband
dispersion
units
0.8-1.i
Filtered
photometer
i1
l.6
Lead sulfide
radiometer
1.56-2.55
R4K Radiometer
3.0-3.5
NBS Spectro-
Deleted
reter
Spatial Radiometry
IR
Project Ba.2 (DASA).
Optical Phenomenology of High Altitude Events.
Donald F. Hansen, EGG.
This project consisted of approximately 100 cameras and spectrometers
located at Johnston, KC-135 north of burst,
and Tonga.
f
For a complete list
KC-135 east of burst, Tutuila,
of instrumentation see DASA Projected
Measurements Summary.
The bulk of the film has not yet been developed and analyzed.
4o
oSo (Orbiting Solar Observatory.)
Center,
Dr. W. Hess, Goddard Space Flight
Greenbelt, Maryland.
Experiment in the UV (1100-1250 A) and 3800-4800 A ranges.
Results:
No data; satellite not operating.
Injun I Satellite, Dept. of Physics and Astronowl,
State University of
Iowa, Iowa City, Dr. Brian O'Brien, Dr. James Van Allen.
Auroral photometer (571
Results;
A)
Data not yet available.
0i~el
Los Alamos Scientific Laboratory Measurements.
Dr.
H. Hoerlin, LASL.
Refer to Appendix I for a discussion of the phennmenology of the
burst.
Vela Sierra system detectors,
photometers at Maui,
spectrographs,
cameras and
Johnston and on a KC-135 near French Frigate Shoals.
41
F.
Measurement of Electromagnetin Signal due to the Weapon
Project 6.5a (DASA).
Dr. Philip Newman,
Ionospheric Soundings and Magnetic Measurements.
AFY-RL.
Mitre Corporation had detection equipment on Palmyra, including
electromagnetic senscrs. There were a number of other electromagnetic
sensors throughout the world.
Results:
Locatiorn
Frequency
Range
Johnston
ELF
Johns ton
VLF
Kona, Hawamii
VLF
Bedford,
VLF
Date
404/
Ot
MASS.
Kauai, Tonga- 5 kc
tapu, Palmxrra
Tutuila
5 ke
Johnston
5 ke
Christmas
20 -lO00cps
Project 6.5b-3M (DASA).
Sylvania Electronics Defense Laboratory.
Dr. John T. Harding.
42
I
Figare 7
-
Christmas Island ELF Signal Facsimile
43
Four receivers in
the 50 to 500 kc (10 kc bandwidth) range monitored
electromagnetic pulse from blast.
Results:
DatI. not yet available.
Project 7.1 (DASA).
Bridges,
Electromagnetic tUnderwater Measurements.
Dr. A.
P.
Kaman Nuclear Corporation.
Electromagnetic
signatures as a function of time were measured
above and below the ocean sur-face as a means of indirect bomb damage
assessment.
Data are 35 r= filyr
VLF receivers.
recordings of oscilloscope readout of
Two VLF deck-mounted whip antennas, 2 VU,underwater
antennas (loop and trailing wire).
Result s:
De I eted
Lawrence Radia'tion Laboratory ?,easurement.
Dr.
Measurement of time interval from electromw
R.
Partridge,
LRL.
Aetic signal received
in Honolulu.
Results:
Deleted
Los Alamos Scientific Laboratory Measurements.R.L. Wakefield,
Measurement of time interval from electromagnetic
C-130 aircraft,
753 nautical miles from burst, at ll
24, 750 feet.
Results:
DeIeted
4h
LASL
signal received in
16'
N,
1150 07'
V,
II
I, 0ted
r
isi
r
I
Figure 8
EM~ Time Interval Signal on C-130 Aircraft
~753 Nautical. Miles from Bu~rst
45
G.
Biomedical Measurements
Project 4.1 (DASA).
Investigation of Chorio-Retinal Effects.
R. G. Allen, USAF, AMD,
Lt. Col.
Brooks AFB.
Rabbits and monkeys looking at the burst, plus photocells and a
calorimeter to determine incident light.
The animals'
examined after detonation for retinal burns.
eyes were
Various filters and
protective devices were tested.
Results:
723 miles,
zero.
Five aircraft at 20,000 feet at 205, 302, 430, 663 and
plus Johnston gra'.nd station 17 nautical milez from surface
Protective devices set for fast rise times apparently triggered.
Vo chorioretinal burns were found in the tested animals.
Detailed.
microscopic examination of the eyes will be made to determine if
were microscopic effects; however, these are not expected.
r
46
there
H.
Measuremenrts of Effects on Rad'ar
Note:
Small scale radar measurements of limited interest
bxe
omitted
from this compilation.
Project 6.5b-3A.
RADC Griffiss AFB, Rome,
Backscatter radar at 12.4 Mc,
second,
located at Rome, N. Y.
and pen recording of phase.
N. Y.
Gordon Weatherup.
1 kw peak power at 10 pulses per
-Magetic recording of coherent signal
Total and gated backscatter energy was
recorded.
Result.s:
Data not yet available.
Project 6b.-3E.
Naval Research Laboratories.
J.
M. Hedrick.
Madre-Bak.scatter radar at NRL Chesapeake Bay Annex using VY radar,
4.6 megawatt peak, 100 kw average power.
13-26 Mc,
round the world forward scatter,
Backscatter and
=plitude versus time, continuous
spectrum analysis versus range.
Results:
Data not yet available.
Project 6.;b-3K.
Washington,
Patuxent River Naval Air Station.
Donald Decker,
D. C.
Measurement of oblique backscatter radr at two frequencieb Detween
6 and 30 Mc;
vertical ionospheric sounder.
Results:
Project 6.2b-3.
Data not yet available.
Stanford University.
Dr. 0. G. Villard
HF backscatter radar looking off at one side of tests, using
azimuthal slewing of array- of 8 rhombic antennas (1600 ft. aperture).
Range time records of the amplitude and phase of the backscatter signals
were made;
and its
eventually a picture may be built up of the MID disturbance
motion as a function of range as well as azimuth.
Results:
Data not yet available.
47
Project 6.5b-3N.
University of Queensland, Australia.
Professor of Physics,
At Maggill,
St.
Lucia, Brisbane,
near Brisbane, latitude
there were backscatter sounders at
Results:
Pro~ect 6.9.
H. C. Webster,
Australia.
27.50 S, longitude 152.90 E,
16, 55, and 15-30 Mc (sweep).
Data not yet available.
Radar Clutter and Radar Physics Measurements (DASA).
Project Officer:
R.
L. Leadabrand,
L. Dolphin (alternate),
SRI.
A large number of radar measurements from Johnston, the DAMP ship,
and RC-121 type aircraft.
location, extent,
Object was to obtain data to deterrine the
and time history of clutter ionization due to beta
electrons at the burst location and magnetic conjugate areas; determine
its reflection capabilities,
spectral bandwidth and general characteris-
tics as a function of frequency; determine the relative deposition of
energy at the conjugate ae compared to the burst area.
The 1210,
850,
"and 398 Mc radars used an 85 ft parabolic dish in comn.
The 2Q.through
50 Mc radars used rotating log-periodic antennas in comon.
The 4 to
10 Mc radars used a vertical log periodic antenna.
AN/APS-95 radar.
The 140 and 370 Mc radars used 30 ft dish antennas.
The 52 and 3.1 Mc radars used yagi antennas.
Results:
Aircraft used
Location
Observation
Acania, near Niua Fo 'ou
looking normal to field
lines
RC-121 Aircraft, 285 n
miles SE air zero
RC-121 Aircraft, 41' n
miles SE air zero
RC-121 Aircraft, South
Conjugate Area
Deleted
Johnston Island HF
Sounders
Johnston Island, 398 Mc
Johnston Island, 850 Mc
Johnston Island, 1210 MC
49
Pc
J
Project 7.2
Radio-Frequency Radiometry.
Project Officer:
James H.
Pannell, Lincoln Lab., MIT.
Synchrotron radiation at 50 and 100 Mc was measured from Palmyra.
K and S band radar Dicke-type radiometer systonns mapped the disturbed
region from Johnston.
Synchrotron radiation was observed from Palmyra, randomly
polarized at early times. Other data not yet available. See Appendix 2.
Results:
Project 7.9
Officer:
Nuclear Effects on Operational Shipboard Radars.
:t. Cdr. J. S.
PrQject
G-ischy (Op Nav OP-353).
Ships assigned to JTF-8 in and around the operation areas tracked
targets of opportunity from shortly before detonation until no further
effects were apparent.
Results:
Record data by scope photography.
Data not yet available.
Effects on Nike-Zeus Radar System from Kwajalein Atoll.
Officer (AOMC),
Kwajalein.
Target Tracking Radar (TrR),
Acquisition Radar (TAR)
Missile Tracking Radar (M{R),
Target
were all turned on at Kwajalein and looking
toward the burst.
Results:
Nqike-Z~As Project
Deleted
51
I.
Direct Ionization Measurements
Protect 6.3
D Region Physical Chemistry.
Project Officer, Warren
Berning, EL.
Mass spectrometric measurement of positive and negative ion species
above 30 km; also ion trap. Instruments rocket-borne from Johnston
Island.
Results: Data not yet fully available; some instrumentation
difficulties were encountered.
Deleted
Project 6.4.
E and F Region Physical Chemistry.
Project Officer:
W.
Pfister, AFRL.
Mass spectrometric measurement of positive ion composition as a
function of time and altitude above 100 km using instruments rocket-borne
from Johnston Island.
r
Results:
Project 6.7.
Whitaker,
No data recovered because of telemetry failure.
Debris Expansion Experiment.
Project Officer:
Lt. W.
AFSWC.
Rocket-borne Faraday cups measuring the presence of ionized debris
plasma and betas.
Results:
Data not yet available.
f
52
J.
Communications and Ionospheric Disturbance Measurements.
Project 6.2
Rocket-Borne Gamma Ray Scanner.
Project Officer:
Warren
Berning, BRL.
Project 6.4
Officer:
E and F Region Physical Chemistry.
Rocket Probes.
Project
W. Pfister, AF(RL.
Three frequency propagation experiments using rocket-borne phase
coherent beacons (37,
148, and 888 Mc).
Ground receivers mixed and
frequency multiplied the telemetry signals to produce dispersive Doppler
and Faraday rotation data.
Amplitude of each frequency recorded.
All
rockets launched from Johnston.
Results:
Rocket Launch Time
Project Number
Location of Measurement
H -600 seconds,
6.4
300 to 325 km altitude
H +420 seconds,
6.4
Flight Path Azimuth 148&
(true) below 350 km
H +1203 seconds,6.2
Flight Path Azimuth 28*
(true) 300 km altitude,
128 km horizontal
distance
H +40 minutes,
Project 6.3
6.2
Electron Concentration
D•leted
Flight Path Azimuth 240
(true)-
D Region Physical Chemistry.
Project Officer:Warren Berning,ERL.
RF antenna impedance in the low megacycle region was measured as the
rocket passed through the debris cloud.
Results:
De le ted
53
De feted
Project 6.5b-B.
Magnetic and Electric Field Measurements and Cosmic
Noise Absorption.
C. Stone, ARF.
Sets of riometers at Tonga and Tutuila using various types of antennas.
Results:
L
See Appendix 2.
Deleted
54
Project 6.5b-lD:
HF Phase Measurements.
C. Stone, ARF.
Data on addItional ionization produced in D, E and F layers of
ionosphere above the South Conjugate Area by broadcasting CW at 3.5,
7 and 9 Hc from Tonga to Tutuila.
Results: Data not yet available.
Satellite Data Acquisition.
Project 6.5b-lE.
C. Stone, AR.F.
Obtain signal strength data on satellite transmission to measure
ionospheric disturbances. A 4.076 kc tone generator in Injun I and 12.5
kc in TRAAC,
transmitted to Tonga.
Data not yet available.
Results:
U. S. Army Signal Missile Support Agency, White Sands,
Project 6.5b-3B.
New Mexico.
Contact:
NCOIC at Ionosphere Station.
Vertical Ionosonde,
Results:
1-25 Me.
Data not yet available.
Project 6.5b-3D.
Naval Electronics Laboratory, San Diego, California.
Projec4 -
Dr. T. J. Keary, NEL, San Diego.
fficer:
Measurement of phase and asxlitude of VLF (l1 kc) link from Arizona
to San Diego.
Results:
Data not yet available.
Poject 6.,5b-3E. Naval Research Laboratories. Contact J. M. Hedrick.
Recording of phase differences of VLF (10.2 kc) between NRL in
Washington, D. C., and Bodo, Norway.
Results:'
Data not yet available.
Project 6.5•b-3F.
Conmercial Communications.
C. Stone, AEF.
Information was obtained on circuit outages, corrective measures
taken and other sigrificant effects. Also propagation 1inks through
the D and F layers passing in the vicinity of Hawaii, north to Alaska
r
55
and south to Australia were of particular concern.
A large number of
links were monitored.
Results:
Data not yet available.
Project 6.22-3J.
HRB-Singer Inc.
Jr.,
State College, Pennsylvania.
Science Park,
Contact:
Dr.
Chalmers F. Sechrist,
VLF amplitude and phase measurements were made at State College for
MaA (18 kc from Balboa) and NIM
(18.6 kc from Jim Creek, Washington).
Also atmospheric noise near 18 kc was measured.
Results:
Project 6.5d.
Data not yet available.
Ionospheric Soundings.
Project Officer:
F. H.
Dickson,
USASRPA.
Ionosonde at Johnston and Kwajalein,
and a "Pinwheel Experiment"
determine off-great circle path effects on HF communications.
Receivers
at Adak, Okinawa and Palo Alto to record azimuths of strongest Iignal
from Hawaii.
r
Results: Location
Results
Okinawa
Adak
Johnston
Deleted
I
SKwajalein
Kauai
r
56
to
Project 6.5b-30:
Radio Physics Laboratory.
Dr. D. F. Martyn, CSIRO,
Camden, New South Wales, Australia.
Vertical ionosonde,
rotating backscatter measurements at 12,
18,
30 Mc.
Results:
Data not yet available.
Project 6.5b-3Q.
National Bureau of Standards, CRPL. C. Stone, ARF.
Vertical ionosonde, riometers at Huanceayo, Peru (on magnetic
equator).
Results:
Data not yet available.
Project 6.5c.
Vertical Sounding of the Ionosphere.
William Utlaut,
CRPL.
Project Officer:
Vertical incidence ionosondes at Wake, Tutuila, Y.anch F'rigate
Shoals, Maui, Canton, Midway and Tongatapu.
Results :
Chronology from Midway and Maui (Northern Area.)
Time
Observation.
Within I second
0
Remainder of night to sunrise, Maui and Midway
Maui. day-time 9 andi 10 July49
Morning 11 July, Maui
5
I-
57
Time
Obse vation
* 20 minutes, Maui
+ 35 minutes, MidwVy
peted
+ 30 minutes to + 5 hours,
Maui and Midway
Sunrise
Project 6.8.
Riometers.
T' •Ject
Riometers at Oahu, Johnston,
FiJi, Palmyra, MV Acania,S1,
S2,
Officer:
S. Horovitz,
AR.
Tutuila, Tongatapu, Midvay, Wake,
S3,
s4, S5 and DAMP ship.
300 Mc
radiometer on Johnston Island.
See Appendix 2 for discussion of data.
Results:
Project 6.9.
Radar Clutter and Radar Physics Measurements.
Officer:
L. Leadabrand,
R.
High frequency radea
&I
L. Dolphin,
SRI.
sounders at Johnston Island.
Deleted
5
58
?'oject
project 6.10.
Whidden,
HF, VLF, Loran-C Propagation.
Project Officer:
Roger
AFCRL•
Step frequency ionosphere recorder,
height for frequency record.
in
KC-135,
giving a
Three HF receivers at 10, 15 and 20 1c.
Loran-C phase and amplitude recordings.
ionospheric recorder at Fiji.
and Palqrra.
i-25 Nc,
Also ground based step frequency
HF receivers at 5,
10 and 15 Mc at Fiji
Loran-C recorder on Maui and VLF receiver on Maui monitoring
NIM, (19.8 kc from Honolulu).
Results:
At H hour KC-135 aircraft at 177 0 47'W,
Location
Measur eme nt
Under Southern
Conjugate Aurora
Vertical
ionospheric
recorder
( F~ii)
Results
Fiji and KC-135
Reception of
Tongatapu 4 and
6 WHF
transmission
KC-135
Loran-C receptior
from Hawaii and
Kur e
KC-135
NPM Oahu (19.8 kc)
Midway to Maui
HF Data Link
Midway to Mau
12.229 Mc
Midway to Maui
9 .o43
Midway to Maui
4.557 Mc
Wc
59
15822'S at 43403 ft.
Results
Location
Measurement
Maul Phase Swept
Interferometer
253,
Maui
255
Maul
Radio station
reception
Maui
VLF and Loran-C
Phase and Amplitude
147,
52 Wc
-.
of 19.8 kc
Project 6.1i.
IU CommunicaLions Simulation Experiment.
Project Officer:
Howard Kitts, USASRDL.
A complex set of 4 Granger sounders (Okinawa,
Roi-Namur,
Canton, and
Kauai) and 8 receivers (Tutuila, Fairbanks, Palo Alto, Mfdwsy, Tongatapu,
Rarotonga,
Wake, Viti Levu arni Hawaii) thro'*,hout the Pacific area,
operating at 4 to 63.6 Nc.
Monitoring of NBA and other commniurcation
links.
Resu-lts:
,eIeted
U
Observation
Location
Okinawa to Palo Alto, Hawaii, Tutuila; Roi-Namur
to Fairbanks, Palo Alto; Canton to Wake, Fairbanks,
Hawaii; Kauai to Wake, Midway'; Kauai and Canton
backscatter.
Deleted
Kauai-Tutuila, Roi-Namur-Wake, Okinawa-Fairbanks,
Roi-Namur-Thituila, Canton-Midway, Canton-Palo
Alto, Canton-Rarotonga, Canton-Tutuila and RoiNasur - Kauai.
Other paths.
6o
L
Observation
Location
Deleted
Project 6.12.
A.Bena,
Piggback Satellite Packages.
Project Officer:
Capt.
R.
AFL'.
Retarding potential probe and ion trap, and. hynchrotron noise
measurement from Discoverers 1127 and 1128.
Results:
Project 7.2_.
No data.
Satellite not operating.
Radio-Frequency Radiometry.
Pannell, Lincoln Lab.,
Project Officer:
James H.
M.I.T.
Measurement of synchrotron noise with VHIF rotating dipole assemblies
at Palnyra,
and Dicke-ty-pe radiometers systems at Johnston,
61
CL
to measure
~1
AJei
Receiver Location
Observation at Receiver
Oahu
Midway
Deleted
Viti Levu
Palo Alto
L
Data not yet available.
Wake, Canton, Samos,
Rawaii, Roi-Namur
Signals in the HF band from various places were received on~a KC-135
located 200 miles NE of Johnston.
Transmitter' Location
Observation at Receiver
March AFB, California
I
Conmrunications from Krajal,-in:
Nike Zeus Prcject (AOMC)
All communications circuits monitorede
63
Kvajaletn.
Frequency and Receiver
Description
location
13 Mc to Honolulu
20 kc to Honolulu
9,
12, 15 Mc to
D eeleted
California
14 Mc to Alaska, Fax
East and Australia
4 Mc to U. S. A.
Sandia Corporation Measurements.
J.
J.
Sandia Corp.
Miller,
Signal strengths were measured from the rocket-borne telemetry
systems used in
other Sandia experiments.
The following data were reported from the Kauai receiving
Results:
station:
Rocket
Frequency
200 Mc
Altitude
160o km
Deleted
20o Ie
50
6 kMc
160km
Project 7.5:
VLF Monitoring Through Nuclear Environment.
&
Project Officer:
Capt. L. R. Raish, CNO.
A worldwide VLF net check on 14.7, 22.3,
Results:
Data not yet available.
LF Monitoring Through Nuclear Environment.
Project 7.6.
Capt. L. R.
18.6, 19.8, 17.44 and 18 kc.
Project Officer:
Raish, CNO.
A check of LF communications throughout the Pacific area, transmitted
Receivers at Guam, Adak,
at 185 ke (Honolulu) and 155 kc (Guam).
Honolulu, Japan and shipboard.
Results:
f
Data not yet available.
Project 7.7.
Capt.
L. R.
M Ground Wave Monitoring Through Nuclear Environment.
Raish,
CNO.
A check on ship-to-ship MF communications in the 2 to 3 Me range.
Results:
Data not yet available.
Project 7.8.
HF Radio Teletype Broadcast Monitoring Through a Nuclear
Environment.
Project Officer:
Capt. L. R. Raieh,
CNO.
HF radio teletype transmissions were monitored in
Results:
Project 7.11.
Data not yet available.
Nuclear Ftfects on Certain Operational Electronic
Navigation and Identification Equipment.
S.
the Pacific Area.
Project Officer:
Lt. Cdr.
J.
Grischy.
To determine the effects on TACAN,
aircraft operating in the Pacific area.
Results:
Data not yet available.
65
IFF/SIF equipment with ships and
K.
Magnetic Field Measurements and Earth Current Measurements
Project
6
Officer:
.5a.
Ionospheric Soundings and Magnetic Measurements.
Project
Dr. Philip Newman, AFMRI.
Variometers at Hawaii, Midway,
Palmyra,
Palo Alto, Huan ayo, Genoa.
Earth current probes at Hawaii,
Wake,
Tutuila, Canton, Okinawa,
Palmyra, Tutuila, Ghana, Alaska, New Zealand.
Result•:
Variometer Readings
Location
Readings
Kauai
Canton
Deleted
Tutuila
Trinidad
University City,
Pa.
Kona , Hawaii
Wake
4
Project 6.5b-iB.
Magnetic aud Electric Field Measurements and Cosmic
Noise Absorption.
C. Stone, ARF.
MYanetometers and buried electrodes at Tongatapu and Tutuila.
Results;
Measurement
Results
Earth Current
Deleted
Magetometer N component
change
66
Magnetometer declination change
Deleted
Magnetometer Z component change
Project 6.5b-lE.
Satellite Data Acquisition.
C. Stone, ARF.
Magnetic field strengths from Injun I and TRBAC satellites.
Results:
Data not yet available.
ProJect .L b-.
SRDL, Ft.
Monmouth, N. J.,
Robert Noyes, Caox
Evans
Signal Lab.
Earth current and magnetometer measurements in the U. S. A.
Results:
Data not yet available.
Project 6.5b-3N.
Webster,
University of Queensland, Australia.
Contact:
H. C.
Professor of Physics, St. Lucia, Brisbane, Australia.
Flux gate-type geomagnetic variom.:ter near Brisbane, Australia.
Earth current and geomagnetic micropulsation measurements near Brisbane.
hesults:
Data noL. yet avajiaable.
Project 6.5b-30.
Radio Physics Laboratory (Australia).
F. Martyn, CSIRO, Canden, New South Wales,
Contact:
Dr. D.
Australia.
Z-magaetometer in Australia.
Results: Data not yet available.
Project 6.5b-3P.
Zealand.
Department of Scientific and Inaustrial Research, New
Contacts:
J. W. Beagley, A. L. Oullington.
Flux gate magnetometer in New Zealand.
Results:
Data not yet available.
67
Project 6.5b-3Q.
National Bureau of Standards,
Askinia magnetometer at Huancayo,
Results:
Data not yet available.
Project 6.5e.
Magnetic Measurements.
CRFL
Peru.
Project Officer:
Dr. H. A. Bomke,
Tutuila, Da.llas,
Texas,
USASRDL.
?Megetometers
locations.
at Waimea (Hawaii),
Earth current measurements in
Results:
Instrument
Waimea, Island
of Hawai"
Large loop magnetometer confirmed -r
Florida.
Chronology
metastable hell',
magnetometer
Tutuila
Metastable helium
magnetometer
Columbus,
S.C.
Large loop
magnetometer
Lebanon State
Park, N. J.
Large loop
magnetometer
Lebanon State
Park, N. J.
Rubidium Electron
Spin Magnetometer
Dalla.s,
Metastable helium
magnetometer
Texas
Baxter State
Large loop
Park, Maine
magnetometer
\
68
and other
Project 6.7.
Debris Expansion Experiment.
Project Officer:
Lt.
Whi taker, AFSWC.
Rocket-borne magnetometers launched from Johnston.
Results:
Equipment apparently operated properly but data not
yet available.
rr
L
69
W.
T,.
Miscellaneous Measurements
Falling-Sphere Project.
Project 9.1a.
Project Officer:
Dr. K. S. W.
Champion, AFCRL.
Measurement of ambient air density at 30 to 100 Rm, using a
sensitive accelerometer to measure drag on a sphere ejected from a rocket.
Results:
Data obtained but not yet available.
Measurenent of Upper Atmospheric Winds.
Project 9.1b.
Dr. K. S. W.
AF=RL.
Champion,
Nike Cajun rockets containing sodium vapor experiment to measure
wind and wind shear at 230,000 feet to
&80,000feet.
Rockets launched
at pre-shot and post-shot twilights.
Results:
Each payload operated normally.
successfully skin tracked by the Range Tracker.
Both rockets were
From the dusk rocket
data were obtained from 200,000 feet (61 km) to 432,000 ft (132 )M).
Shears were noted at 80 and 1.15 ki.
Winds appeared typical.
dawn rocket data were obtained from 150,000 feet (46
From the
on) to 429,000 feet
Two marked shears were observed, and there may have been some
(131 kim).
slight disturbance of the atmosphere at this time.
Lawrence Radiation Laboratory Measurements.
Radio Chemical Samplers.
F.
C. Gilbert, URL.
1.
Rocket-borne aluminized nylar balloons were inflated prior to
entry into the debris area; after passing through the area, the balloons,
with the debris adhering to them, were punctured and drawn into a small
container.
2.
The containers were sealed afhd were to be recovered.
Small sample collection cups were carried on the pods.
Results:
The rocket-borne samplers were not recovered.
borne samplers were recovered;
f-
-,
Deleted
70
The pod-.
Sandia Corporation Measurements.
Rockets SJS-151,
J.
Scott, Sandia
152 contained rad-chem samplers which used 6 foot
Wlar sails which were to be retracted after exposure,
recovered.
Results:
Containers were not recovered.
71
sealed and
APPENDIX 1
STARFISH PRIME
JTF-8
PEEIDMINAY FIELD REPORT
STATUS AS OF H + 5 DAYS
1962"
"With Additions as of July 31,
q
By:
rAl-I
Herman Hoerlin,
IASL
STARFISH
JTF-8
TU 8.1.1, IASL
Preliminary Field Report
Status as of E + 5 Days
"With Additions as of July 31, 1962"
Berman Hoerlin
This report is
based on cursory inspection of photographs,
records and
data supplied by the following project officers and staff members and
also by N+G:
E. Bennett,
R.
Bussard,
D. Holm, R.
Kiehn,
Stone,
Westervelt; also H. Argo,
D. R.
R. Tascbek.
Tbp
R.
K. Mitchell, M. Peek,
J.
Cowan,
T. Godfrey, M. Bawe,
W. Began,
D. Steinhaus, S.
Conner,
J.
Coon,
S.
Singer and
-ontributors of all fTsk Unit members participating in
the high altitude phase of Dominic are acknowledged.
Special thanks are
due to D. R.
Kiebn, B. M. Peek,
and B.
Westervelt,
E.
Bennett, D. Steinbaus,
R.
Hayes for taking on many difficult operational responsibilities.
The Sandia Corporation was responsible
or small rocket firing and tele-
metry;
Scott and J.
the assistance of D.
Shuster, J.
valuable.
AI-2
J.
Miller was in-
ABS MACT
The LASL H + 5 days field report on Starfish reviews in a cursory
fashion the phenomenoloe~cal features of this event as they are
;tood at this date.
ruder-
The early hyd•rodynamic debris expansion in vacuum
was observed and found to have a velocity of 2000 k_,/sec; the later expansion is mainly governed by the geomagnetic field at higher altitudes
and by air and field at lower altitudes.
Very large fractions of the
debris were deposited north and south of the burst at the intersections
of the magetic f,.eLd lines through burst and through points above the
burst with the at -'i':bere at altitudes of about 120 to 150 km, producing
north and south large localized areas of strongly ionized air.
bination sepears to be slow.
Recom-
The brightness-tiL'ne history and the spatial
characteristics of these phenomena were recorded with photographic,
photoelectric and spectroscopic
instrumentation; data obtained are
believed adequate to arrive at an understanding of the physical phenomena
occurring during and after uucb an ene-gy release at the Starfis5
%lti-
tude of 400, km.
Diagnostic methods
other characteristic
instrumen'r
*
'cr measuring X-ray yield, time.interval and
sovrce characteristics were developed; rocket born
.on demonbtrated a high degree of space testing capability.
Ground bpced optical methods were found useful.
Detection equipment of the Vela Sierra type was operated with good
success and range and sensitivities of the method were found to be at
least aq good as predicted.
'
The &cientific fringe benefits that cwi be derived from a lLrge
array of data appear to be very rewarding indeed.
/-
*
e-ational InformatIon
A.
Bur5t Location and Burst Time
Starfish was fired Juiy 8, 2300 Hawaii time.
Burst location
was well vithir. the erro.: box; nominal altitude was 400 km; ground zero
about 3)6 ka
Ac-
south of Jonnston Islanad on the georagnetic neridi-an.
cording to latest information provided by Sandia Corporation the deviation from air zero was
A X = - 1890 feet N
B,
v.-A Y
2190 feet E
A Z
+ 617 feet H
Station Operation
1.)
Johnston Island.
The station operated according to plan
with 9% of the instrumentation getting data.
At shot
time the direct line of sight vas almost clear,
only a
thin cirrus layer interveniln.
for transmission is
2.)
Maui.
The preliminary estimate
50%.
The station operated according to plan with about
805 of the instrumentation getting data.' "Te dire'ct line
of sight was cle'r, surrounded by a comfortable hole in
the clouds.
However,
a large part of the sky above burst
position was obscured ;reventing data acquisition from
late phenomena.
5-)
KC-135 Aircraft.
The LASL instrumented KC-135 took off
from Hickam Air Force Base, Honolulu; at 203.5 hours
Hawaii time, and flew -Lo geographic position 240,
1660,
12' W, arriving there at 2158 hours.
14 '
1,
According to
aircraft navigational instruments at detonation the
geographic position of the aircraft was 240, 08' 45" N,
1650,
53' W, its altitude was 39,250 feet, and the geo-
graphic headIng was 114° 45'.
This position is approxi-
mately 3 nautical miles east of the planned position at
detonation time and 4250 feet higher than the planned
altitude.
Al-4
These differences in altitude and position would be expected to produce a change in
the burst location of about 0.30
azimuth and about 0.070 elevation; both errors are well within
the field of view of any instrument used on the aircraft.*
At
detonation time, the aircraft was above all detectable clouds.
The pre-shot computed line of sight distance from. the aircraft
to the burst is
1040 kn.
Instrunentation worked according to plan with more than
90% of the units getting data.
4.)
Kauai.
All eight LASL instrumented rockets flew and good
telemetry signals were received.
All instruments operated
according to plan and yielded data.
5.)
Arguello.
Arguello locked on the JTF-8 count at minus
780 seconds and both vehicles were fired at the proper time.
However,
vehicles.
1.
no data was obtained due to the failure of both
Details are:
Telemetry contact with the Astrobee was lost about 15
seconds &rter launch.
The vehicle apparently "disintegrated
early during the powered phs-e of flight.
but not yet definitely known,
Sare
being evaluated in
Cause is
suspected
and telemetry records and photos
an a'tbempt to determine reason for fail-
ure.
2.
Telemetry contact with the Argo was lost about 385 seconds
after launch, and radar track indicates splash at about 410
secondu after launch.
Preliminary investigation indicates that
the second stage igniter fired, but did not ignite the propellent and because of vehicle design this would also prevent the
*
third stage from firing. The fourth stage fired as planned.
7/31/62 - Subsequent analysis of one of the aircraft cameras records
that the aircraft was probably mispointed to a greater degree.
Al-5
3.
Obviously, no diagnostic data was obtained because pay-
loads impacted prior to event time.
4. Preliminary evaluation of the telemetry records indicate
that the entire payload on each vehicle was functioning properly until vehicle breakup or splash.
Pre-launch calibrate
signals were normal, and DC level of detectors during flight
appeared correct.
Al-6
II.
Phenomenology
A. Early Debris Epansion
This expansion phase is shown in a good framing camera record,
taken from Johnston Island, parts of which are reproduced in
It
Figure 1.
appears that the bomb materials are separated into two parts, a,
central core which expands rather slowly and b,
expanding shell.
related.
It
is
the
an outer spherically
not certain to what extent core and shell are
Hydrodynamic expansion of debris was expected to proceed in
spherical fashion without leaving a substantial core behind.
COe may
therefore consider the possibility that the core represents the upper
part of the warhead which contains the primary and much of the f'using
and firing equipment,
In any case the separation of the debris into two distinct
fractions has a bearing on the later explosion history.
The diameter of the expanding shell is
500 microseconds,
approximately 2 km at
corresponding to a mean expansion velocity oi 2 cm
per shake.
The subsequent expansion was recorded with a total of at
least four, probably five 35 mm Photosonic cameras operating at Johnstoa
Island, Maui,
and in
the aircraft.
good, well resolved data.
and little
Me majority of these pictures show
Inspection so far has been very superficial
can be sAd at this time with the exception of the following.*
r
Deleted
A1-7
I
Figure 1
This is
a partial reproduction of a Model
record taken from Johnston Island.
6 - 40" - Framing Camera
Full coverage of 160 frames at
approximately 5 microseconds between frames was recorded with good
densities.
The lower 3 framesl of the enlarged reproduction to the right were
taken during the first
15 microseconds.
This part is
overexposed and
shows also a series of lower density images of the very bright core,
resulting from off-axis window reelections.
The second row shows frames 58, 59 and 60; the third row frames 85,
86 and 87 and the upper row frames 121, 122 and 123.
appearing in
the periphery of the latter pictures is
The dense spot
probably the missile
booster.
The main film is
exception of the first
amenable to brightness evaluation, with the
frames.
These in
turn can be evaluated from the
color-film-bipack, which shows well developed images during thlg_-hase.
Not reproduced here are the data obtained with the Model 104-32"
streak camera.
This camera was running successfully and yielded two
I
well exposed bipack films, which should also give good dat:..
_I
I
1
.J
J
A1-8
Figure la.
This is a reproduction of the first
frames of an EG+G Pbotosonmc
film, 35 um, taken from Johnston Island at 2600 frames per second.
J
I
'i
:1]
I
Al-b/H-i
~
J
booster and with the three pods is clearly recorded; it
in
= Photosonic records,
70
Figures 2 and 3.
reproduced,
one of which is
is also visibj .
in part, in
The booster appears very bright for a relatively long
time and - as will be described later - yields also an interesting
spectrum (Figure 12).
The early photographs have not been evaluated yet in
brightness versus time,
terms of
but should yield good results.
Useful early debris brightness time data were recorded photoelectrically, on all
three stations; the more or less collimated photo-
detectors recorded incident flux versus time.
The problem in
-all
cases
was to eliminate the contribution -ifthe X-ray excited air fluorescence
which,
while not as bright as the source in
covers a very large area and is
terms of surface brightness,
therefore substantial.
Successful
attempts were made to differentiate or eliminate the fluorescence light.
shown in Figure 4.
One "Direct Optical" signal trace is
Preliminary
analysis shows a shape not strikingly different from the predictions by
Longmire et al in
IASL document T-1316; the peak amplitude is
however,
three times higher than calculated - though well within/the safety
is
Analysit-of otl'er detector data
eyeburn calculations.
factor used in
in progress.
B.
Late Debris Expansion
-
-
The description of the later phases is
rather inaccurate and
based on one rather
may require serious revision later' because it
is
cursory inspection of motion picture and still
photographs only.
No
geometric or densitometric readings have been taken.
Slow EG+G Mitchell camera films taken on Maui create the impression
that the outer shell of expanding bomb materials assumes, after a few
frames,
i.e.,
at H + 1/25 to 1/10 sec,
an elongated ellipsoidal shape
with the long axis oriented along the magnetic field lines.
This is
a
fairly well delineated pattern, that continues to develop for a long
time thereafter,
indicating that at least a substantial fraction of the
bomb debris remains ionized.
One gains the impression that at this
Al-12
TI Pr e 2
Frames 0 to 7 of Photosonic record taken from aircraft in southwesterly direction.
Framing rate 300 per second; focal length 135 =;
distance to burst 1040 km. The debris expansion is shown in the upper
left; close inspection reveals presence of booster and of all three pods
and interaction of debris with them. The lower right shows the growth
of the "near geomagnetic beta ray pa cake."
This is
I
1
a contact print
from the 70 mm original.
Photo by EG+G.
4.
I
I
s
-,4
!
ii
U
!
Figure
Continuation of the 70 mm Photosonic record shown in
frames 18 through 26.
This picture series shows the growth of beta ray
pancake and the beginning of the debris pancake.
shown as a slowly growing bright spot in
frames.
Eventually it
Figure 2,
I
The debris pancake is
the lower right section of the
extends (not shown) to the same size as the beta
cake but exhibits much greater brightness.
Photometric analysis ought
to yield valuable data.
Photo by EG+G.
I
I
I
I
I
1'
Al-15-p
re-.t (i.c'i,.al bte-tion System
Deleted
Al-?
stage a large fraction of the debris is
following the field lines in an
upper, southerly direction; the fraction moving down, north appears to be
somewhat smaller.
The development of the northern branch is
documented
rather well in the 70 mm Photosonic film, parts of which are reproduced
in Figures 2 and 3.
A good 35 = Mitchell camera color film, also
In these films one
taken from the aircraft, supplements this picture.
observes very clearly the arrival of a large stream of beta particles
This
followed by a much more intense and rapidly expanding debris beam.
latter phase is
very pronounced in the later frames of the original film,
which are not reproduced here.
Photometric analysis of the cake photo-
graphs may permit an estimate of the fraction of bomb debris deposited
here.*
We also hope to gain related information from spectral data.
One aircraft spectrograph was pointed at a point below the burst.
Be-
cause of the lateral expansion of the "magnetic debris pancake" into the
line of sight a well exposed record was obtained.
This time integrated
spectrum "Lower Hilger Medium Quartz Spectrogram" is
5; its
reproduced in-wigure
doinant features are air-emission; whether bomb debris are re-
corded among the many so far unidentified weaker lines remains to be
seen.
The strong pancake expected by some to develop directly underneath
,he source was apparently very weak indeed.
There is
diffuse light
emitted ficm the space belov the zero point for sorie time; however, this
emission could possibly be produced by the "afterglow" phenomenology of
the X-ray excited air and by fission ganma rays.
The upwards motion of the debris is
not all its
very fast and is
features are clearly understood.
However,
well documented;
three phases are
evident; some are demonstrated in Figure 6:
-
7/3/62 - Rough Photometric analysis of the debris pancake bright-
ness i'i-egraTed over time and space yields a total kinetic energy for
tre incoming debris
1)eleted
AI-18
a)
Broad diffuse and narrow sharp streamers move from a large
core to the "upper right," that is north from the risin&
debris; they are believed to arc cver the aircraft and
French Frigate Shoal until they hit the atmosphere at
points 200 - 300 kn north of French Frigate Shoal.
The
auroral display there was described as being spectacular
and unexpectedly brilliant.
.)
c)
The Mitchell camera operating in the aircraft shows distinct streamers moving apparently straight up; thus, some
debris may have escaped into space.
Injection into the southern magnetic pipelines was very
atrong and is well demonstrated in Figures 6a, b, and c.
Intercsting enough and hard to understand is the seeming
reversal of this southerly trend.
Whether this is
due to
field distortion or due to a misleading perspective can
d)
not be firmed up yet.
7/31/62 - Figure 6, frame d, shows streamers that originate
along the right edge of the frame and move down to the
left with apparent strong magnetic focusing action along
the earth's field lines to the south.
At thie dtc.ge it
is too early to state-vhether or not we will
be able to account for 'he debris disposition quantitatively and with
adequate accuracy.
The amount of data collected is however large and
the chances for success are good.
Many records and observations cannot be incorporated in this
report; two picked at random are added.
One observation deals with a detailed phase of the early
debris expansion.
In frames 19 and 20 of Figure ) one observes at the "near geomagaev . beta ray pancake" in the lower right the beginning of what
appears to be the debris pancake.
Al-20
Deleted
Figure 6
Reproductions of four 2-1/4 x 2-1/4 color shots taken by W. Regan
from KC-135.
a.)
F + 25 sec, f = 38 m,
b.)
H + 35 sec, same optics.
c.)
H + 50 sec, same optics.
d.)
H + 180 sec,
field of view at burst-580
x
580 km.
f
80 mm
field of view at burst
300 x
300 km.
Exposure time 15 sec.
-
I
AI-21
J
veleted
However,
it
has been calculated by Longmire* in
1959 that
hydrodynamic acceleration of the surface layers of a bomb in
vacuum may
lead to heavy particle velocities of this order of magnitude.
These
fact particles should bi
hard to see at the source,
one Fuotosonic record
's a halo-like extension of the expanding
sphere,
It
is
but indeed at least
which could conceti'ably consist of such a particle precursor.
hard to visuali.ze other mechanisms that would explain the early
appearance of the interaction of debris with the Aenser atmosphere.**
The second cbservation is
a series of good auroral vpectra
taken by S. Stone from the USS Iwo Jima which,
over a period of 39
minutes, covers various phases of the northern and southern branchez- cf
the debris aurora.
No aaalycic haz
Several of tnese spectra are reproduced in Figure 7.
been attempted yet, althu.gh the prevence of veil krow4n
auroral lines and bands is
*
clearly evident.
Argo, Hoerlin, Longrnire,
-
Petschek and Skumanich,
Applications of Nuclear Explosions, Plovshare'eetin•,
California, May,
**
Scientific
San Fraunci, o,
1959.
W. Ogle suggests the alternp.te possibility that delayed fission
products might be tiae source.
A I-?_
A).-23
III.
Diagnostics
A.
Rocketborne Instrumentation
The following is
taken from J.
Coon's monthly laboratory report
for August.
Rocketborne diagnostics were attempted on the July 8 Starfish
Prime shot from Johnston Island, with rocket launches from Kauai, Hawaii
Although readiness status at
and from Point Arguello, California.
Arguello appeared to be good and instrumentation checkout was satisfactory,
no data were obtained because of failui'es of both of the two rockets
launched,
an Astrobee 1500 and an Argo D-8.
At Kauai,
of the eight Nike
Apache rockets launched (by Sandia Corp.) carrying IASL diagnostic
instrumentation, all eight rockets and their radtiotelemetry performed
satisfactorily, and successful diagnostic data were obtained from all
It is felt that the objective of proving the feasibility
instrumenuts.
of getting good bomb diagnostics from instrumented rockets in a space
testing program is in some measure already achieved, although further
participation
D e I e t di
with the hope of getting data from
Point Arguello as well as Kauai would add much to the development of
techniques.
Presented below are the data obtained from the Kauai launcbes
on Starfish Prime.
to be in
The rocket altituaes at burst time were highi enough
line-of-sight with negligible attenuation by the residual
atmosphere.
Distance from burst point
was abouc 1300 )on.
Deleted
to -ocket instruments
Quoted values of diagnostic data presented below are
based on absolute sensitivity calibrations carried out i, the laboratory.
B.
Neutron Tied
d
Neutron arrival Aime bietr
from the first
-
records appear 'o be good for times
arrival of neutrons of enery- about 16 MYv to arrival times
of several seconds.
However,
atmospheric scattering becomes increasingly
important for times longer than those corresponding to 10 Mev line-of-sight
The experimental value for the
neutrons, and has not yet been evaluated.
integral of the number of neutrons escaping from the bomb, on the
4IJ-25
Deleted
F.
Optical, Groundbased Inst nentation
1.
Time interval
The gamma ray excited air fluorescence was measured with
moderately •- .,11ted photoelectric detectors using various optical bandpass or no filtera.
The data obtained are as follows, on basis of pre-
liminary analysis:
Johnston Island:
Deleted
KC-135
The time interval detectors used on Maui vent off scale probably due to
an unexpectedly large electromagnetic signal and inadeqaate shielding.
Figure 6 shows a reproduction of two timc interval traces taken on Johnston
Island.
2.
X-ray flux measurements
The X-ray excited air fluorescence was measured from all
three optical stations with photoelectric detectors collimated to 3' and
looking off-burst by 1.5° to 20P.
with good time resolution.
f
A total of 15 records were obtained
The frequencies Belected are mainly from the
N2 second and first
o
positive and the N2 + first
negative systems; i.e.
0
0
4o6o A, 8911 R, 3914 A, 4709 A, 5228 ý and others.
None of the data are
completely reduced in view of need for further analysis of air transmission
corrections.
The late transmissometer measurements on Johnston Island were
disturbed by rocket light.
Furthermore the observed relative intensities in
the 0,0; 0,2 and 0,3 sequences of the first
abnormal)
negative system were again
L eteted
being of lower intensity.
- short wavelengths
The aggregate of data is,
however,
so extensive
(including the photographic spectroscopic records) that one can be confident to obtain eventually usetul quantitative numbers.
Deleted
Av~
i)>oI44-~
Ak-2)
IV. Vela Sierra
A.
All Sky Systen
The 1960 model of the all sky detection system was operated at
Johnston Island with all
three channels, 3914, 5228 and the background
charnel at 4140 ý operating properly.
Neutral density filters had to be
employed to reduce the incident fluxes by eight powers of ten.
were obtained in all
channels; they have not been read yet but are of the
expected order of magnitude.
Figure
Data
COe typical signal trace is
reproduced in
.1.
Two channels of the new Z-system were operated on Maui; channel
1 had a 4140 A filter
while channel 2 had a 3914 ý filter.
Because of a
peculiarity in the triggering syt'tem only the 3914 1 channel yielded a good
record, which,
however,
was of excellent quality.
In addition to the operational field systems three separate groups
of four each all sky detectors were operated in the three stations.
The
CCP-type detectors (constant current photodetectors) are more amenable to
yielding quantitative data than the field-operational systems. "All channels
worked.
Data are being analyzed; generally the siguals yere substantially
higher than computed by the High Altitude Fluorezscence code using fluorescence effi iency data derived from pertinent electron gun laboratory
experiments.
Analysis of these data and their bearing on the detection
range of such systems will be most interesting.*
B.
Direct Optical System
Records of early bomb light were obtained on Johnbton Island and
Maui.
The results of the J.
I.
measurement were discussed in
Phenomology,
and a record is
Maui data is
incomllete at this writing.
*
reproduced in Figure 4.
Chapter II,
The analysis of the
7/31/62 - a detection range of approximately R = 2.5 x lsCry km
(y in kilotons) is
indicated.
A-1-31
V.
Spectroscopy
The discussion of spectroscopic data should properly fall into the
related chapters of the phenomenological aspects of the burst. However,
analysis of spectrograms is tedious and only very qualitative information
is available so far. There ýre, I am restricting myself to a description
of the type of coverage acrhieved and to the presentation of a few, though
relatively poor reproductions.
Spectrograms were obtained as follows:
1. Good streak record of burst seen from Johnston Island.
resolution - 5 P sec; cine-quartz-fluoride spectrograph.
Time
The bomb debris
spectrum shows many lines during the first few hundred microseconds and a
strong continuum extending well into the ultra violet.
2,
A very interesting time resolved streak record of the debris
spectrum over the first
several milliseconds was obtained from Maui.
Both continuum and lines are noticeable.
Lines of lithium and aluminum,
also H alpha and H beta have been identified so far.
The saw
recor4
shows also at H + 1.4 milliseconds a very rich line spectrum extending
in
time to H + 20 milliseconds.
This spectrum
originates from the heated
also seen in two other spectrograms (it
booster and is
would be nice to
get numbers for the related temperature and the amount of blow-off -from
this vehicle.)
3.
The spectrum is
reproduced in Figure 12.
Two medium resolution spectrographs (ARL,
1.5 m and a Bausch and
Lomb grating instrument) gave well exposed time integrated spectra of the
burst, showing mainly a continuum with growth of lines at the edges.
These
instruments used small images of the source as entrance slits and growth
of source is reflected in line spectra above and below the continuum.
Figure 13 is
4.
a demonstration of a typic&l spectrum of this sort.
The 3.4 meter Ebert on Maui saw the first
burst; it
10 microseconds of the
shows a continuum whose only unusual feature is
a faint hint of
the 3914 1 N2 + (0,0) band in absorption.
5.
we~a
The Hilgcr medium qaax-tz spectrograph in the aircraft obtained a
exposure of the burst in the time interval 315 to 700 microseconds.
Al-33
6.
A mach stronger bomb debris spectrum was obtained with the Meinel
from Johnston integrating from 500 P sec to 1 msec.
Figure l4.
many broadened lines are present.
7.
A continuum and
Another debris spectrum covering the period 500 to 800 P sec was
obtained with the Eilger Intermediate Quartz from the aircraft.
8.
Au additional field of the Meinel was exposed to the bomb debris
with an integrated exposure from 1 msec to 200 msec.
Figure 14.
namerous lines appear on the record.
9.
A continuum and
The fourth field of the Meinel was exposed from 0.2 sec to 40 sec
looking at the burst.
The main features are strong atomic oxytgen lines.
Debris have mo%•d out of the field of view.
10.
Spectrograms of air fluorescence were obtained with several
instruments.
a)
from J.I. with the Meinel looking 200 off burst.
This is
a
strongE very well developed spectrogram.
b) from the aircraft with the Hilger medium quartz pointing 120
below the burst, exposure interval from 50 p sec to 170 p sec.
c) from J.I. the Infrared spectrograph integrated from 10 sec to
110 sec covering wavelengths froi? 4500 t6 9000 •.
emission is
Oxygen
dominant.
d) The below burst "pancake"
Medium Quartz (Figure 5)
spectrum Dbtained with the Hilger
and the suroral spectrograms
obtained from the Iwo Jima (Figure 7) were described in
Chapter II.
11.
Late light was observed in
the burst region from Maui with the
Steinheil and auroral spectrographs until three minutes after burst.
Mainly air compments and H alpha appeared.
12.
A line width experiment operated satisfactorily at Maui.
Quality
of data not yet established.
13.
Fnotoelectric records of the brightness of the 6300 R and 5577R
oxygen lines were taken at angles of 20, 100 and 20 0 from burst over a
period of 16 minutes.
Al-36
Pe,ý- 41-37 T
k)
II
Postscripts 7-31-62
Ii.
Phenomenoloy
A.
Early Debris Expansion
An EG+G Photosonic Camera. record from Maui 360 cm focal length,
3203 frames per sec,
shows the expansion of the bomb debris from approx-
imately 1/3 msec to almost 10 msec.
The partition of the bomb debris
into two parts described on page 7 is
shown; in
particular the develop-
ment of the "core" into an upwards muhroom3like expansion configuration
is
seen clearly.
disc.
The fast moving fraction takes the shape of a thick
Also the interaction of the bomb debris vith the booster-at an
apparent distance (projected)
15 Is
.f
approximately 1.5 km is
shown.
Figure
a reproduction of frames 2 through 7.
B.
Late Debris Expansion
Two Mitchell camera pictures taken from Maui show the debris
expansion in the neox horizoatal,
in the upwards (hunp)
northern downwards direction ! .e.
alo';
they make contact with the
=', .el.71
beta ray "pancake"
disc seems ÷
,
the
the magnetic field lines until
just above 'Lhe horizon.
.-
n
The early expransion of the
be governed by the attitude of the E/V .t
Al- 38
and in
btrst time.
Is
a
Mitchell camera record st +0.05 sec, enlarged.&
I:
I
I
I
I
I
a
•
AI-..O
I
I
II I
I
I
fI I I
II
i
l .. Tije!
• I
SECRET
Figure 17
Mitchell camera record at +0.12 sec1 enlarged.
Al-
2
•..•nB
I II
I
SECRET
I
Table of Contents
A.
Ifm~edlate Attenuation
B.
Delayed Attenuation
C.
Synchrotron Radiation
D.
1.
Early Phase
2.
Round-the-world phase
5.
Long-term decay
SuI.ary
A2-2
A.
Immediate Attenuation
Following the burst immediate attenuation of cosmic noise was noted
at riometer locations within line-of-sight of the detonation poInt.
rapid onset and decay,
frequency dependence,
The
and decrease with radial
distance from the detonation point of the attenuation appear to agree
with predictions of absorption caused by prompt radiation (X-rays,
prompt gamma rays,
neutrons).
Because of the slow chart speed the
immediate attenuation appears as a sharp pulse on the EA records.
A
detailed examination of the onset and decay can be obtained from Rustrack
records limited by the riometer time constant of about 1 second.
Table
A lists riometer locations where immediate attenuation due to prompt
radiation was recorded.
TABLE A
Riometer Locations Recording Immediate Attenuation
Oahu
French Frigate Shoals
AA RICPN MARINER (W44p)
S 1, S 2,
S 3,
S 4, S 5
Wake
Midway
Johnston Island
Palnyra
Canton Island
Christmas Island
In addition to the riometer locations listed in Table A,
immediate
attenuation (within a few seconds) was noted at Fiji, Rarotonga,
Tongatapu,
Tutuila, Viti Levu, and the ACA1IA.
Reports of prompt
absorption were also received from Adak and Boston (but not from Menlo
Park).
Since these stations are beyond line-of-sight from the burst,
the attenuation is
not due to X-rays or prompt gemma rays.
In the
conjugate region beta rays following the earth's magnetic field lines
from the burst locale or beta and gamma rays emitted from debris wbicb
A2-3
has been directed along the magnetic field lines to the conjugate
region may account for attenuation within a few seconds after burst.
possible source of attenuation at Adak is
A
upward directed neutrons vhicb,
after spontsaneous disintejation, produce beta rays which can be guided
by the earth's magnetic field to locations beyond line-of-sight froi the
burst.
B.
Delayed Attenuation
D-region absorption caused by beta and delayed gamma rays emitted
from the fission debris is
noise.
a source of persistent attenuation of cosmic
Because beta rays are confined by the earth's magnetic field,
the D-region absorption is
a function of the spatial
d..tribution of
the debris and the inclination of the magnetic field.
rays radiate in all
Delayed ganua
directions from the debris causing D-region absorp-
tion over a region similar to that experiencing immediate attenuation.
While the presence of synchrotron noise mtakes estimates of attenuation
due to gsnma ray absorption difficult,
the riometer locations listed in
Table B appear to have experienced ganmma ray absorption without cdtcurrent beta ray
absorption (at early times after burst).
-
TABLE B
Riometer Locations Recording Delayed Ga=.,a Ray Absorption
Ohu
Midway
S1
Johnston Island
S 3
Palmyra
S 4
Canton
As previously mentioned beta rays are confined by the earth's magnetic field producing D-region absorption down the field lines from the
burst point and at the southern magnetic conjugate area in a region
determined by the spatial distribution of the debris.
hemisphere,
Mn the northern
strong absorption was recorded at riometer locations (espe-
cially at S 5) where the magnetic field lines passing through the
detonation point intersect the D-region.
A2-h
Table C lists the riometex
locations which best describe beta ray
absorption immediately following the burst.
TAkBi
C
French Frigate Shoals
ACAI\'IA
A=ICA;C MAPINEh
Viti Levu
(DAMY)
S 2
Fiji
S 5
Tongatapu
Table D shovs the 30-MO attenuation observed at the riometer stations
for ieveral intervals of time.
The data in
Table D are only rrelimtnary
based on assumptions which attempt to compensate for synchrotron r&adiation.
p
A2-5
30 14C Attenuation (db)
T-ne A-er S'hot - In
Vinutes
Y~ir.
_________
6-
Ar
1,1mI
Fr. Frigate Shl.
American Variner
S4
s5
Midway
Johnston Island
Palm~yra
Canton
ChristLa•
is.
Acania
Viti Levu (Fiji)
Rarotonga
Tutuila (Samoa)
Tongatapu
Note:
S - off scale reading due to synchrotron radiation.
Following the first
the detonation,
there is
recovery of absorption in the region north of
a second phase of absorption which can be
associated with debris motion.
Table E lists the approximate onset
time of this second phase cf absorption and the time when it
maximn.2.
!M
reached
TA.IE E
Onset and Maximum Times of Second Phase of Beta Ray Absorption
Time of Maxidmum
Minutes
Time of Onset
Minutes
Station
S 4
Johnston
$2
el ted
AYPERICAN K
S5
s3
Note that the second absorption phase appears to be spreadlng from
the detonation region.
A possible explanation is
that part of the
debris originally trapped at about the burst point (causing the hot
spot around S 5) falls to lower altitudes where it
then spreads hori-
zontally.
There are several interesting characteristics of the riometer data
which will require more detailed examination and correlation with oler
projects before deciding upon the best explanation.
the apparent anamoly in
MRCl=
One of-those is
the attenuation recorded by the AMERICA4I
and the ACANIA.
These two ships were located at opposte ends of the same magnetic
field line (conjugate to each other) so the beta ray absorption would be
expected to be the same at each location.
difference in
It
does not appear that the
absorption (particularly the time variation) can be ex-
plained by the effect of delayed gamma radiation.
Other variations ip the cosmic noise records of interest are:
(1)
the brief recovery of attenuation noted at Tongatapu and Viti Levu about
10 seconds after burst;
(2)
the apparent build up of delayed attenuation
at Midway following the t.mmedlate attenuation;
(3)
the rather complicated
nature of the Viti Lev-u records which show three distinct phases of
attenuation in
the first
few minuter after burst; and (4)
attenuation noted at Rarotonga.
several locations; however,
the immediate
Small sunrise effects can be noted at
the effect of
synchrotron noise makes esti-i
mates of long term debris motion difficult.
C.
Synchrotron Radiation
When high speed electrons on the order of I Mev energy or higher are
influenced by the earth's magnetic field, their rotary motion causes
wide-band radio noise to be emitted in the VhF spectrum.
Successful
launch of these electrons into the earth's magnetic field requires higý
burst altitude in order to avoid containment by neutral air of beta
producing fission debris.
Mirroring must occur at altitudes in
of about 400 km at the longitude of Johnston Island in
excess
order that
electrons will have some possibility of surviving a single trip around
the world (30 minutes for 1 Mev approximately).
high altitude fission debris is
Continual feeding by
likely to offset the loss of trapped
betas and zould,
in
ation with time.
The end-points of the field dip deepest into the
theory, result in an increase of synchrotron radi-
earth's neutral atmosphere and so the synchrotron radiation would be
expected to persist longest at the magnetic equator (Christmas and
Huancayo,
Peru).
Estimates of the frequency spectrum have been at-
tempted (see Schwartz,
spectrum,
ener•f,
R. N.) on the basis of estimates of fission beta
likely trapping altitudes, radiation per electron. of given
and directional characteristics of -.he radiation with respect to
the earth's magnetic field.
It
is
concluded that synchrotron radiation
at 30 Mc would be expected to be a factor of 10 greater than cosmic
noise maximum.
As a result of Starfish Prime,
were observed.
after burst.
The first
two phases of synchrotron radiation
was most intense and lasted cnly a few minutes
The second phase starting after plus 10 minutes can be
isolated from the first
because,
at Wake,
the betas which circum-
navigated the globe appeared at plus 10 minutes where no synchrotron
radiation had been observed earlier.
This second phase was not changing
perceptably with time (for equatorial stations) in
days of observation.
A2-8
the course of several
1.
Early Phase
Following the initial strong absorption due to the burst, synchrotron
radiation (discerned by the record exceeding the normal cosmic-noise
level) vas observed at Oah.u, Johnston,
S !, S A, Palr-y.a, Christras,
Other
-tutla.ships and French Frigate Shoals might have
Canton and
observed early-phase synchrotron radiation if the attenuation had not
been so extreme.
The effect was greatest at the stations long and to
the east of the magnetic meridian of the shot and was apparently greatest
for the stations closest to the-equator.
In general, the synchrotron radiation reached a maximum at about plus
30 seconds, and died in the course of several minutes.
Presumably the
synchrotron radiations were maxidmum immediately after burst time but was
attenuated in the D-region before reaching the riometer.
At Canton Island, special equipment was provided to measure the
nature of thea polarization of the sy.chrotron radiation.
On 13 Mc, four
total power receivers were operated in conjunction with four zenithal
antennae, each having a different polarization, so as to uniquely cftermine
the polarization ellipse as well as the random polarization--component.
Deleted
On
120 Mc,
a riometer was connected to a zenithal,
linearly-polarized Yagi ante-na turning about a vertical axis, at a rate
of about
3.3 rotations per minute.
This equipment should have been able
to determine the ratio of axis of the polarization ellipse, but the
polarization also appeared to be random.
On 60 Mc,
a 10-wavelength
interferometer with slowly sweeping lobes was arranged on an east-west
line to reasure the width of the radiating "Lube" of trapped betas overhead.
The antenna spacing was chosen too large so that all that was
shown was that the radiating source was larger than about 5 degrees in
width.
A2-9
At Johnston Island, two auxiliary 120 Mc riometers were operated
with high-speed Rustrak recorders,
one riometer attached to a Yagi in
tne meridian plane and the other Yagi scanning the horizon.
The
meridiean plane equi-ent showed early synchrotron radiation arriving
fron approxamately overhead
(uithin about hO degrees).
The rotating
equipment showed early synchrotron radiation arriving from the southeast.
As the electrons spiral about the magnetic field lines and oscillate
along the field lines from one hemisphere to the other, there are
several forces which cause negatively-charged particles to migrate eastward and positively-charged particles to migrate westward.
Only the
electrons are expected to give synchrotron radiation of irportance in
the VhT spectrum.
Hence,
stations located along the magnetic meridian
of the shot and to the eastward should observe the strongest radiation
du-rng the first few mpinutes.
(There is
a high. population of I and. 2
Mev betas which require roughly 30 minutes and 15 minutes,
to travel around the world.)
respectively,
G"
The riometer network did not observe synchrotron radiation at any
of the stations west of the magnetic meridia' (Wake, Midway and Fiji).
Midway and Oahu are located roughly magnetic east-west of each other at
about the same magnetic latitude.
Oahu cbserved off-scale synchrotron
radiation but Midway observed none.
Stations far to the north and far to the south did not observe
synchrotron radiation (Tongatapu) because the radiation is emitted
primarily at right angles to the magnetic field.
French Frigate Shoals and the northern ships did not observe
-
I
synchrotron radiation because of heavy absorption at the time (due to
fission-debris, or beta bombardment overhead of. those sites).
A2-10
I.°
2.
Round-the-world Phase
Once betas are trapped in the earth's field, they will migrate eastward and reappear at the riometer network from the west.
cially clear at the Wake station,
This vas espe-
well to the west of significant delayed
absorption and well to the west of early synchrotron radiation.
Wake
The
30 Mc riometer began to show noise above the normal cosmic noise
level at about plus 10 minutes,
which maximized at about 25 minut.'r,
holding approximately this level theaeafter.
The round-the-world phase appeared at the rest of the riometer
stations even before the other effects of the shot had disappeared,
making inter,.'-etation difficult.
The South African magnetic anamoly is
expected to cause a considerable loss of the trapped electrons, especially at latitudes well reaoved from the equator.
Consequently,
each
transversal around the globe emphasizes the equatorial stations such as
Christmas,
3.
Ceanton and Palmyra.
Long-Term Decay
It is
abundantly clear that there is
at these and other stations.
long-term synchrotron radfation
Canton, for example,
showed n- significanL
decrease of the synchrotron radiation in the course nf five post-shot
days of observation
(53 Mc,.
At Christmas on the magnetic equator the -
synchrotron radiation (at 30 Mc) appeared to have decreased 20 percent
in
going from plus 10 hours to plus 100 hours.
D.
Sumr~ary
From the preliminary analysis attempted here, it
would appear that
at least part of the fission debris was contained within a few hundred
kilometers of the detonation point.
In the northern hemisphere, the
prompt radiation absorption agreed in magnitude and extent with expectations.
The presence of debris spreading to altitudes on the order of
1000 kn or higher is difficult to determine because there were no riometer sites north of French Frigate Shoals and south of Tongatapu where
beta rays would be directed by the earth's magnetic field.
However,
the
appreciable absorption at French Frigate Shoals, Viti Levu and Tongatapu
A2-ll
(particularly the absorption seen with oblique riometers looking south
from Tongatapu) and the moderate absorption observed by the northern
hemisphere ships, suggest that a sizeable fraction of the debris was
spread over a considerable altitude distribution.
This is
confirmed by
the significant efficiency of the synchrotron radiation during the first
five minutes.
Before the shot there was a suspicion that the snow-plowing of the
debris at several hundred kilometers height could give rise to an "ioncurtain" of very heavy attenuation. However, the fact th'At the Johnston
Island rioneter had recovered Jn agreement with the X-ray deposition
indicates that the ion-curtain effect did not sipificantly occur.
For Starfish, detailed predictions of synchrotron radiation were not
made. The long lifetimes clearly imply that injection of betas occurred
well above detonation altitude.
A Parch was made for absorption associated with the appearance o."
sunlight. Weak effects were found at many stations implying that the
debris was spread over great distances very thinly.
There was evidence
for the debris region slowly falling and spreading in radius dxfring the
night (migrating slowly from Johnston to S 5); the magnitudes 4-ply that
at least some of the debris went into this system.
difficult to determine.
A2-12
The fraction is
Appendix 3
Miscellaneous Reference Data
1. R/V and Pod Positions, and Time of Burst
Detoation occurred at 0909009029Z, 820.7 second.s after lift
corresponding to 9.02
off,
seconds after 2300 hours, 8 July 1962, Honolulu
time.
The follor-ing are the preliminary positions of the poda and the
re-entry vehidle relative to the Thor launch pad on Johnston Island.
Note that both Cubic Corporation and Sandia Corporation tracked Pod S-3,
and that there is a slant range discrepancy between the two measurements
on Pod S-3 of 1.5 km.
Preliminary Measured Positions
Pod S-1
30,950 ft W
102,000 ft S
1,285,300 ft Mat
(Cubic)
Pod S-2
30,200 ft W
101,500 ft S
1,274,000 ft high
(Cubic)
Pod s-3
Pod S-3
29,6oo ft W
31,900 ft w
100,350 ft S
96,900 ft S
1,236,200 ft high (Cubic)
1,235,400 ft high
(Sandla)
R/v
34,95o ft w
100,800 ft S
1,312,450 ft high
A3-1
(Sandia)
2.
SMALL ROCKET DATA
2 . Rockets Launched from Johnston Island (Total number, 27)
Time of
Launch
Pad Project Rocket
No.
IT)
Type
Azimuth
true
(degrees)
Elevation Apogee
Last Stage
(nautical Impact
(degrees)
miles)
Point
Type of Measurernmer.t
H-2 3/4 hrs. 21
9.1
Nike Cajun
155
85
74
33 n miles Winds with Na Vapor
H-30 min.
20
9.1
Nike Cajun
155
85
74
33 n miles Winds with Na Vapor
H-600 sec
19
6.4
Javelin
90
83
270
E-510 see
25
6.7
XM 33
198
78
555
H-500 sec
1
6.7
XM3
10
85
715
1-280 sec
2
6.7
X)3
10
85
715
h--206 sec
14
STI 152 Nike Apache
195
88
93
16.480N,
X 8 Y-rays.Ioniza162 .&854
tion
.36s,
Mag.field and Debris
172.60W
Expansion
24.40N,
Hag. field and Debris
169.6"W
Expansion
24.4'N,
Mag. field and Debris
169.6"w
rcpans ion
18 n miles X-ray
, -201 sec
10
SJ'I 152 Nike Apache
195
88
86
17 N miles X-ray, 8-ray
E-200 see
7
STI 11l Nike Apache
195
88
86
H-199 sec
9
SJI 151 Nlike Apache
195
88
66
H-190 sec
H-160 sec
8
24
SJI 112 Nike Apache
6.7
M2433
195
198
88
85
86
17 n miles X-ray, Rad. Chem.
Sampler
17 n miles X-ray, Rad. Chem.
tampler
17 n miles X-ra,, Rad. Chem.
S,=pler and Debris
5p80N
Hag-field
rL'J>
1.
78
5:5
SJS 151 Nlike Apache
195
86.5
95
172.2 "W
Ercpansiorn
.5"S,
Mag.field and Debris
172.60w
Expanolor,
33 n miles Rad Chem Samyler
120
85
48
25 n miles X, 8,
n-1 4v b c
6.'(
c.
H-132.5 sec
13
H-90 sec
6
6.3
Honest John
Nlike
H-60 sec
16
6.3
Nike Cajun
90
85
64
29 n miles Mass Spectrometry
H+220 sec
3
6.13
Speedbsll
10
84
124
75 n miles Radar Jitter
H+420 see
18
6.3
Honest J.hn
90
85
48
25 n miles X, 8,
Nike
S
U
7-rays,
Ionization
7-rays,
Ionization
H+420 sec
22
6.4
Javelin
120
80
237
H+450 see
15
6.3
Nike Cajun
90
85
64
ll.47N,
X, 8. V-rays,
161.360w
Ionization
29 n miles Mass Spectrometry
H+710 see
26
6.13
Speedba._l
190
82
124
98 n miles Radar Jitter
H+960 sec
17
6.4
Javelin
90
Eý
270
H+1200 sec
5
6.2
Javelin
15
80
315
16.48*N,
162.3W5
27.39,
H+1860 sec
27
6.13
Speedball
180
82
121
167.9"W
98 n miles Radar Jitter
H+2400 see
4
6.2
Javelin
15
80
345
H+3540 sec
11
195
86.5
95.4
SJS 152 Nlike Apache
X, 5, 7-rays.
Ionization
ti
tonz
7. I8,
27.09*N,
7, 8, Photometry
167.9*W
33 n miles Rad. Chem. Sampler
0549,D+1
21
9.1
Nlike Cajun
155
85
74
33 r n' 1es Winds with Na Vapor
All1 data are based on pre-shot planning and therefore approximate.
A3-2
b.
Rockets
Vo,.e:
Tine o:
Launc-h
Csecci.-.)
waunched from Barking SL-nds.
Yauali (Tota!l Number 21)
III1 rockets az-c Nike-Apaches.
Iden'.1ficatior.
Fzporsoring
Organization
______
AIi-A
~
(degrees)
______
Lev a' Icl,
(degrees)
_____
Ap'ogee
( Nautical
Era
S7ecoiij S-tb~e
impact distance
(
c
imies)
90
9i
85
80
i'v-e C:
Measiaremer..
______
H£c
E'Z- 15 1
S and Ia
3 4z
Ji-205
Sý:: -111
U1
345
80
H -2041
SIC -l.2
L.' 1
34'5
8080
H-2C5
sY"-l'15
LR.
3451
8-2
84.5
64
Alpha
F -2C'5
S~i- 113l
LAST-
A45
82
85
65
1,e-tIr ro.
Ii-.5
Si=- iy'
Lk~:&
H-205
SK2-151
Sam l-a
345
80
8
85
Time Interval
H-235
SIC -154
Sarndi a
345
8-1
86
69
!;eutron, 1,-ray
H-195
S~i -l13
I:-"
C,52
848649
1P-295
SIC.-1114
LIRL
352
82.
H-195,
Sla -133
LASL
347
H-195
sYI -13E
IAS-L
347
&1
64
63ý
7-ray
lH-1ý8
SFI-116
LPL
345
82
85
£-4
Alpha
SKI-134. lIASL
347
82
84
63j
X-ray
Ii leg
SY.-1 5 2
Sanjdia
345
80
8586To
Ii -164
S ýa-1,5 5
Sandia
345
8-
78
4.6
I~e-.t*ror..
H-154
Sla -157
Skj'dia
~'A56
84
77
46
X-raky
slia-15 `
Sarnij'a
345
BC
75
74
-a
Sla13-i
LAS'_
345
62
85
64
Neutron
SICI-13 5
LASL
345
6-1
86
64
7-ray
S la -13-1
LA_-L
35
62
8664
11-89
F,1.5
11-49
R-49
11-49
Neu;tror.
X, vy-ray.
86
49
844
A3ý- 3
Neutrorn
Y., Y-ray
X-ray
ntra
7-rNy
7-rkay
c.
Rockets launched from Point Arguello, California (total Number,
Both the F-480 second Argo D-18 and the Ii-1+O0 second Astrobee 1500
failed.
Each payload included neutron and X- and 7-ray experiments; no
data was obtained as both pyloado inpacted before detonation.
3. Ship, aircraft ard island locations
Ship Locations
a.
Longitude
Name
Latitude
8-i Oak Hill
100 27'
S-2 Irt. Marion
18" 57.5' N
S-3 Polk County
17" 57'
N
164" 24' W
S-4 Pt. Barrov
W6" 53'
N
172* 12' W
S-5 Taylor
21" 33.0' N
(DAVY)
19e 52.5'
American Mariner
171' 28.5' W
N
1690
6.5' w
168" 50' wI
168
N
58.5' W
Within 2 miles of Niua Fo'ou
Acania
AMproximately 175" W, 150 S
b.
Aircraft Locations
Project
a/C Call
Tye
Latitude
8
A.1, A.2
Kettle 1
KC 135
22'
8
A.1, A.2
Kettle 2
KC 135
15" 53'
N
1660 23' W
6.10
Kettle 3
KC 135
1i* 22'
3
177" 47' W
4.1
Caboodle 1l
C I18
19
4.1
Caboodle 12
C 118
200 03'
4.1
Caboodle 13
C .18
200 08' N
A3-4
Longitude
4.3' N
11' N
N
1680 24.5'
1670 27'
W
165'
W
56'
1630 04' W
W
2)
Project
A/C CaLl
D
Latitude
Longitude
4.1
Cabood]e 14
C i18
21" 00' T,
159
4.1
Caboodle 15
C i18
210 21' N
i157" 55' W
7.4
Baxter
B-47
19" 55' N
161
7.4
Cognac
MC 135
170 57' N
166" 13' w
7.4
Cordova
KC 135
150 07' N
172" 20' W
6.9
Lambkin 1
RC 121
140 00' N
1650 28' W
6.9
Iambkin 2
RC 121
10* 57' N
165
6.9
Iazbkin 3
RC 121
3.2 *43
170e 10.5'
6.9
Lambkin J+
RC 121
08055'S
169* O1' w
IJkSL
Rewstone
C-130
ll& 16' N
115" 07' W
LASL
Kiboah 2
KC-1I5
24* o8'
1650
c.
S
i
Island Locations
See Map (Page x of Reference e.) next page.
A3-5
00' W
05' w
47' W
'
W
w
I
0
I.
::- *,
."::byI
'
;:
.-__
_
________
-
•
.!
•1i•
At-
44
*e.
I
I
I
I
I
I
I
I
I
I
4.
REFERENCES
The major references used in
however,
this compilation are listed blow;
very much of the data was obtained from conversations, notes
and specialized TWX' s which are not listed here.
a.
TWX OIC TE 8.1.3.2 Hickam AFB, Hawaii,
1962, TU3a621062-D,
to Chief DAA, July 10,
I (H Plus 24 Hour Report).
b.
TWX OIC TE 8.1.3.2 Hickam AFB, Hawaii, to Chief IASA, July 12,
1962, T3H62-093-D,
(H Plus 72 Hour Report).
c. TWX CTU 8.1.3, Johnston Island to Chief DASAA, July 12, 1962,
TU3H62109-D,
(H Plus 72 Hour Report).
d. TWX CM 8.1.3, Johnston Island to Chief DZSA, July 10, 1962,
T!J3J62182Z4-D,,
(D Plus 1 Da.y Report).
e. DSAM Special Report 1 (Revised), Operation Fish Bowl, Projected
Measurements Summary, May 23, 1962, J2-65,
A3-7
5.
ORGANIZATIONAL ABBREVIATIONS
AFCRL
Air Force Cambridge Research Laboratories
AFSw;C
Air Force Special Weapons Center
AMD
Aerospace Medical Division
AOMC
U. S. Army Ordnance Missile CcEand
APL
Johns Hopkins University, Applied Physics Laboratory
ARF
Armour Research Fbundation
ARPA
Advanced Research Projects Agency
ASD
Air Force, Aeronautical Systems Division
BRL •U.
S. Arzy Ballistics Research Laboratory
CN0
Chief Naval Operations
CRPL
Central Radio Propagation Laboratory, National Bureau of
Standards
DASA
Defense Atomic Support Agency
EGG
Edgerton, Germeshausen and Orier, Inc.
GCA
Geophysics Corporation of America
LASL
Los Alamos Scientific LAboratory
lRL
lawre.-ice Radiation Laboratory
NIT
Massachusetts Lnsitute of Technology
1NDL
ArmW Chemical Center, Nuclear Defense Laboratory
MM
Navy Electronics Laboratory
RADC
Rome Air Developmen4
9RDL
U.S. Army Si.t.al Research and Development Laboratory
SRI
Stanford Research Institute
USASRDL
U. S. Arny Signal Research and Development Laboratory
USASRPA
U. S. !rW
,enter, Griffiss AFB
Signal Radio Propagation Agency
A3-8
6.
Prime
Weather Sumary for St.rsh
Johnston Area. 0900 Z (Shot Time).
1/8 thin cirrus.
2/8 alto-cumulus over Johnston,
Poorer conditions over ships to the north, vith some
showers to the north.
.aui Area: 09D0 Z. 2/8 cumulus, bases 3,000 ft., 6/8 strato-cuwalus, bases 4,,500 ft., 2/8 cirrus, visibility 15 miles plus. From the
station on Mt. Haleakala the direct line of sigbt was clear through a
ligt
hole in the clouds.
South Conjugate Area:
I.
miies plus.
Samoa 0600 Z.
1200 Z.
4/8 cumulus, bases 2,000 ft., visibility 10
1/3 cniulus, no other change.
Nandi 0600 Z. 1/6 cumilus, bases 3,000 ft., overcast with
clto-cumulus and cirrus, visibility 10 miles plus.
1200 Z. 1/8 cumal2us and strato-cumulus, bases 3,000
2.
ft., scattered alto-cumulus, visibility 10 miles plus.
A3-9
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