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 NOAA Technical Report OOE 1 
 
 
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 A Submersible 
 Physics Laboratory 
 Experiment 
 
 Washington, DC 
 January 1979 
 
 U.S. DEPARTMENT OF COMMERCE 
 
 National Oceanic and Atmospheric Administration 
 
 Office of Ocean Engineering 
 
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 """^"ofco* 
 
 NOAA Technical Report OOE 1 
 
 A Submersible 
 Physics Laboratory 
 Experiment 
 
 Kurt R. Stehling 
 
 Manned Undersea Science and Technology Office 
 Washington, DC 
 January 1979 
 
 U.S. DEPARTMENT OF COMMERCE 
 
 Juanita M. Kreps, Secretary 
 
 I *■• 
 
 National Oceanic and Atmospheric Administration 
 
 £» Richard A. Frank, Administrator 
 
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 Office of Ocean Engineering 
 
 Steven N. Anastasion, Director 
 
Mention of a commercial company or product does not constitute an endorsement 
 by the NOAA Office of Ocean Engineering. Use for publicity or advertising purposes 
 of information from this publication concerning proprietary products or the tests of 
 such products is not authorized. 
 
 For sale by the Superintendent of Documents, U.S. Government Printing Office 
 
 Washington, D.C. 20402 
 
 Stock Number 003-017-00435-0 
 
 11 
 
CONTENTS 
 
 Page 
 
 Summary 1 
 
 Introduction and background 2 
 
 Basic physics 2 
 
 Applied physics 6 
 
 Engineering 8 
 
 Operations 8 
 
 Conclusions 11 
 
 FIGURES 
 
 1. Examples of Benthos glass spheres 2 
 
 2. Variation of muon energy with water depth 4 
 
 3. Samples of elementary particle events 5 
 
 4. Rate of muon stopping by water depth 6 
 
 5. Rate of positive ion stopping by water depth 6 
 
 6. Nuclear emulsion drying oven 7 
 
 7. Track of collision between a muon and a proton 8 
 
 8. Liquid emulsion on chilled plate 9 
 
 9. Processing tanks used for nuclear emulsions 9 
 
 10. The JOHNSON-SEA-LINK 10 
 
 a) cut-away profile 10 
 
 b) on RV JOHNSON 10 
 
 c) bottom hatch detail 10 
 
 d) specifications 11 
 
 11. Detail drawings, Harbor Branch lockout chamber 12 
 
 12. Gear for transferring lockout chamber between ship and ocean 12 
 
 13. Schematic of sub and platform chamber 13 
 
 in 
 
Digitized by the Internet Archive 
 
 in 2013 
 
 http://archive.org/details/submersiblephysiOOsteh 
 
A Submersible Physics Laboratory Experiment 
 
 Kurt R. Stehling, Senior Scientist 
 
 Office of Ocean Engineering/ Manned Undersea Science & Technology Office 
 National Oceanic & Atmospheric Administration 
 
 SUMMARY 
 
 In autumn 1976, I proposed to Edwin Link, Vice President, Harbor Branch 
 Foundation, Inc., Ft. Pierce, Fla., that Harbor Branch/Johnson-Sealink (JSL) sub- 
 mersible be used to prepare on the ocean bottom, and then lock out, sensitive photo- 
 graphic emulsion stacks for the detection of cosmic-ray muons.* The ocean would 
 serve as an homogeneous and isotropic filter, absorbing most cosmic-ray and other 
 nuclear particles, except, for purpose of this experiment, the muons (or mu-mesons). 
 
 After a meeting at Harbor Branch in early 1977, President S. Johnson and E. 
 Link agreed that the University of Washington/Western Washington University ( U. of 
 W./WW.U.) experimenters (J. Lord and P. Kotzer) with NOAA/OOE/MUS&T (K. 
 Stehling as scientist-monitor-observer) would be granted JSL time. Furthermore, 
 Harbor Branch then proposed, designed, and built a unique ocean bottom-sitting 
 receptacle or chamber (a modified JSL aft "sphere," unused), which they deployed in 
 September 1977 off West End, Grand Bahama Island (lat. 26°41'4"N, long, 
 70°00'8"W). 
 
 During the week of Oct. 3, 1977, two emulsion stacks in glass cassettes** were 
 prepared in the JSL and deployed, one at 1,000 ft (328 m) within the bottom cham- 
 ber and one for reference at 400 ft ( 122 m) . 
 
 In March 1978, the 400-ft cassette was retrieved and locked into the JSL, and the 
 emulsions were developed in situ. The 1,000-ft emulsions were retrieved in October 
 1978. New experiments are being planned. 
 
 The following features highlight this unique experiment, which blends ocean 
 engineering with high-energy physics : 
 
 1. A submersible was used as a minilab for preparing cosmic-ray detectors. 
 
 2. Lockout into a bottom chamber was achieved, at 1-atm. pressure. 
 
 3. The JSL crew remained, in one mission, for 12 hr at 1,080 ft with no adverse 
 consequences. 
 
 4. A partnership between the NOAA and Harbor Branch, a not-for-profit founda- 
 tion, was achieved, with the Harbor Branch contributing most of the technical 
 and logistic support and equipment to the missions. 
 
 5. The University of Washington/Western Washington University scientists have 
 already found evidence of new muon interactions. 
 
 * Mention of a particular item does not constitute endorsement by NOAA. 
 
 **9-in diameter glass spheres, manufactured by Benthos Corp., Falmouth, Mass. (fig. 1). 
 
INTRODUCTION AND BACKGROUND 
 
 Since 1972, NOAA (OOE & MUS&T) and the Uni- 
 versity of Washington Physics Department, have been 
 associated in the underwater detection and analysis of 
 cosmic radiation flux. The reasons for operating under- 
 water are: 
 
 a. The water is an isotropic and homogeneous 
 medium that "filters" or absorbs many "stray," or 
 unwanted hadrons* and leptons** which are filtered 
 also by rock and soil as in a mine, but the filtering 
 function of a heterogeneous overburden is ambiguous; 
 
 b. The natural radioactivity of seawater is much 
 less than that present in deep mine shafts where vari- 
 ous cosmic-ray detection experiments have been tried; 
 
 c. Water, from the nuclear interaction standpoint, 
 is a hydrogen or proton "soup" wherein collision 
 products are much easier to predict, discern, and 
 analyze. The dissolved metallic and other ions do not 
 materially affect this property of water; 
 
 d. The water itself can act as a detector (in a 
 deep mine, tanks of water or other liquids are also 
 used) with the high-energy cosmic-ray neutrinos pro- 
 ducing muons by inelastic nuclear collisions, which in 
 turn generate microscopic "Cerenkov" light flashes in 
 the water, detectable with photomultipliers. Tracks 
 made by the muons can be discerned in media such as 
 a photographic emulsion as described herein. 
 
 The deeper the cosmic-ray detection device is placed 
 in the ocean the greater is the filtering factor, with 
 the stray particle density reduced almost linearly with 
 depth increase. A 50-ft depth experiment shows an 
 almost 10 percent decrease in unwanted particle back- 
 ground. At 400 ft one can expect trivial noise back- 
 ground, leaving mostly neutrino-generated muons to 
 be detected by the photoemulsions. 
 
 The purpose, then, of past (1972-76) underwater 
 (HYDROLAB-based) experiments, and those described 
 in this paper has been to take advantage of the nuclear 
 cosmic-ray related qualities of the ocean water mass by 
 allowing the experimenter (s) to work in situ on the 
 sea floor, rather than attempting to try an impractical 
 alternative: lowering a prepared photoemulsion de- 
 tector to the bottom from a surface vessel, a method 
 that would yield an unacceptably surface-radiation- 
 cluttered emulsion. 
 
 This report describes briefly the four elements that 
 motivated or comprised the subject experiment: 
 Basic Physics which motivated the mission 
 Applied Physics, including particle detection, emul- 
 sion chemistry, calibration, and scanning 
 
 Figure 1. — Examples of Benthos glass spheres — pro- 
 tective "hard hats" in rear. 
 
 Engineering, including design and fabrication of 
 supporting apparatus, use of a submersiblef 
 and a bottom lockout chamber. 
 Operations, including submersible dives, ship sup- 
 port, emulsion preparation, deployment, recovery, 
 and development. 
 
 BASIC PHYSICS 
 
 It is believed that the phenomena of the universe are 
 best understood in terms of the set of elementary 
 particles that have been discovered and the four basic 
 forces (gravitation, strong, electromagnetic, weak) 
 which govern their dynamics. Each time a phenomenon 
 involving higher energy particles has been investigated, 
 new insights (and often new particles and laws) into 
 the structure of our world have been discovered. 
 Recently, the study of neutrino reactions at accelera- 
 tors has produced evidence that may lead to a syn- 
 thesis of two of the great laws of physics — quantum 
 electrodynamics and weak interactions; in addition, 
 the existence of charmed quarks as well as the standard 
 three quarks has been implicated. 
 
 A particularly rich field of investigation has been 
 that of cosmic radiation. The highest energy cosmic- 
 rays sofar detected have an energy of 4 X 10 21 eVft 
 (electron volts) or 40 billion times greater than the 
 highest energy particle produced at the Fermi National 
 Accelerator. 
 
 Two features of cosmic radiation make it a particu- 
 larly important field. First, it provides a guidepost to 
 the nature of physical laws at energies far greater than 
 
 * Nucleons: e.g., protons, neutrons. 
 
 * * Extranuclear particles : e.g., electrons. 
 
 t The submersible (JSL) was modified slightly to permit 
 lock-on to the bottom chamber. 
 
 tt The energy accrued by an electron while traversing a 
 1-Volt field/cm. A flea jumping to 10 cm generates about 
 0.6 X 10" eV. 
 
machines can produce. Second, study of the composi- 
 tion and energy spectra of primary cosmic rays can 
 be used to learn about astrophysical processes in the 
 formation of stars and star systems. The roles played 
 by the elementary particles, particularly the neutrino, 
 are thought to be crucial in the evolutionary develop- 
 ments of the universe. 
 
 The nature of the ultra high-energy (over 10 15 eV) 
 primary cosmic rays is being studied in the "Fly's 
 Eye" experiment of the University of Utah. This ex- 
 periment is capable of determining if the higher energy 
 cosmic rays are neutrinos. Another experiment has 
 indicated that the primary cosmic radiation may be an 
 admixture of magnetic monopoles and protons. (There 
 are no other experiments supporting this result as yet.) 
 
 A major effort by a group of scientists is being 
 expended on the proposal for a deep undersea neutrino 
 observatory, which is now in its early, conceptual 
 stages. Knowledge of the lower-energy cosmic-ray 
 muon background is of central importance to this 
 experiment. One purpose of the described experiment 
 is to study the low-energy radiations and its com- 
 position underwater as it may relate to background 
 in proposed designs of deep undersea neutrino observa- 
 tories. 
 
 Among the possible detectors considered, nuclear 
 track sensitive photographic emulsion was chosen for 
 the following reasons: 
 
 a. The nuclear emulsion is simple, compact, and 
 can be prepared anywhere, even in the confines of a 
 submersible. A particle penetrating into the dense 
 emulsion has a high probability of colliding with 
 nuclei : hence, there is a good chance that the emulsion 
 will show interesting events, including scattering, dis- 
 integrations, and even the formation of new particles. 
 From the moment it is manufactured, an emulsion 
 begins to collect random particle tracks from cosmic 
 rays (and terrestrial radioactivity, if any). It is true 
 that by the time the film is developed it is difficult to 
 disentangle separate events and impossible to tell when 
 the various tracks were made. Moreover, it takes tedi- 
 ous scanning under a high-power microscope to find 
 the tracks at all. However, unlike emulsion records 
 from nuclear accelerator or high-altitude balloon ex- 
 posures, undersea nuclear events are relatively infre- 
 quent (and there is little background "noise"). 
 
 b. They give unprecedented resolution in the ar- 
 rival angle of the cosmic-ray particle. When this in- 
 formation is coupled with the uniform overburden, one 
 may derive considerable information about muons in 
 the trans-accelerator energy region. 
 
 c. It is possible to measure a totally unexplored 
 (except for the ir") region of particle lifetimes ( 10 -11 to 
 10 -16 s).* No other detector has the capability of pro- 
 ducing measurements in this time range, yet recent 
 theories unifying the weak and electromagnetic inter- 
 actions may indicate a new class of particles in this 
 area. 
 
 d. In contrast to electronic counter systems, nu- 
 clear track-sensitive photographic emulsion measures 
 the particles directly, with no "pile up" problem; 
 therefore, relatively lower noise limits accrue. 
 
 e. The nuclear emulsion detector can search for 
 particles between the energy levels of the natural 
 radiation background and the lower limit (usually 20 
 MeV) set by Cerenkov, scintillation, and other coun- 
 ters. 
 
 f. Being passive, nuclear track-sensitive photo- 
 graphic emulsion requires no maintenance or power 
 for operation. 
 
 Data Sought From Nuclear Track-Sensitive 
 Detectors 
 
 The initial experiments have concentrated on the 
 determination of the flux of the low-energy component 
 of the undersea cosmic radiation including the ha- 
 drons. The study of the hadronic component yields 
 information regarding the photonuclear interaction 
 and perhaps other processes due to unkown radiation 
 components as postulated to explain "Cowan events" 
 and Lande "neutrino" bursts. The following is a dis- 
 cussion of measurements of important parameters of 
 the undersea cosmic radiation that can be determined 
 by the use of nuclear track-sensitive detectors and 
 associated arrays. 
 
 Range-Flux and Angular Distribution Measurements 
 of Underseas Muons — The uniform nature of the ab- 
 sorbing medium in these experiments will make it 
 possible to obtain very accurate information on the 
 flux of cosmic-ray particles as a function of depth in 
 water. Particularly interesting would be a check of the 
 absolute flux determinations by Allkofer, which show 
 that at energies from 1 to 50 billion electron-Volts 
 (GeV), the long-accepted flux values were about 25 
 percent too low. Measurements of the angular distri- 
 bution bears in an important way on the existence of 
 the intermediate vector bosons in the study of the weak 
 interactions. 
 
 The primary cosmic radiation greater than 2 X 10 12 
 eV energy would create the postulated intermediate 
 vector bosons** (which have a mass of 58 GeV accord- 
 ing to the Weinberg-Salam Theory). The radiation is 
 
 if = pi-meson or pion, a neutral particle (in this case). 
 
believed to produce muons in the following interac- 
 tions: 
 
 1. p + p-»w + + n + p 
 
 v = neutrino 
 p = proton 
 H = muon 
 Vu = muon-neutrino 
 
 (only neutrino that 
 produces muons) 
 
 2. p + n-»w- + p + p 
 
 w" 
 
 + H 
 
 — The prompt decay of the w ± compared to it and K* 
 decay would produce excess of high-energy muons at 
 large zenith angles. 
 
 Intensity of Stopping Muons — This measurement 
 bears directly on the origin of the x-processes.** 
 The intensity of stopping muons will be measured in 
 the emulsion stacks described later. In the experimental 
 data from underground measurement, there are ex- 
 tremely large differences in the intensity of muons 
 measured by different observers. Since each measure- 
 ment is taken in an underground room of different di- 
 mensions, the fraction of muons contributed by the 
 decay of pions would be expected to show wide varia- 
 tions. The observations in this experiment are made 
 in uniform containers (i.e., emulsion stacks) so that 
 geometry will be the same in each case. In addition, 
 the medium (water) is uniform (fig. 2). 
 
 Underground and Underwater Hadronic Cascades — 
 An underground experiment near Turin, Italy, showed 
 an anomalously high intensity of stopping muons that 
 has led to speculation about the characteristics of the 
 hadronic contamination of the underground muon 
 "beam." In a model proposed by Keuffel, this excess 
 of stopping muons is the result of energetic hadronic 
 cascades produced by fast muons in their interactions 
 with the rock nuclei. Analogous with the degradation 
 of energy in an extensive air shower, these under- 
 ground hadronic cascades have as a constituent of 
 their final products, slow nearly isotropic pions that 
 could decay into muons and result in the observed 
 excess. To get agreement with the Turin results, 
 KeuffeFs model requires either an increase in the 
 photonuclear cross section or the postulation of some 
 new process. In view of the above observation of 
 Keuffel and those of Raman Murthy in India, it is 
 clear that there is a great need for more direct visual 
 
 1,000 10,000 100,000 
 
 Depth in meters of water 
 
 Figure 2. — Variation of muon energy with depth of 
 water penetration. 
 
 observation of and detailed information about the 
 nature of the hadronic cascade under water. 
 
 The large size of the emulsion stack f permits trac- 
 ing or following all tracks produced by a muon — 
 which originate from a star and either interact within 
 or leave the scanning volume (fig. 3). In this way, it 
 will be possible to classify the nuclear cascades for 
 multiplicity of (1) protons, (2) fast pions, and (3) 
 slow pions, as a function of depth. This will give a 
 better understanding of the importance of pions of 
 moderate and low energies to muon and neutrino 
 experiments. 
 
 At a depth of 305 m, the stack is expected to ac- 
 cumulate, in a 1-yr exposure, 34 stopping muons, 2 
 stopping pions, 4 neutron stars, about 10 recoil pro- 
 tons (from fast neutrons) and 1 to 3 muon photonu- 
 clear stars (figs. 4 and 5). 
 
 The Anomalous Neutral Component of Cowan — The 
 purpose is to determine if the strange events of Cowan 
 are due to hadronic cascades. The emulsion stacks 
 used in the proposed research program will be searched 
 for stopping muons. It will be possible to follow back 
 a certain fraction of muons and see if they might have 
 been produced in the emulsion by a neutral radiation 
 of the type described by Cowan. There would be about 
 one such Cowan-type event for each 10 cm 3 of emul- 
 sion exposed for 1 yr. If Cowan's rates are correct, 
 one should find about 40 events in the stacks exposed 
 in these experiments. 
 
 However, there are no firm expectations for finding 
 Cowan events: The chain of circumstances that would 
 produce an unambiguous Cowan "signature" is too 
 serendipitous and too subtle to permit either firm 
 prediction or clear recognition of this phenomenon. 
 
 *K=zKaon or K-meson. 
 * * fis created by neutral particles. 
 
 t About 400 cm 3 of emulsion for each emplacement described 
 here vs. about 70 cm 3 for the earlier HYDROLAB experiments. 
 
a. Relativistic Muon 
 
 f 
 
 tffa 
 
 ■ K \ 
 
 d. Muon electro- 
 magnetic shower 
 
 b. Stopping u.t 
 
 
 « 4u 
 
 ■"> V 
 
 j. Neutron-proton 
 collisions 
 
 e. Inelastic muon 
 interaction with 
 emulsion nuclei, 
 hadronic shower 
 
 g. Muon' production h. Stopping "Jft 
 by a mu neutrino 
 
 k. Coherent neutrino 
 interaction 
 
 c. Stopping A- 
 
 invisible 
 
 •.\r 
 
 f. Muon production 
 by mu neutrino 
 
 Ay* 
 
 * ~:y 
 
 i. Stopping 7T~ 
 
 1. Radioactive decay 
 of trace elements 
 
 Figure 3. — Samples of elementary particle events in nuclear emulsion. 
 
 Inelastic Muon-Nucleon Interactions — The study and 
 understanding of hadronic cascades will result from 
 the scanners finding several inelastic nuclear inter- 
 actions produced by muons. It is most important to 
 make a thorough study of these events. 
 
 The observations of Cottrell on the inelastic scatter- 
 ing of muons showed a wide discrepancy between 
 theory and experiment. As a matter of fact, all experi- 
 mental cosmic-ray observations to date show a major 
 departure from the calculations of quantum electro- 
 dynamics (which is the best theory available to date). 
 This is especially puzzling since the measurements of 
 Cottrell were compared directly with corresponding 
 
 determinations from accelerator-produced muons that 
 agree with theory. Since both measurements were made 
 with the same emulsion technique as well as by the 
 same scanners, the differences can only be due to an 
 important new process or improper understanding of 
 the contributions of hadrons to the underground muon 
 "beam." 
 
 It is hoped to use the muon events found in the 
 present study of hadronic cascades to test the theory of 
 inelastic muon interactions. The experiment will, in 
 this case, make it possible to subtract out the contri- 
 butions of pions and other contaminants to the scatter- 
 ing. 
 
ii — i i i nun — i 1 1 mill — I i i iiiii 
 
 I I llllll 
 
 10 
 
 icr icr 10 
 
 DEPTH (hg/cm 2 ) 
 
 10' 
 
 Figure 4. — Rate of muon stopping as a function of 
 depth of water penetrated. -\- George and Evans 
 (1950), A Barton and Slade (1965), O Short (1963), 
 • Baschiera et al. (1970). Solid curve is calculated 
 rate of stopping. 
 
 APPLIED PHYSICS 
 
 Emulsion Preparation and Development 
 Procedures 
 
 The key and crucial procedure in these missions, 
 and that which makes them unprecedented and unique, 
 is the preparation, under water, of the photographic 
 emulsions at NTP*. The heating, pouring, gelling, and 
 hardening of the liquid emulsion is essentially a 
 physical-chemical process that is sensitive to ambient 
 pressure, humidity, and temperature, and which may 
 be prejudiced by marked increases from NTP and 
 "average" relative humidity (RH) of, say, 50 percent. 
 
 When an emulsion pouring attempt was made in the 
 "La Chalupa"** habitat, some years ago, the emulsion 
 would not gel properly. This was, after some analysis, 
 
 * Normal (i.e., "room") temperature and 1 atm pressure. 
 
 * * An underwater habitat/lab deployed off Puerto Rico. 
 
 10 
 
 >. 
 
 a 
 
 ■a 
 
 i 
 
 E 
 
 rr -4 
 m 
 
 Z) 
 
 UJ 
 
 < 
 
 rr 
 
 -5 
 
 10 
 
 -6 
 
 10 
 
 1 — i — i i 1 1 m i 1 — i i i i i n| 1 — r 
 
 i i i 1 1 nl i i i i 1 1 nl \ i i i iiiii 
 
 j 
 
 10' 
 
 SEA 
 LEVEL 
 
 10' 
 
 10' 
 
 10" 
 
 DEPTH (hg/crri ) 
 
 Figure 5. — Rate of positive ion stopping as a function 
 of depth of water penetrated. Rates not corrected for 
 losses of pions due to decays in Flight near the de- 
 tector. O Short (1963), A Barton and Slade (1965). 
 Solid curve due to Keuffel et al. (1972). 
 
 traced to the high ambient (3 atm) pressure and, to 
 a lesser extent, the 80°F (26°C) temperature and high 
 humidity. For the missions described in this paper, it 
 was hoped, and expected, that the aft-submersible- 
 compartment would be at NTP and less than 50 percent 
 RH. Actually, while P was, of course, 1 atm, the tem- 
 perature hovered around 20° C. The RH was above 50 
 percent, which caused some difficulties with the gelling 
 and especially the drying of the emulsions. 
 
 A summary of the operational procedures and emul- 
 sion characteristics follows, with the detailed sequences 
 appended : 
 
 a. Emulsion Composition and Properties. 
 
 The University of Washington, a pioneer in the use 
 of photographic cosmic-ray detection, has been using 
 a liquid, collodial silver halide (AgBr) solution made 
 in England (ILFORD 1G5). 
 
 The IG5 was used in past HYDROLAB experi- 
 ments and in the 400-ft (120-m) cassette mission 
 described in this report. For the 1,000-ft (330-m) 
 deployment, however, a Kodak NTB-3 emulsion was 
 used — its first underwater application. The NTB-3 is 
 still experimental; however, its physical and photo- 
 
chemical properties seem superior to those of the IG5. 
 The liquid is shipped and kept in plastic bottles until 
 ready for use. The substance is, of course, subjected 
 to cosmic, and other, radiation flux from the moment 
 of manufacture. However, the exposed microscopic 
 trails or tracks left by the traversing particles are not 
 permanent (as in a dried plate), but are quickly 
 blended into the fluid and disappear. 
 
 b. Emulsion Preparation, Coating, Drying, De- 
 velopment, and Scanning* — A Minisequence: 
 
 1. About 500 cm 3 of IG5 and NTB-3 emulsion 
 were transferred into the JOHNSON-SEA- 
 LINK dive chamber after being preheated 
 to around 40°C. 
 
 2. The four bottles were poured out, one after 
 the other, onto the eight, 5- by 5-in almost 
 optically flat glass plates or pellicles that 
 were lying (four at a time) on an aluminum 
 chilled flat table or plate. The yellowish 
 liquid was allowed to spread evenly over 
 each plate, which had its edges blocked by 
 chrome-plated brass "dikes"** to prevent 
 the emulsion from running off the plates. 
 
 The emulsion thickness had to be 400 jam thick. 
 This was attained by pouring out a (previous- 
 ly) accurately weighed volume from each 
 metered bottle. After about one-half hour the 
 material had gelled sufficiently to permit the 
 pellicles to be placed, stacked vertically, into 
 the electrically heated drying "oven" (fig. 6). 
 The plates were separated by about % cm, 
 permitting the blower-forced warm air at 28°C 
 (86°F) to pass over and between them and then 
 through a desiccator bed to keep the chamber's 
 RH at 30 percent, assuming an ambient RH 
 of 60 percent. 
 
 Laboratory tests had shown a drying time of 
 about 5 hr, but, due to higher than expected 
 humidity (about 80 percent) in the submersible 
 compartment and the resultant inability of the 
 drying chamber to hold its own RH below 30 
 percent, the emulsion drying and hardening 
 time lengthened to 8 hr. for the first deploy- 
 ment mission and 6% hr. for the second, re- 
 sulting in total JOHNSON-SEA-LINK bottom 
 times of 11 and 9% hr, respectively. 
 Once dry, the pellicles were packaged, deployed, 
 and left on the ocean bottom (described under 
 "operations"). 
 
 * The sequence applies to both (400-ft and 1,000-ft) deploy- 
 ments and the 400-ft recovery. 
 
 * * Designed and made by Harbor Branch R. and D. per- 
 sonnel 
 
 Drying 
 fii/tnt 
 
 t 
 
 i 
 
 If 
 
 fan 
 
 He a. ter 
 
 //om ,' at i s? a. t 
 
 Th 
 
 errnc S 
 
 tat 
 
 Figure 6. — Simplified sketch of nuclear track-sensitive 
 emulsion drying "oven", and cut-away profile. 
 
 Retrieval of the 400-ft (120-m) cassette (also 
 described under "operations") was followed by 
 development and "fixing" of the pellicles. 
 This process follows fairly conventional 
 photographic practice with a sequence of de- 
 velopment, stopping, and fixing immersions in 
 reducing chemical solutions contained in spe- 
 cial trays designed and built by Harbor Branch. 
 Strict temperature control was maintained, and 
 development was accomplished in less than 5 
 hr for a total mission time of about 8 hr. The 
 chemicals had been previously screened, eval- 
 uated, and cleared regarding toxicity within the 
 JOHNSON-SEA-LINK's chamber's atmosphere. 
 The pellicles were dried within the JOHNSON- 
 SEA-LINK, repackaged, and shipped to the 
 University of Washington physics laboratory 
 for further fixing before analysis. The analysis 
 consists of scanning the emulsions (which are, 
 by now, translucent) with near-field, or some- 
 times phase-contrast microscopes. This scanning 
 is a tedious procedure requiring above-average 
 
eye resolution and a trained perception for the 
 subtle manifestations of muon (and other parti- 
 cle) tracks within the reduced silver/gel colloid. 
 Not only must the initial track (which may be 
 only a fraction of a millimeter long) be de- 
 tected, but its trail through the emulsion, into 
 the next one (if the particle has penetrated that 
 far) must be traced. Most importantly — and this 
 helps to identify the particle — collision proces- 
 ses (if any) must be noted and angles of the 
 "debris" trail must be measured (fig. 7). 
 
 ENGINEERING 
 
 Apparatus Used (Nonmarine) 
 Most of the apparatus used for the emulsion work 
 was designed and built by the Harbor Branch Research 
 and Development staff. The versatility and general 
 quality and innovation demonstrated were exceptional. 
 The missions were successful because of this. 
 
 The following is a list of major equipment that was 
 designed and built for the experiment: 
 
 1. Emulsion drying chamber (fig. 6). 
 
 2. Leveling aluminum chilling "table" with heat 
 transfer fins and cooling bath (fig. 8). 
 
 3. Desiccator cassette. 
 
 4. Emulsion storage heater box. 
 
 5. Four stainless steel bins or tanks, 5-liter capacity 
 each, fabricated by Harbor Branch, were used 
 for the developing and soaking cycles during the 
 400-ft retrieval mission. One tank was thermo- 
 statically controlled at 24°C. (fig. 9). 
 
 Major Marine Facilities and Equipment Used 
 October 1-7, 1977 Mission I, and March 14-16, 1978 
 Mission II 
 
 1. JOHNSON-SEA-LINK No. 2 (fig. 10); crush 
 depth 6,000 ft (1800m) gross weight 23,000 
 lb.* 
 
 2. October 19, 1977/only— The SEA-DIVER sur- 
 face support ship; 100 ft (31 m) long, 270 long 
 ton displacement. 
 
 2A. March 19, 1978/only— The RV JOHNSON sur- 
 face support ship; 123 ft (37.5 m) long, 350 
 long ton displacement. 
 
 3. An ocean-bottom deployed lockout or transfer 
 chamber (fig. 10), suggested, designed, built, 
 and deployed at 1,080 ft (333 m) by Harbor 
 Branch. Emplaced September 1977. 
 
 4. Winching and hoisting gear for the submersible 
 and bottom chamber (fig. 12). 
 
 *A bottom mating flange and split "O" ring were added for 
 lock-on, as were two guide "cones" for directing the vehicle on 
 to 2 guide bars affixed to the bottom "cosmic chamber." 
 
 Figure 7.— Track of a collision between a muon and 
 a proton in an emulsion exposed in HYDROLAB. 
 
 5. Laboratory and mechanical/hydraulic working 
 space and equipment aboard both surface sup- 
 port ships. 
 
 6. Appropriate sonar and Loran C locator equip- 
 ment. 
 
 OPERATIONS 
 
 The sequence of field operations for the October 
 1977 and March 1978 missions was about the same, 
 with these differences: 
 
 1. Kotzer/Stehling/Roesch — Harbor Branch diver 
 and submersible technician, do "dry-run" of 
 emulsion operations inside the JOHNSON-SEA- 
 LINK, in the Harbor Branch shop, a day or two 
 before departure to the test site. 
 
 2. The JOHNSON-SEA-LINK (fig. 10A) was 
 hoisted and lowered by a specially designed 
 crane on the support vessel. 
 
 Harbor Branch ship operators were very adept and 
 experienced at handling the JOHNSON-SEA-LINK 
 
Figure 8. — Liquid emulsion poured on a chilled glass 
 plate (pellicle) surrounded with chrome-brass dikes. 
 
 (JSL), even in fairly rough seas, and few difficulties 
 in retrieving the JSL were encountered during the 
 March mission. The surface support ship was rolling 
 and pitching in moderate seas while the JSL was 
 suspended in midair. 
 
 Diving Procedures 
 
 After several shallow water test dives and a trial 
 rendezvous with the bottom chamber, the chamber was 
 deployed at 1,080 ft. with a sonic "pinger" attached 
 for location by the JSL. The location was also noted 
 from Loran C coordinates. 
 
 During all muon missions, the JSL would dive in 
 the general area of the chamber's location. Each time, 
 via active JSL sonar and signals from the chamber's 
 pinger, the vehicle homed in on, and located, the 
 chamber. This process required from 45 min to 1^2 
 hr depending on equipment performance, above-aver- 
 age currents (about % kt), etc. 
 
 The pilot then maneuvered the JSL on top of the 
 chamber and settled on it, guided by two locator rods. 
 This tricky operation took about 15 min. The JSL 
 had previously removed a plexiglas lid from the 
 chamber, using the manipulator to place the lid next 
 to the chamber for later replacement. 
 
 The JSL finally settled or nestled on the chamber, 
 guided during the actual mating by three wedge- 
 shaped guide fins that prevented lateral movement 
 during contact of the JSL and chamber's flanges (fig. 
 13). 
 
 When the pilot concluded that the JSL had, in fact, 
 made contact and that the grooved "0" ring of the 
 JSL's flange was sitting correctly upon the bottom 
 chamber (b.c), he directed R. Roesch, in the rear, to 
 achieve an atmospheric seal by relieving the water 
 pressure in the chamber by opening a valve connected 
 to the JSL hatch manway. The valve was connected to 
 a one-quarter inch relief line that ran to an atmos- 
 pheric-pressure "holding" tank (later, directly into 
 the JSL aft-end chamber's bilge). When the valve was 
 
 Distilled Water 
 
 Stop Eath 
 
 Plastic Disposal Reservoir 
 10 Liter Capacity 
 
 Time Table for 
 
 400 iim thick pellicles 
 
 1. 1.5 hrs cold developer 
 
 2. 1 hr. warm developer 
 
 3. 1 hr. cold fixer 
 
 Figure 9. — Processing tanks used for nuclear emul- 
 sions during a retrieval mission. 
 
 opened, a loud "thump" could be heard as the pressure 
 in the bottom chamber went to 1 atm, with about a 
 quart of water spraying into the tank (or bilge). 
 
 The valve was then closed and the depth gages were 
 watched; any increase in depth (from "O" on the 
 gage) meant a leak. None occurred, and when the pilot 
 was satisfied with the system's integrity and sealing 
 he directed the rear bottom hatch to be opened. Roesch 
 and Kotzer then lowered the packaged glass sphere 
 into the b.c. For the actual emplacement within the 
 b.c. at the 1,000-ft depth, the sphere was anchored to 
 a weight and floated upward from its own buoyancy. 
 For the 400-ft mission, the sphere was also locked into 
 the b.c, but then removed by the manipulator and 
 transported to the preselected 400-ft site. 
 
 Beginning in March 1978, three successive dives 
 were made for recovery of the 400-ft (120-m) sphere 
 and emulsion development at 1,000 ft. Sea conditions 
 were moderately rough, but the RV JOHNSON, once 
 it was approximately over the b.c. area as located by 
 Loran C coordinates, launched the JOHNSON-SEA- 
 LINK with little difficulty. However, the physical dis- 
 comfort of the JSL crew increased the longer JSL was 
 bobbing on the surface and it was a great physical 
 relief to dive into quiet subsurface water. 
 
 There was no immediate location of the 400-ft 
 package, although the b.c. was located despite a slight 
 current and a seemingly unusual turbidity. 
 
UNDERWATER 
 ELECTRONIC 
 STROBE 
 
 PILOT SPHERE 
 
 SURFACE BUOYANCY 
 TANKS <P ft S) 
 
 DIVER BALLAST 
 TUBE (Pft S) 
 
 VERT 
 /STER 
 
 PILOT SPHERE 
 HATCH COVER 
 
 -PLOT SPHERE 
 
 HOLD- DOWN 
 
 ASSEMBLY 
 
 r SONAR ANTENNA 
 
 r\ 
 
 LIFT CLAMP 
 ASSEMBLY 
 
 DIVER COMPARTMENT 
 
 STRONGBACK 
 
 AUX GAS 
 STORAGE 
 (P.ftS) 
 
 PILOT SPHERE 
 AIR CONDITIONER 
 
 a dehumioification 
 
 UNIT 
 
 SONAR TEST TRANSDUCER 
 
 DEEP SEA FLASHER 
 
 BEACON PINGER, S7KHZ 
 PASSIVE TRACKING SYSTEM ' 
 
 NON-C'RECTIONAL UNOERWA-Ef- 
 , . T ELEPHONE TRANSDUCER 
 
 BATTERY 
 COMPARTMENT 
 EMERGENCY 
 RELEASE 
 
 3ATTERY 
 COMPARTMENT 
 14 2V CELLS 
 
 BOTTOM PENETRATION HATCH 
 
 
 Figure 10.— The JOHNSON-SEA-LINK shown A) in cut-away profile, B) at aft end 
 of the R/V JOHNSON surface-support ship, C) in bottom hatch detail, and D) 
 specifications and operating characteristics. 
 
 B 
 
 
 r- 
 
 
 — L 
 t ,1, | rt*- H 
 
 f-~ 
 
 
 £*> 
 
 T 'S-irj^jj 
 
 ,\m 
 
 F*^-«-^^^ 
 
 Figure 10. — (continued) 
 
 The next day, a second dive located the 400-ft sphere 
 (although its "pinger" had quit), because of its prox- 
 imity to an overturned bus whose position relative to 
 the b.c. had been mapped. A back-vector from the b.c. 
 
 Figure 10. — (continued) 
 
 put the JSL on course. The sphere was grabbed by the 
 manipulator, and the JSL returned to the b.c. and 
 dropped in the sphere. 
 
 On the third day the emulsion cassette sphere was 
 retrieved from the b.c. and the film package was found 
 intact although a bit of water (about 50 cc) was found 
 
 10 
 
OPERATING CHARACTERISTICS 
 
 JOHNSON-SEA-LINK I & 
 Specifications* 
 
 DIMENSIONS 
 
 
 
 Overall 
 
 
 
 Lenglh 
 
 22- 10" 
 
 
 Beam 
 
 T ■ 11" 
 
 
 Height 
 
 10- ■ 7" 
 
 
 Draft 
 
 7'- 6" 
 
 
 Gross Weight 
 
 23,000 Ihs. 
 
 
 Pilot Sphere 
 
 
 
 Outside Diameter 
 
 6G" 
 
 
 Inside Diameter 
 
 58" 
 
 
 Thickness 
 
 4" 
 
 
 Internal Volume 
 
 59 cu. It. 
 
 
 Hatch Clear Ooening 
 
 18" diameter 
 
 
 Material 
 
 Acryl.c Plexiglas Grade 
 Annealed 
 
 'G 
 
 Diver Compartment 
 
 
 
 Length 
 
 8' 
 
 
 Outside Diamoter 
 
 59'/;" 
 
 
 Internal Diameter 
 
 53" 
 
 
 Hatch Clear Opening 
 
 20" diameter 
 
 
 Material 
 
 Aluminum Alloy 5456 
 
 
 Internal Pressure 
 
 Test pressure 1,000 psi 
 
 
 
 Operating pressure 670 
 
 psi 
 
 'Specifications apply to both submersibles, since they differ only in minor respects. 
 
 Depth 
 
 Operating Depth 
 
 ABS Classification Depth 
 
 Test Depth 
 
 -Crush Depth 
 
 Speed 
 
 Cruise 
 Maximum 
 
 Life Support 
 
 Endurance 
 
 Carbon Dioxide Scrubbers 
 Pilot Sphere 
 Diver Compartment 
 
 Emeigency Breathing Masks 
 Pilot Sphere 
 Diver Compartment 
 
 Metabolic Oxygen Bleed 
 
 Oxygen An.ilyzer 
 Pilot Sphere 
 
 Diver Compartment 
 
 Carbon Dioxide Monitors 
 Pilot Sphere 
 
 1.000' 
 1,000' 
 2.000' 
 6.000' 
 
 3/4 knots 
 1 3/4 knots 
 
 480 man-hours (20 man-days) 
 
 Harbor Branch Foundation 
 Li ndbergh-Hammer 
 
 Diver Compartment 
 Emergency Life Support-Rebreathers 
 Pilot Sphere 
 Diver Compartment 
 
 Power 
 
 Oil Compensated Lead Acid Battery 
 
 Inverter 
 
 Equipment on Board 
 
 Six Function Manipulator 
 
 Sonar 
 
 Dopplcr Navigation 
 
 Underwater Telephone 
 
 VHF Transceiver 
 
 Zenun Short Arc Light 
 
 Flood and Spot Lights 
 
 Emergency Location and Rescue Buoy 
 
 Deep Sna Still, Movie and Video Camera Systems 
 
 Video Tape Recorder 
 
 Fail Sale Drop Lock Sub Release System 
 
 Adjustable Equipment Arm 
 
 Diver Self-Contained Rebreathing Apparatus 
 
 Optional Equipment 
 Cable Cutter 
 Line Cutter 
 Rotenone Dispenser 
 Sea Hook 
 Corer 
 
 Two 
 
 One Analyzer, One Remote Meter 
 from Diver Compartment 
 One Oxygen Monitor 
 
 One Carbon Dioxide Monitor, One 
 Analyzer. One Remote Meter from 
 Diver Compartment 
 One Monitor, One Analyzer 
 
 Two 
 Two 
 
 32 KWH @ 23 VDC 
 
 1 1 7 VAC @ 2.5 amps 60 HZ 
 
 Figure 10. — (continued) 
 
 in the sphere. It was probably condensed moisture 
 trapped in the sphere and also exuded from the 
 pellicles. The film pellicles were unwrapped from their 
 lightproof covering and then developed and "stopped" 
 in about 3 hr. A minor incident enlivened this mission: 
 the defunct sonic pinger on the cassette, with 1,000-ft 
 (330 m) water apparently trapped in its batteries, 
 "exploded" a few seconds after it reached atmospheric 
 pressure in the after chamber. The two crew members 
 were lightly spattered with chemicals, zinc, etc., but 
 no eyes were damaged because crewmembers both had 
 been looking away at the moment. They will wear 
 safety glasses next time, although no such pinger will 
 again be used. 
 
 CONCLUSIONS 
 
 In general, the missions were accomplished suc- 
 cessfully with only trival mechanical, electrical, or 
 
 hydraulic problems. 
 
 The b.c, built at considerable expense by Harbor 
 Branch, was a brilliant innovation that permitted dry 
 lockout at atmospheric pressure. It can be used to 
 2,000 ft. (660 m) or more; as deep as the JSL can go, 
 in fact. 
 
 Other experiments, physics, biology, and the like, 
 can be accommodated. The b.c. can be retrieved at will 
 for inspection and cleaning. However, after 6 mo 
 down, no corrosion or coatings were noticed and not 
 much may ever accumulate because of the relatively 
 sterile ambience and the very little free O2 available 
 to produce corrosion. 
 
 New and otherwise unobtainable high-energy 
 physics and cosmic ray data can be obtained with 
 undersea experiments of this kind. 
 
 Glass spheres, as experiment apparatus (emulsions 
 in this case, and perhaps photomultiplier or solid 
 
 11 
 
Figure 11 — Detail drawings of the Harbor Branch deep submergence, lockout trans- 
 fer chamber. 
 
 Washington/Western University (and now Harl 
 Branch Foundation) missions are beginning to cc 
 sider deeper ocean deployment of large arrays of pi 
 toelectric and even acoustic cosmic ray (neutrin 
 detectors. However, the small-scale experiments i 
 scribed here, and their probable electronic successo 
 fill a valuable niche in the panoply of possible cosn 
 radiation sensing techniques. 
 
 The NOAA/University of Washington/Weste 
 Washington University /Harbor Branch Foundati 
 association has been successful and mutually prodi 
 tive. The Harbor Branch Foundation have invesl 
 large funds in these missions and the engineeri 
 support work. The NOAA funding contribution 
 Harbor Branch Foundation, while growing, has be 
 — and still is — relatively modest with Harbor Bran 
 Foundation still providing the largest fraction of ea 
 mission support. 
 
 The use of the JOHNSON-SEA-LINK for the pi 
 pose described herein is an example of an unders 
 laboratory application. 
 
 Figure 12. — Winching and hoisting gear lowering 
 lockout transfer chamber into ocean. 
 
 state detectors in the future) are relatively inexpensive, 
 reliable and convenient "pressure vessels" for deep 
 ocean work. 
 
 Other (besides University of Washington/Western 
 Washington University) U.S. and foreign physics 
 groups noting the success of the NOAA/University of 
 
 12 
 
ATMOSPHERIC CHAMBER FOR 
 PLATFORM CHAMBER PRESSURE 
 BLEED OFF 
 
 PLATFORM CHAMBER' 
 
 'G^ggfcp 
 
 -> 
 
 _to- 
 
 Figure 13. — Schematic of sub and platform chamber for dry transfer of pellicle plates. 
 
 BIBLIOGRAPHY 
 
 1. "Electromagnetic Interactions of 5-50 GeV/c 
 Cosmic Ray Muons with Electrons", P. Kotzer, Uni- 
 versity of Washington Dissertation, 1964. 
 
 2. "Positive Excess of Shower Producing Cosmic- 
 Ray Particles", S. H. Neddermeyer, S. Curtis, P. 
 Kotzer, Bulletin of the American Physicial Society, 7, 
 1962. 
 
 3. "Muon-Electron Interactions at High Energies", 
 P. Kotzer and S. H. Neddermeyer, Bulletin of the 
 American Physical Society, 7, (463), 1962. 
 
 4. "Muon-Negation Interactions at High Four- 
 Momentum Transfers", P. Kotzer and S. H. Nedder- 
 meyer, Bulletin of the American Physical Society, 10, 
 (80), 1965. 
 
 5. "Scattering of Cosmic-Ray Muons on Electrons", 
 P. Kotzer and S. H. Neddermeyer, Bulletin of the 
 American Physical Society, 12, 1967. 
 
 6. Abstract for Presentation to American Physical 
 Society Meeting, Washington, D.C., on "Observations 
 on Cosmic Ray Quark Like Tracks in a Cloud Chamber 
 in a Magnetic Field". 1971. 
 
 7. "Proton-Tungston Nuclear Collisions at 200 GeV", 
 J. R. Florian, L. B. Kirkpatrick, J. J. Lord, J. Martin, 
 R. E. Gibbs, Peter Kotzer, R. Piserchio (1973), A. LP. 
 Conference Proceedings No. 3, Particles and Fields 
 Subseries No. 2 (1973), Vanderbuilt University, Nash- 
 ville, Tenn. 
 
 8. "Underwater Cosmic Rays", P. Kotzer and Jere 
 J. Lord (1973), Hydrolab. Journal, 1, (2), July 1973. 
 
 9. "Cosmic-Ray Nuclear Interactions Over 5 Tev and 
 Comparison with Scaling", J. W. Martin, J. R. Florian, 
 Robert E. Gibbs, Peter Kotzer, J. J. Lord. (1973), 
 Proceedings of the 13th International Conference on 
 Cosmic Rays, Denver, Colo. 
 
 10. "Cosmic-Ray Muons Underwater", S. Anderson, 
 J. J. Lord, and Peter Kotzer. (1973). Proceedings of 
 the 13th International Conference on Cosmic Rays, 
 Denver, Colo. 
 
 11. "Proton Interactions in Heavy Nuclei at 200 
 GeV", J. R. Florian, L. B. Kirkpatrick, J. J. Lord, J. 
 Martin, R. E. Gibbs, P. Kotzer, R. Piserchio. Paper — 
 A.I.P. Division of Particles and Fields, 1973 Meeting, 
 Berkeley, Calif. 
 
 13 
 
12. "Changing Composition of Cosmic Ray Pri- 
 maries in the TeV Energy Range", P. Kotzer, S. N. 
 Anderson, J. R. Florian, L. D. Kirkpatrick, J. J. Lord, 
 J. W. Martin, A. I. P. Division of Cosmic Rays, 1973, 
 Tucson, Ariz. 
 
 13. "Composition of Cosmic Ray Primaries at En- 
 ergies > 1 TeV/Nucleon", P. Kotzer, S. N. Anderson, 
 J. R. Florian, L. D. Kirkpatrick. J. J. Lord, J. W. 
 Martin, A.I.P. Division of Cosmic Rays, April 1974 
 
 14. "Cosmic Ray Nuclear Interactions at Very High 
 Energies", J. W. Martin, J. R. Florian, L. D. Kirk- 
 patrick, J. J. Lord, R. E. Gibbs, P. Kotzer, American' 
 Physical Society, Washington, D.C., April 1974 
 
 15. "Neutron Production by Muons at Various 
 Depths Underwater", S. Anderson, P. Kotzer, J. J. 
 Lord, American Physical Society, June 1974 
 
 16. "Interaction of 300 GeV Protons with Tungsten 
 and Silver," Abstract submitted for the Fall meeting 
 of the Division of Particles and Fields of the American 
 Physical Society, 1975. J. R. Florian, L. D. Kirkpatrick, 
 J. J. Lord and J. W. Martin, Univ. of Wash., R. E. 
 Gibbs, East Washington State College and P. Kotzer, 
 Fairhaven College. 
 
 17. "Absorption and Interactions of the Cosmic Ray 
 Muon Beam in Great Thicknesses of Matter," Abstract 
 submitted for the Annual Meeting of The American 
 Physical Society, Anaheim, California, Jan-Feb 1975, 
 S. Anderson, P. Kotzer and J. J. Lord Unievrsity of 
 Washington, Seattle. 
 
 18. "Slow Muons and Other Associated, Locally 
 Produced Particle Fluxes at 60 Meters Underwater" 
 P. Kotzer, S. Anderson, J. J. Lord, K. Stehling, Pro- 
 ceedings of the 14th International Cosmic Ray Con- 
 ference 1975, Max Planck Institut Fur Extrater- 
 restrische Physik, Miinchen, Germany. 
 
 19. "Anomalous Stopping Particles at Great Depths 
 Underground" P. Kotzer, S. Anderson, J. J. Lord, 
 
 Proceedings of the 14th IUPAP International Cosmic 
 Ray Conference 1975, Max Planck Institut Fur Ex- 
 traterestrische Physik, Miinchen, Germany. 
 
 20. "Proceeding of the 1975 Summer Workshop on 
 Neutrino Interactions in the Ocean Depths and on 
 Oceanographic Physics and on Marine Engineering, 
 twenty four contributions, 317 pages, Western Wash- 
 ington State College, 1976, P. Kotzer, editor. 
 
 21. "Design Parameters of Large Scale Underseas 
 Supernova Neutrino Detectors" P. Kotzer, D. Davis- 
 son, J. J. Lord, S. Neddermeyer, K. Stehling, Bulletin 
 of the American Physical Society, April 1976. 
 
 22 "Residue Cosmic Ray Muon Fluxes at Great 
 Depths Underground", P. Kotzer, S. Anderson, R. 
 Lindsay, J. J. Lord, Bulletin of the American Physical 
 Society, April 1976. 
 
 23. "DUMAND as a Supernova Neutrino Detector", 
 P. Kotzer, J. Lord, F. Reines, Proceedings of the 1975 
 Summer Workshop on Neutrino Interactions in the 
 Ocean Depths and on Oceanographic Physics and on 
 Marine Engineering, Western Washington State Uni- 
 versity, Bellingham, 1976. 
 
 24. "Long Range Alpha Particles and Correlation 
 with Superheavy Nuclei" P. Kotzer, R. Lindsay, S. 
 Anderson, J. J. Lord, S. Neddermeyer Paper presented 
 at the Annual Meeting of the APS/AAPT. Chicago, 
 111., 7-10 February 1977. 
 
 25. "Neutrino Detection in an Undersea Habitat", 
 Kurt R. Stehling, Sea Technology, December 1973. 
 
 26. "Man and the Atom in the Ocean", Kurt R. 
 Stehling, NO A A Magazine, Vol. 5, No. 1, January 
 1975. 
 
 27. "Keeping a Watery Eye on the Universe", 
 Kurt R. Stehling, NO A A Magazine, Vol. 7, No. 2, 
 April 1977. 
 
 28. "Manned Submersible Study Cosmic Radiation 
 Deep in the Sea", Robert S. Jones, Peter Kotzer, Sea 
 Technology, March 1978. 
 
 •U.S. GOVERNMENT PRINTING OFFICE: 1979 0—274-543 
 
 14 
 
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