Theory of the Fireball

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i.e., the part which has not yet been reached by the cooling wave, con- tinues to expand adiabatically; it therefore cools very slowly and remains opaque . Af'ter the entire isothermal sphere is used up, the fireball becomes transparent and the radiation drops rapidly. The ball w ill therefore be left at a rather high temperature (Sec. 7), about 5 0'. The cooling wave reaches the isothermal sphere at a definite pressure p, M 5(p1/po) 1/3 bars, where p is the ambient and po the sea level 1 density. The radiating temperature at this time is about 10, OOOo . The slight dependence of physical properties on yield is exhibited in approx- mte formulae.. 4
I am greatly indebted to Harold Brode of the Rand Corporation for giving me a patient introduction to the work on fireball dynamics since World War 11, for sending me the pertinent Rand publications on the sub- ject, and for doing a special numerical computation for me. To Burton Freeman of General Atomic I am grateful for several interesting discus- ! sions of fireball development and opacities of air. I want to thank Herman Hoerlin for much information on the observational material, and for selecting for me pertinent Los Alms reports. I am ?specially grateful to Albert Petschek for critical reading of the manuscript and for several helpful additions. My thanks are also due to many other members of Groups J-10 and T-12 at Los Alamos, to J. C, Stuart and K. D. watt at General Atomic, Bennett Kivel and J. C. Keck at Avco-Everett, and to F . R. Gilmore at Rand for important infomat ion. 5 . I ~
Page 1 and 2: , - Ip.L ,. : CIC-14 REPORT COLLECT
Page 3: LA-3064 UC-34, PHYSICS TID-4500 (30
Page 9: 1. INTRODUCTION 2. PHASES IN DETELO
Page 12 and 13: 6 radiation .(Stage A of Sec. 2) is
Page 14 and 15: frequency, the opacity, which is su
Page 16 and 17: elations as (3.2) between shock rad
Page 18 and 19: in this case there is no Stage D 11
Page 20 and 21: highest possible density of about l
Page 22 and 23: \ and the average of y' is taken ov
Page 24 and 25: The radius R is given R3 = I"- P P
Page 26 and 27: T-R -10 (3.16) 8 The numerical calc
Page 28 and 29: Since the interesting values of R a
Page 30 and 31: Most of the radiation comes from a
Page 32 and 33: higher frequency (above, and Sec. L
Page 34 and 35: 4. ABSORPTION coEFF1c1ms a. Infrare
Page 36 and 37: (3.21), it is small compared to the
Page 38 and 39: hv (ev) P/Po = 1 ff N2 0- Table N.
Page 40 and 41: w Q P/Po 1 0.1 0.01 T 4,000 6,000 8
Page 42 and 43: Table VI. Average Mean Free Paths (
Page 44 and 45: The fraction of the Planck spectm b
Page 46 and 47: The W beyond 3.5 ev will be strongl
Page 48 and 49: The equation of continuity is aH aJ
Page 50 and 51: U" J, A Ho - H(T1) To determine u w
Page 52 and 53: temperature is aromd Tb, and in whi
Page 54 and 55: internal energy in that sFhere; in
Page 56 and 57:
y integrating (5.8); it depends on
Page 58 and 59:
a log I1 - y' - 1 a log p at - y' a
Page 60 and 61:
2 vitn A = 0.1G q/cm and n = 6.3. T
Page 62 and 63:
or a radiating temperature of 10,80
Page 64 and 65:
assuming the strong shock relation
Page 66 and 67:
pressure is larger than pa, (5.50)
Page 68 and 69:
inconsistency in our apyroximations
Page 70 and 71:
G. We& Cool-ing Wave In Stage C I1
Page 72 and 73:
6. EFFECT OF THREE DDENSIOUS a. Ini
Page 74 and 75:
6. Sinrinkage of Isotnemal Sphere W
Page 76 and 77:
Pa f(x) = - P and obtain the simple
Page 78 and 79:
From y = 1.18, y=l-A Y= -1 2.2 - 0*
Page 80 and 81:
where Re is the outer edge of the l
Page 82 and 83:
esult of the three-dimensional cons
Page 84 and 85:
4 dF: = - 4KaT at where a is the St
Page 86 and 87:
1. 2. 3. 4. 5. 6. 7. 8. 9. 10 . REF
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Theory of the Fireball

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