R130
Discossisn
Preshoc calculations sinilar to those presented bere were made at Sandia
Laborate: 3
The differences berween the present effort ami preshot work are
as follows:
(a) accorate, rather than predicted, rocket trajectories were used, together with accurate positioning of the warbead at zero tice.
(>) Clood-rise rates were inserted on the basis of ‘observations; in Im1601 they were ceglected.
(c) Bo effort was made in this analysis to include the effects of gamma
rays prodoced by neutrons captured in nitrogen.
treatment.
This is a defect in the present
However, the Large mass of material in the Redstone missile between
the warhbcad and che earth prevented a good fraction of ¢he neutrons which otherwise would hrve escaped in that direction from so doing.
Monte Carlo calcula-
tious by C. RB. Hebi* of Sandia indicate that the frequency of (n, 7) reaction
is samewbat lover than had been estimated.> Further, ‘the (n, 7) source is extended in space.
For these reasons, it is felt that (n, 7) contributions were
not significant, apd no indication of this compovenotis found in the data.,
There is more information available from the model. From Table 4.2 one
ean find a quantity proportional to the energy deposited per unit path length
in the atmosphere.
This is done in a straightforward way by converting the
mumber of ga/es* of air traversed to an equivalentheight in the atmosphere.
This results in the integral curve sbown in Fig. 4.9.
actually, the intensity is given by
I(r) =
Pbate
ett
i s
2
ar
and Fig. 4.9 is, as indicated, a plor of har? 1(r)/1, versus r.
of this function is also plotted in Fig. &.9.
The derivative
This curve is, togerher with the
integral carve, a mezsure of energy deposition per unit path length in the at-
mosphere.
The caximm of the derivative in Fig. 4.9 oceurs at about 21 to 23
km above the earth's surface.
This is in rough agreement with sore sophisti-
cated calculations of the height of maximm erergy deposition.
Cy,
LASL results?
115
Lt