AD-AI07 918 NAVAL RESEARCH LAB WASHINGTON DC F/6 18/3THE PHARO CODE(U)NOV 81 E HYMAN, M MULBRANDON, S L OSSAKOW

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E. Hyman*, M. Mulbrandon, and S. L. Ossakow

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*Present address: Science Applications, Inc., McLean, Virginia 22102

This research was sponsored by the Defense Nuclear Agency under Subtask S99QAXHC, work unit00011, and work unit title, "Phoenix."

It. KEY WORDS (Co1fn.. on "e10o ado II n.cet..ary ad Identfy by block nutrb.)

Visible radiation SensorsInfrared radiation Line and band transitionsIsophots High altitude nuclear data comparisonsCameras

2 STRACT (Continue on reverse tIde It necessary and Identify by block nu..ber)

The PHARO code predicts the visible and infrared radiative output of high altitude nuclear bursts.Using the results of the large scale NRL hydrocodes, both the spatial and temporal variation of theradiation (watts sr) in arbitrary wavelength intervals is determined. The results are a series of"isophot" plots for rbitrariiy placed cameras or sensors which can be tirectly compared with experi-ment. In addition)1 monitoring the important line and band transitions the bound-bound, free-bound,and free-free radia ion is calculated for a recombining oxygen plasma. In particular, the bound-bound

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20. ABSTRACT (Continued)

radiation does not assume a Saha population of excited levels but calculates this radiation as a functionof electron temperature and density and ground state oxygen density. Comparisons with representa-tive high altitude data are exhibited.

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CONTENTS

I. INTRODUCTION ..................................... 1

II. HANE RADIATIVE EMISSION CALCULATIONS ........... 2

III. PHARO GEOMETRY ................................... 5

IV. RESULTS AND DISCUSSIONS ........................... 6

ACKNOWLEDGMENT ................................. 8

REFERENCES ....................................... 18

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THE PHARO CODE

SECTION I

INTRODUCTION

PHARO, an acronym for "Phenomenology and Radiation Output,"

is a computer code developed to calculate the visible and infrared

(IR) emission from a disturbed atmosphere. As part of NRL's high

altitude nuclear effects (HANE) program, it utilizes the results

of NRL's high altitude phenomenology calculations, specifically

the MRHYDE (and its successor, PHOENIX) computer code. It is

currently being used, also, to study LWIR emission from plasma

cloud releases, using codes which model the development of spatial

irregularities in the high altitude atmosphere. PHARO calculates

emission in the visible and IR from all sources of radiation

including:

(1) bound-bound transitions in the decaying atomic

plasma and transitions from the low lying metastable

states of atoms and atomic ions,

(2) band emission from molecules due to electron impact

excitation or heavy particle reactions, which leave

a product species in an excited electronic or

vibrational state (e.g., chemiluminescence),

(3) free-bound and free-free continuum transitions.

A detailed description of these lines and bands is given in

Section II.

The output of the PHARO code consists of contour plots of

radiative intensity (watts/cm ster) or "isophot" plots for

arbitrarily placed sensors. These will be described in more detail

in Section III. A series of these plots give both a spatial and

Manuscript submitted August 25, 1981.1

I I 'i - I

temporal picture of the radiation, which is directly comparable

with experiments. In Section IV we present a comparison between

PIARO results and some measured values, and a discussion of further

potential comparisons.

Briefly, PFARO works as follows: the calculation of the

radiation starts with the results of a computer code such as MRHYDE,

a three-dimensional, two fluid MHD reactive flow code which describes

both the hydrodynamics and chemistry of the high altitude burst.

MRIYDE begins its calculations on the order of one second after burst,

using as initial conditions the atmosphere after prompt x-ray emis-

sions and deposition of uv energy, debris energy, and inclusion of

a blast wave.

The PHARO code reads from tape the MRHYDE results at

prespecified times and at a large number of mesh points. For the

results we will present in this report, there were of order 104

mesh points (due to reflection symmetry about a vertical plane

through the magnetic field there are effectively twice this number).

This report will describe PHARO II which differs from PHARO I 1

primarily in the treatment of the bound-bound radiation. In PHARO I

the calculations assumed a hydrogenic recombining plasma with Saha

populations of the excited states. In PHARO II an oxygen plasma

is assumed and actual population densities of the excited states

are calculated.(2)

SECTION II

HANE RADIATIVE EMISSION CALCULATIONS

The species carried in the MRHYDE code are given in Figure 1.

The temperatures listed are the electron temperature, Te, the

2

vibrational temperature of N2, TV, and the heavy particle kinetic

temperature, Ta . Some of the HANE codes currently carry separately

the ion temperature, Ti, and the neutral temperature, Tn* N is

not carried in MRHYDE since it is generally a minor ion by the

time the MRHYDE calculations are initiated. It is carried in the

iv deposition code which provides initial conditions for MRHYDE,

however. In Figure 2 we exhibit the major line emissions from

metastable states and molecular bands that the PHARO code monitors.

It is apparent that not all of the excited state species that we

require for PHARO are carried in MRHYDE. Those not carried we

assume to be in quasi-steady state equilibrium and calculate their

populations. The species for which this assumption is used are

N(2 P), O( S), N+ ( 1 S), 0 ( D), 0+(2P), 02 (a A), and 0 2 (blE).

To calculate the NO chemiluminescence in the fundamental at

S.3p and the overtone at 2.7p the following assumptions were used.

The vibrationally excited NO, formed via the reaction N + 02 - NO + 0,

is sufficiently exothermic to populate NO up to the 6th vibrational

state. In addition, N(2D) + 02 - NO + 0 can excite up to the 18th

vibrational level of NO. We assume half the exothermicity is

available to vibrational states. A straight-forward steady state

calculation then gives the number of photons of the fundamental and

overtone for these reactions. Since quenching has not been included,

this will give an upper limit to the emitted radiation. Also, we

include the translation-vibration reaction between NO and hot 0

atoms which is frequently a critically important source of 5.30

and 2.7p radiation. In some applications more sophisticated models

have been used for determining the number of photons/reaction.

3

In a similar way the NO+ radiation from vibrational transitions

at 4.3p and 2.15V are calculated(3) assuming formation of vibra-

tionally excited NO+ via N+ + NO - N + NO +, N + 02 - NO + + 0,2

N2 + 0 NO+ + N, N+ + O2 NO + + 0. In addition, the N2 Meinel(3) + D) +A2

Bands are assumed to arise (3) aN 2 + N2 (A~n, v = 1) + o

v 2

and the second negative of 04 in the visible is assumed (3) to result

from 0+(2 D) + 02 -1 0(A 21) + 0. Finally, a model for the 4 .3p andU 10.6p radiation from CO2 is included.

To calculate the late-time atomic bound-bound line radiation

PHARO II assumes the late-time disturbed atmosphere to be a decaying

oxygen plasma. Calculation of the radiation requires a knowledge of

the population of the excited states of oxygen as a function of

electron density and temperature and, for sufficiently high temper-

ature, the ground state population, O(3P). To accomplish this a

model (2) has been developed which determines the population densities

of all triplet and quintet oxygen levels up to n = 18 as a function

of these parameters. These calculations have been performed for 11

electron temperatures ranging between .03 and 2.0 eV, 7 electron

densities between 10 and 101 2cm , and, in the case of electron

temperatures equal to or greater than .5 eV, the same range of

oxygen ground state densities.

The results of the above calculations, the population of 338

excited levels for each of the above set of parameters, are stored

on disk. Once wavelength intervals are specified a separate code

reads the disk and determines the radiation emitted in each wave-

length interval for each set of parameters. These results are,

in turn, stored on a disk which is read by the PHARO code for

4

interpolation to the actual temperature and densities at a

given point.

Finally, the continuum radiation, oxygen free-bound and free-

free emission, are based on the calculations of Davis and Lewis.(4 )

SECTION III

PHARO GEOMETRY

In Figure 3 we display the geometry used in the PHARO code

to produce the "isophot" plots. B represents the initial burst

position. The X-axis is in the direction of the horizontal com-

ponent of the earth's magnetic field. The proposed position of

the camera or sensor is specified by its distance from the burst

point, s, a polar angle relative to the upward vertical direction

at the burst, e, and an azimuthal angle, (D, measured relative to

the horizontal magnetic field direction. A camera at this position

may have an arbitrary orientation relative to the burst point. Two

angles specify the direction of the line of sight of the sensor:

a polar angle, o, relative to the burst-sensor line and an azimuth

angle, 0, (not shown in Figure 3) measured relative to the plane

defined by the burst point, the sensor position, and the center of

the earth.

Having specified the sensor position and orientation a set

of rays is constructed. The first ray is along the line of sight

of the sensor (as indicated in Figure 3) and the others are arrayed

on a set of equally spaced cones with common apex at the sensor

point and common axis along the sensor line of sight. On each

cone the rays are equally spaced around the cone. Next, a set of

equally spaced points is chosen along each ray, from the sensor to

5

-MR

the far side of the MRHYDE mesh. By interpolation between the

MRHYDE mesh points and these points the total emission at each

point along the rays is determined for each wavelength interval

of interest, using an appropriate volume as illustrated in Figure 3.

Finally, a summation is performed along each ray and the total radi-

ation (watts/cm 2ster) from each ray direction determined. In the

present version of the code, PHARO II, the emission is assumed to

be optically thin. Furthermore, the code permits attenuation of

the radiation as it travels from its source through the ambient

atmosphere to the sensor. An atmospheric model has been developed

and incorporated into PHARO based on the models of McClatchey at

AFGL.

The set of ray directions relative to the sensor line of

sight form a two-dimensional polar grid of intensities from which

the contour plots are constructed. In some applications of the

PIIARO code, the rays are arrayed on a rectangular grid and the

contour plots are constructed from a two-dimensional rectangular

grid. With a PHARO sensor placed where measurements were taken

it is possible to construct plots that can be directly compared

with experimental isophot plots.

SECTION IV

RESULTS A1,D DISCUSSION

In Figures 4-8 we exhibit typical PHARO plots predicting the

radiance (watts/cm ster) in the 8-14p band from a high altitude

nuclear burst at successive times following initiation of the

MRHYDE calculation (times 0.0, 20.0, 60.0, 100.0, and 140.0 seconds).

The camera is a distance of 500 km from the burst with its optic

6

axis passing through the burst point. The ordinate and abscissa

give the angle in degrees from the camera axis. Alternate contours

are solid lines or dots, with the latter, only, labeled. The

numbers at the top of the plot label the radiance values. Reading

from left to right, the leftmost value corresponds to contour

number 1 which is the smallest radiance value that can be plotted,

the middle number to contour number 10, and the rightmost number

the inverse of the number of contours per logarithmic decade. Thus,

in Figure 4, contour 8 represents a radiance of 1 x 10-5 watts/cm 2ster

and contour 2 is 1 x 10 watts/cm ster. The Figures 4-8 exhibit

clearly the temporal effects: the effect of the hydrodynamics in

heating the atmosphere and diffusing the plasma, and the chemistry

in reducing the emission.

In Figure 9 we see a measured isophot plot of visible radiation

from a high altitude burst (on the right) and the corresponding PHARO

prediction. Additional predictions and comparisons with data have

been documented in the literature.

We view the PHARO code as a very versatile code particularly

useful in providing predictions that are easily compared directly

with measurements. Specifically, the high altitude bursts that

can be modeled by a MRIIYDE (PHOENIX) 3D 2-fluid magnetohydrodynamic

code provide a set of measurements that can provide direct tests

of our understanding of disturbed atmosphere phenomenology. In

the past several years there have been important improvements in

our understanding of a variety of these atmospheric phenomena

that directly bear on measurements that were made, and that "a\'c

not been tested by comparison with these results.

7

Consider the Starfish event. There are a set of isophot

plots of visible radiation that have been published for times out

to 33.9 seconds of the northern conjugate region from an aircraft.

There are similar data from other locations that has not been

analyzed. This kind of data is in an ideal form for comparison

with PHARO predictions.

In addition, there were IR measurements made with a variety

of detectors on each of two aircraft. In many cases data above

background were obtained for 103 seconds. The measurements include

the 1.1 - 3 .Oi band (spatial radiometer), 4.8 - S.Sp band and

2.6 - 2.7p band (filter photometer), a variety of bands between

1.5 and 2.8p (filter wheel radiometer), 1.55 - 1.6211 (PbS radio-

meter), 5.0 - 5.51 (IR Spectrometer). There are, in addition, a

variety of uv, visible, and near infrared measurements made both

from aircraft and ground stations. The reliability, extent, and

state of analysis of this large quantity and variety of data

require evaluation. But, in principle, PHARO predictions make

these measurements directly accessible to analysis.

ACKNOWLEDGMENTFThis work was supported by the Defense Nuclear Agency.

8

N2 , 0 2 , NO

0+ +2O NO"", 2"

N, N(2D), N +

O, 0 1D), 0 +

Te, Tv, TaFig. 1 - Chemical species and temperatures carried in MRHYDE

(and PHOENIX) 3D hydrocode

° " 9

PHARO II

PHENOMENOLOGY AND RADIATION OUTPUT CODE

OPTICAL AND IR TRANSITIONSo o

6300A, 5577A

N 5200A, 1.04,u

N+ 6527A,5754&

0 + 7320A2 3914A, 9212A, 1.5m

02 7619A, 1.26p

NO 2.7p, 5.4p

NO* 2.15p, 4.3yFig. 2 - Important visible and infrared transitions monitored in PHARO

10

PHARO GEOMETRY

e y

Bx , CAMERA LINEI OF SIGHT

I //

Fig. 3 - Line integration of volume emission from conical segment$at a particular wavelength, along a ray, to obtain radiance, s is thedistance between camera and burst point, B. 0 and t define thedirection from burst to camera. 0 and 0 (not shown) define the direc-tion of the camera line of sight relative to the burst point.

11

8 14M CAMERA 2 T(SEC) 0.

CONTOURS 5.IE-09 TO I.OE-04 DEC. 5.0E-01

: 4S.06

30.04

15.05

.021

4 4

4 " . 4

"60.00 -44.99 -9.91 -14.97 .03 15.05 0.04 OAS .0

Fig. 4 - Radiance in the 8-14 p band (watts/cm 2 ster) from a highaltitude burst %1. see after burst. Abscissa and ordinate in degrees.

12

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

0 14M CAMERA 2 T(SEC) 2.OOOE 01

CONTOURS S.IE-11 TO t.OE-06 DEC. S.OE-O1

45.05

.02

d 4

-29.98~

-60.00 -44.99 -29.91 -14.97 .02 15.05 50.04 OAS0 60.04

Fig. 5 - Radiance in the 8-14 pband (watts/cm2ster) from a highaltitude burst " 20. sec after burst. Abscissa and ordinate in degrees.

13

8 14M4 CAMERA 2 T(SMC .OO 01CONTOURS S.IE-12 Ta I.OE-07 DEC. 5.OE-01

40.14

41.04

0.04

-'4.94

-4 4.99

-60.00 -44,99 -29.98 -14.97 .01 15.01 50.04 41.01 40.04

Fig. 6 - Radiance in the 8-14 p band (wattslcm2ster) from a highaltitude burst ' 60. see after burst. Abscissa and ordinate in degrees.

14

8 14M CAMERA 2 T(SEC) 1.000E 02CONTOURS S.IE-12 TO 1.OE-07 DEC. 5.OE-O1

60.14

4.01

10.04

Is.814

.03

-t4.97

of*g -44.99 -29.91 -14.97 .At I1.61 0.644041f 46.0 4

Fig. 7 - Radiance in the 8-14 u band (Watts/crn2 ster) from a highaltitude burst 100. sec after burst. Abscissa and ordinate in degrees.

15

8 14M CAMERA 2 T(SEC) 1.400E 02

CONTOURS S.IE-13 TO I.OE-08 DEC. S.OE-01

60.84

4 4

4

-40.00 -44.99 .a9.U -1.9102 I.01 10.04 4S.IS 60.04

16

48 KM 50 KM

5.6 (-8)

STATION KI STATION KI

60 SECONDS 57-58 SECONDS

WATTS/CM 2 SR (3800 - 6800 A) WATTS/CM2SR (3800 - 6500 A)Fig. 9 - PHARO radiance contour predictions compared withmeasured contours for a high altitude burst in the visible spectrum at

60. sec.

17

REFERENCES

1. Hyman, E., A.W. Ali and T.P. Coffey, "PHARO I - Phenomenology

and Radiation Output Code," DNA Second Conference of Appli-

cations of Chemistry to Nuclear Weapons Effects, IDA,

Arlington, September, 1972.

2. Hyman, E., P. Julienne and J. Davis, "Departure from LTE in

an Oxygen Plasma, II. Collisional Model," DNA Atmospheric

Effects Symposium, San Diego, April, 1973 and NRL Memorandum

Report 2740, March 1974.

3. Ali, A.W., "Optical and Infrared Emission from Disturbed E

and F Layers, Part 1: Theoretical Considerations," NRL

Memorandum Report 2404, April, 1972.

4. Davis, J. and J. Lewis, "Photoionization Cross Sections and

Recombination Coefficients for Oxygen and Nitrogen Plasmas,"

NRL Memorandum Report 2538, December, 1972.

18

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