Appendix 

I have tried to update to reflect a “Past Mission”, instead of a “Future Mission”

Needed: 	Summary of On-Orbit Operation
		Some LBL results?

Table of Contents
1. INSTRUMENT PURPOSE
2. EXPERIMENT OBJECTIVES
	2.1 Primary
	2.2 Secondary
3. MEASUREMENT TECHNIQUE AND INSTRUMENT DESCRIPTION
	3.1 General
	3.2 Telescope Geometry
	3.3 Detector Thresholds
	3.4 Logic and Ground Commands
	3.5 Telemetry
	3.6 Isotope and Energy Ranges
4. OPERATION IN MAGNETOSPHERE
5. SCIENCE CALIBRATIONS
6. STATUS AND PLANS
7. REFERENCES
TABLES 1 THRU 7
FIGURES 1 THRU 11

1. INSTRUMENT PURPOSE
	The purpose of the ONR-604 instrument was: a) to obtain new data on the isotopic and elemental composition of high energy, heavy charged particles which assist in understanding the high energy conversion processes in solar flares, b) to discover observable solar conditions leading up to the explosive phase of a solar flare, and c) to determine the high energy, heavy ion fluxes in selected regions of the magnetosphere in order to determine the importance of this component as a source of radiation damage and "soft upsets" in electronic devices.

2. EXPERIMENT OBJECTIVES

	2.1 Primary
	The primary objectives of this experiment were: (1) to study solar flare energy conversion and high energy nuclear particle accelerator mechanisms on the sun, (2) to monitor solar flare particle flux levels, (3) to measure the high energy galactic cosmic ray distribution as a "template" for solar flare observations, and (4) to determine the composition of any heavy ions observed in the magnetosphere.

	2.2 Secondary
	Secondary objectives include: (1) examination of constraints imposed on stellar nucleosynthesis models and their application to the sun; (2) determination of parameters for models or origin, acceleration, and propagation of charged particles into the earth's magnetosphere; (3) study of the access of solar particles into the earth's magnetosphere; (4) determination of trapping times for particles observed in the magnetosphere; and (5) space flight verification of the new technology embodied in the solid-state position sensing detectors. (Ref. 1C)

3. MEASUREMENT TECHNIQUE AND INSTRUMENT DESCRIPTION

	3.1 General
	Figure 1 shows a schematic cross-section of the charged particle telescope. In order to achieve the high mass resolution needed for isotopic separation of heavy ions, it was necessary to measure the trajectory of each charged particle entering the acceptance cone of the telescope, both to measure the pathlengths in the detectors and to determine the arrival direction of the particles from space. This was done using position-sensing detectors (PSD's) developed and fabricated at the University and shown in Figure 2. As shown on the figure, these detectors use a series of gold strips on the top surface of the detector to collect the charge liberated by the passage of the particle. This signal was read out through a resistive divider network and compared to the total signal from the detector, obtained from the charge collected on the back surface contact, to obtain one coordinate of the point of incidence of the particle. Two sets of PSD's (three per set for redundancy) were used in the telescope to obtain the trajectory of the particle. Calibration of this system with accelerator particles shows that the position can be measured to better than 0.1 mm and the angle of incidence of the particle determined to better than 1°.
	The charge and mass of each particle was determined by the well-known technique of multiple dE/dx vs residual energy using the measurements provided by the stack of 5 mm thick lithium drifted silicon detectors, corrected for the trajectory of the individual particle. For this analysis we require the particle to come to rest within the instrument, which determines the energy range over which each type of particle can be studied. As shown in Figure 1, the entire stack was surrounded by a scintillator guard counter in anti-coincidence to eliminate out-of-geometry events and to eliminate particles that exit from the side of the apparatus. Further, a ground-commandable operations mode was provided for the detailed analysis of proton and alpha particle flux levels. Thus, complete measurements were obtained for any solar flare observed.
	In order to separate isotopes for elements as heavy as Nickel, it was necessary to measure the dE/dx and residual energy signals to a precision level of O.1%. This stringent constraint has been met by developing exceptionally linear, highly stable electronic circuits to analyze the signals from each detector. Each analysis chain was individually calibrated, and the entire instrument performance has been evaluated using high energy heavy ion beams obtained from the LBL Bevalac accelerator.
	The performance of each analysis chain was monitored during flight by an on-board calibrator which sends a sequence of 2000 pulses spanning the entire range of signal sizes. Furthermore, in-flight calibration and normalization was provided by measurement of galactic cosmic ray events. These high precision measurements require that a) the temperature remain stable and constant to within ~3°C over the orbit and b) consequently the instrument power was on during 100% of the orbital period.
	Because the anti-coincidence scintillator guard counter subtends a large solid angle and was used in the instrument logic, it must be shielded from the high counting rates induced by electrons trapped in the magnetosphere. The shielding is shown in Figure 3 and corresponds to complete elimination of < 4 MeV electrons by the AZ31B magnesium shield and the Tantalum collar. The lower part of the scintillator was located well within the instrument package and was surrounded on five sides by electronic modules which offer additional shielding. The backward moving particles were shielded additionally by the spacecraft structure.
	Since a three-year mission was planned, in order to protect further against accumulated radiation damage to the detectors Dl, D2 and D3 (where the average geometrical factor was 87 cm2-ster), a 3mm external Al window shield was placed over the telescope. This shield lowers the magnetospheric integrated proton and electron radiation doses for detectors Dl, D2, D3 below the tolerance threshold of these detectors while moving upwards only slightly the energy intervals for measurement of the heavy particles, which were the main objective of the experiment.
	In addition to heavy particles the instrument measured protons and alpha particles over the energy range 25-119 MeV. In quiet regions of space, a priority system insured that the heavy nuclei were analyzed in preference to protons and alphas. In regions of high background radiation, a commandable heavy particle "normal mode" was invoked. This raises the thresholds on the detectors D1 through D6 to suppress the high firing rates induced by trapped protons and electrons while still permitting the rare heavy ions to be analyzed.
	Figure 4 shows a functional block diagram of the instrument electronics. Besides providing the measurement of pulse height analysis, the instrument had internal accumulators that counted and stored both single detector counting rates and coincidence counting rates, thus allowing the absolute sampling rate and the absolute flux levels to be deduced. A priority system ensured that the rare events were preferentially analyzed and stored. A ground commandable operations mode was provided for the detailed analysis of proton and alpha particle flux levels.
	Table 1 gives a summary of ONR-604’s vital statistics.

	3.2 Telescope Geometry
	Table 2 gives a summary of telescope geometry data relevant to the measurement of fluxes and the analysis of pulse heights of energetic charged particles. The Table gives Dl and the given detector (to top and bottom), the relevant geometrical factors through the window, and the proton energy needed at 0° to penetrate the detectors (see Figure 1).
	The highest quality isotopic data was obtained for particles stopping in K2 and below. However, the telescope can also measure particles:
	a) stopping in K1
	b) stopping in D2 - D6
	c) penetrating K8
	For a) and b) it was necessary to use the signal from the E contact of the PSDs to provide energy loss information. For events stopping in D2 or D3, the pathlength uncertainty was given by sec Q where Q was the maximum angle through the window (69° for D2 which gives a spread of a factor of 2.8). Thus, D1D2D3 analysis can separate protons and helium, but no heavier elements. For particles stopping in D4, the sec Q spread was reduced to a factor of 1.44.
	For particles stopping in D5 - K1, there was trajectory information available and elemental separation was limited only by the quality of the E signals from the PSDs -- in fact there was even some isotopic capability for these events. Finally, the chemical composition of events penetrating the entire stack can be studied over a limited energy interval.

	3.3 Detector Thresholds
	Table 3 lists the ONR-604 detector thresholds in "normal mode" and in "proton mode". In "normal mode" the "proton mode" thresholds of detectors Dl
through D6 were increased by a factor 5.8 and as a consequence the instrument becomes insensitive to protons.

	3.4 Logic and Ground Commands
	Table 4 describes the rate logic and the incident energy intervals for representative energetic particles. Table 5 gives the logic for the pulse height analysis gate control and analysis priorities, and the ground commands and their action on the logic.

	3 .5 Telemetry
	Figure 5 shows the CRRES minor telemetry frame with the location of the 12 8-bit words allocated to ONR-604. 360-bit blocks from ONR-604 were loaded into a first-in first-out (FIFO) register. The contents of FIFO were read out into the downlink in 8-bit words in 4 minor frames or 0.512 sec (0.128 sec/frame).
	The number of bits read out into the downlink was 384 (360 bits of instrument data plus 24 fill bits). The overall bit rate of ONR-604 was 750 bits/second.

	3.6 Isotope and Energy Ranges
	Figure 6 shows the incident kinetic energy intervals in the telescope corresponding to detector penetration ranges (essentially equal to the energies triggering the low thresholds in "proton mode") for isotopes H1 through Ni59. For every isotope the inclined lines connect the points for zero incidence angle (bottom) with the points at 30° incidence angle (top).

4. OPERATION IN THE MAGNETOSPHERE
	Table 6 gives the coverage time for the measurement of various isotopes. This coverage time was the fraction of the CRRES orbital period of the final orbit with Stormer cutoff within or below the ONR-604 sensitive energy range.
The coverage time is given as a function of the index of the particle differential energy spectra assumed to be a power law in energy (i.e. µ E+g).
	Table 7 gives an estimate of the expected counting rates in proton mode for an incident high intensity hard spectrum of trapped protons like the P-4
spectrum present in the South Atlantic Anomaly (M.J. Teague et al., NSSDC Report 72-11, November 1982 and 74-03, April 1974.)
.
5. SCIENCE CALIBRATIONS (PRE-FLIGHT)
	The ONR-604 instrument was calibrated in July 1977, April 1978 and July 1979 with beams of C, Ne, Ar and Fe particles (with energies such that the particles stopped in the telescope) accelerated at the Bevatron/Bevalac of the Lawrence Radiation Laboratory.
	A final calibration of ONR-604 was carried out at this facility before the initial instrument delivery for integration in 1985. This calibration included proton and helium nuclei.
	Because of the long postponement of the CRRES mission after the Challenger accident, a second “final” calibration was performed at the same facility in February 1989, after replacement of most of ONR-604’s detectors.
	After integration with the XXX spacecraft, in addition to test procedures, there was a m-meson calibration at: a) the integration site and b) at the Kennedy Space Center. Each calibration required more than 48 hours of running time. A typical m-meson calibration obtained with a telescope similar to ONR-604 is shown in Figure 7.

6. ON-ORBIT OPERATION
				TBD
7. REFERENCES (Needs to be redone, or else folded into non-appendix reference)
A. 
1A. "The Composition, Propagation and Acceleration of Energetic 	Solar Particles: A Review of United States Research 1979-1982", 	R.E. McGuire, , 21, 305, 1983.
2A. "Spacecraft Measurements of the Elemental and Isotopic 		Composition of Solar Energetic Particles", R.A. Mewaldt , ed. R.0. Pepin, J.A. Eddy and R.B. Merril, pp. 81-101, 1980.
3A. "Elemental and Isotopic Composition of the Galactic Cosmic Rays", J.A. Simpson, , 33, 33, 1983.

B. 
1B."Cosmic Ray Effects on Microelectronics, Part I: The Near-Earth Particle Environment" J.H. Adams Jr., R. Silberberg and C.H. 	Tsao, 
2B. "The Isotopic and Elemental Abundances of Neon Nuclei 	Accelerated in Solar Flares", W.F. Dietrich and J.A. Simpson, , L91, 1979.
3B."The Isotopic Composition of Magnesium Nuclei in Solar Flares", W.F. Dietrich and J.A. Simpson, , , L41, 1981.
4B."Super Enrichments of Fe-Group Nuclei in Solar Flares and their Association with large 3He Enrichments", J.D. Anglin, W.F. 	Dietrich and J.A. Simpson, Proc. 15th Int. Cosmic Ray Conf., Plovdiv, , 43, 1977.

C. 
1C. "A Large Area Circular Position Sensitive Si Detector", J.E. 	Lamport, G.M. Mason, M.A. Perkins and A.J. Tuzzolino, Nuclear 	Instr. and Methods, , 71, 1976.
2C. "ONR-604 Annex" of February 1983 (unpublished).

TABLE 1

ONR-604 VITAL STATISTICS
______________________________________________________________________________

Weight	32 (+1, -0) lbs.

Volume: Package & Telescope	12.0 x 17.0 x 11.75 in.

Viewing: 	a) Direction	Telescope Axis Normal to S/C Spin Axis
 	b) Cone (Unobstructed)	93° (Full Angle)

Geometrical Factor	90 to 3 cm2 ster

Power	6.0 Watts, Average; <8.0 Watts, Peak

Bit Rate	360 Bits/Readout (0.512 sec readout)
	750 b/s at Interface

Operating Duty Cycle	100%

Ground Commands	2 Power, 12 Mode (Command Word)

Calibration and Testing	Through Test Connector -

(Pre-Launch)/(Post-Launch)	IFC Source - Onboard - IFC/Data*

Environmental: 	Temperature	-10°C to ~10°C with < 3°C 
		Variation/Orbit
 	Chemical	Not To Be Exposed to Solvent
		(Because of Solid-State
		Detectors)
 	Humidity	Relative Humidity < 55%:
	 	Dry Air Purging

Energy Range (Isotopes)	25-570 MeV/Nucleon

Charge Range For Isotopic Separation	Hydrogen to Nickel

Mass Resolution At Iron	s » 0.22 AMU

Science Calibration	Performed With Heavy Ion Beams
	at the Bevalac Accelerator of the
	Lawrence Berkeley Laboratory

Critical Requirements	a) Dry air purge of instrument
	 	(Ref. 2C)
	b) Standby bias applied to solid
	 state detectors when instrument
	 power was off (Ref. 2C)
* IFC = Inflight Calibrator

TABLE 2

Detector qm from D1 to: Geometrical Factor (cm2-ster)	Ep (MeV)
					to penetrate to
	Top	Bottom	Top	Bottom	bottom of detector

Window	-	-	379.4	379.4	-
Dl	-	-	95.0	93.6	28.3
D2	87.10	-	87.9	86.6	31.7
D3	84.1	-	81.3	80.0	35.1
D4	50.0	-	16.2	16.3	36.6
D5	47.9	-	14.9	14.9	38.5
D6	46.0	-	13.6	13.7	40.0
K1	41.3	39.2	8.2	7.5	52.0
K2	38.6	36.7	7.0	6.4	62.1
K3	36.1	34.4	6.0	5.5	71.2
K4	33.9	32.4	5.2	4.8	79.3
K5	32.0	30.6	4.4	4.1	87.0
K6	30.2	28.9	3.9	3.6	94.0
K7	28.6	27.4	3.4	3.2	100.8
K8	27.1	26.1	3.0	2.8	107.5
A	-	-	3.0	2.8	108.5
______________________________________________________________________________

Note the large geometrical factor for events in D1, D2 and D3.

TABLE 3
ONR-604 DETECTOR THRESHOLDS (MeV)
______________________________________________________________________________

	Detector	Normal Mode	Proton Mode
		Dl		4.45		0.77
		D2		4.53	 0.78
		D3		4.55	 0.78
		D4		1.65	 0.28
		D5		1.71	 0.29
		D6		1.69	 0.29

Normal Mode and Proton Mode
		Low	Medium	 High
	Kl	0.693	36.9	 1205
	K2	0.647	37.9	 1082
	K3	0.653	-	 1199
	K4	0.654	-	 1197
	K5	0.668	-	 1197
	K6	0.649	-	 1201
	K7	0.680	-	 1209
	K8	0.664	-	 1194
	A	0.214	-		-

 TABLE 4
____________________________________________________________________________
Rate No.		Detector	Rate Logic	Energy Interval		Particle			Interval			of Rate In		Defining
							Proton Mode	Rate Interval
				 			 (MeV)
____________________________________________________________________________
 ____
	1	 D1		D1D2D3	(S)a	24.8- 44.5	Protons
 ____
	2	 D2		D1D2D3D4	(S)a	28.3- 48.2	"
 ____
	3	 D4		D13D4D5D6	(S)a	35.1- 43.9	"
 ____
	4	 D5		D13D5D6K1	(S)a	36.6- 45.5	"
 ___
	5	 K1		D13K1K2K3	(S)a	40.0- 59.4	"
 __
	6	 K2		D13K1K2K3	(S)a	52.0- 70.6	"
 _
	7	 K3		D13K1K3K4	(S)a	62.1- 79.9	"
 __
	8	 K4		D13K1K4K5	(S)a	71.2- 88.5	"
 __
	9	 K5		D13K1K5K6	(S)a	79.3- 96.5	"
 __
	10	 K6		D13K1K6K7	(S)a	87.0-103.5	"
 _
	11	 K7K8		D13K1K7A	(S)a	94.0-116.9	"
 
	12	 A		D13K1K8A	(S)a	107.5-275	"
 
	13	 P3		D13S+D13 (K1+K2)24.8-275	"
 _
	14	 P2		P3 (K1M+K2M)A	42-105	He4

	15	 P1		P3 (K1H+K2H+
				 K3H+K4H+
				 K5H+K6H+K8H)127-352 	Mg24

	16	Single Detector Rates
______________________________________________________________________________

Notes: M Medium Threshold; H High Threshold
 (Low Threshold was indicated by detector symbol not followed by M or H
	 S Scintillation guard counter.
	 (S)a S term included every alternate readout.
 P3 Pulse Height Analysis Gate Control (Priority No. 3 or low
			priority).
	 P2 Priority No. 2 or Medium Priority
	 P1 Priority No. 1 or High Priority

TABLE 5

ONR-604 PULSE HEIGHT ANALYSIS GATE CONTROL AND PRIORITY LOGIC,
AND GROUND COMMAND

______________________________________________________________________________
 _
Gate Control GC = D1D2D3S + D1D2D3 (K1 + K2)

Priority 3 (Low Priority) P3 = GC
 _
Priority 2 (Medium Priority) P2 = GC (K1M + K2M) A

Priority 1 (High Priority) P1 = GC (K1H + K2H + K3H + K4H + K5H + K6H +
 K7H + K8H

Ground Commands 16 Bit Serial Digital Command Word

	Bit No. (In Order Received)		Function

		1	Start Calibrate Sequence

		2	Override Calibrate

		3	Disable Dl

		4	Disable D2

		5	Disable D3

		6	Disable K1

		7	Disable K2

		8	Disable A

		9	Disable S

		10	Inhibit P2

		11	Inhibit P3

		12	Set Proton Mode

		13-16	Spares

TABLE 6

ONR-604 ISOTOPE COVERAGE TIME
(Fraction of Orbital Period)

_____________________________________________________________________________

	Isotope	Spectral Power-Law Indices ( )
		-6	-3	+1

 	He3	0.23	0.31	0.47

	He4	0.47	0.51	0.60

 	O16	0.47	0.51	0.60

 	O18	0.53	0.56	0.64

 	Ne20	0.47	0.51	0.60

 	Ne22	0.52	0.55	0.63

 	Ar36	0.47	0.51	0.60

 	Ar40	0.52	0.56	0.64

 	Fe54	0.49	0.53	0.62

	Fe56	0.51	0.54	0.63

TABLE 7

ONR-604 TRAPPED PROTON COUNTING RATES
(Given For a P-4 Trapped Proton Spectrum)

______________________________________________________________________________

Rate No. Detector Interval Proton Energy Range Counts/Second
 (MeV)
______________________________________________________________________________

	1	D1	25- 45	1.8 x 105

	2	D2	28- 48	1.4 x 104

	3	D4	35- 44	1300

	4	D5	37- 46	860

	5	K1	40- 59	1000

	6	K2	52- 71	500

	7	K3	62- 80	270

	8	K4	71- 89	270

	9	K5	79- 97	240

	10	K6	87-104	100

	11	K7K8	94-117	200

	12	A	108-275	900

	13	P3 Logic Normalization Rate

	14	P2 Logic Normalization Rate

	15	P1 Logic Normalization Rate

	16	Subcommutated Single Rates