Ulysses Cosmic Ray and Solar Particle Investigation (COSPIN) Kiel Electron Telescope (KET) Proton, Helium, and Electron Spin-Integrated Counting Rates Data, 10 min Average Data

COSPIN-KET-RAT-10M

2021-04-27 15:38:11Z

This Data Set contains 10 min Averages of: (a) Spin-Integrated Count Rates of Protons (2.7-5.4, 5.4-23.1, 34.1-125.0, 125.0-320.0, 320.0-2100 and >2100.0 MeV), Alpha Particles (6.0-20.4, 34.2-125.0, 125.0-320.0, 320.0-2100.0 and >2100.0 MeV/n), and Electrons (2.5-7.0, 7.0-170.0 and >170.0 MeV). (b) Eight-Sectored Count Rates of Protons (5.4-23.1 MeV) and Electrons (2.5-7.0 MeV). (c) Count Rates of D10, D20, C10, C20 and A01 single Detector Sensors. The Parameter Keys in the Parameter Level Segments below are specifically relevant to the UFA accessible Versions of the Data.

Please acknowledge the COSPIN PI, R. Bruce McKibben, the KET Co-PI, Bernd Heber, and the UDS and/or NSSDC

spase://VEPO/NumericalData/Ulysses/COSPIN/KET/RATES/PT10M

spase://VSPO/NumericalData/Ulysses/COSPIN/KET/Rates/PT10M

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ZIP

Please acknowledge the COSPIN KET Co-PI, Bernd Heber, CAU Kiel

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CDF

Please acknowledge the Space Physics Data Facility at NASA/GSFC

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Open

Text

Please acknowledge the Space Physics Data Facility at NASA/GSFC

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CSV

Please acknowledge the Space Physics Data Facility at NASA/GSFC

PT10M

Time for the record

Time_PG1

Time for the record given in Year, Day of Year, Hour, Minute, Seconds and coverage in percent. The given time represents the start of the averaging interval.

PT10M

COSPIN/KET 10-Minute Average 2.7-5.4 MeV Proton Spin-Averaged Count Rates (K1)

K1

10-minute average KET spin-averaged proton count rates between 2.7 and 5.4 MeV

Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= K1 18 On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a "calibration mode" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter. Background fluxes of K1 are a combination of components, including a high RTG background rate. This channel should be used only during event times.

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COSPIN/KET 10-Minute Average 5.4-23.1 MeV Proton Count Rates in Spin Sector 1 (K21)

K21

10-minute average KET proton count rates in spin sector 1 (of 8) between 5.4 and 23.1 MeV

Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= K21-K28 120 On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a "calibration mode" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter.

PT10M

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1000000

-707

COSPIN/KET 10-Minute Average 5.4-23.1 MeV Proton Count Rates in Spin Sector 2 (K22)

K22

10-minute average KET proton count rates in spin sector 2 (of 8) between 5.4 and 23.1 MeV

Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= K21-K28 120 On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a "calibration mode" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter.

PT10M

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1000000

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COSPIN/KET 10-Minute Average 5.4-23.1 MeV Proton Count Rates in Spin Sector 3 (K23)

K23

10-minute average KET proton count rates in spin sector 3 (of 8) between 5.4 and 23.1 MeV

Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= K21-K28 120 On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a "calibration mode" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter.

PT10M

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0.0

1000000

-707

COSPIN/KET 10-Minute Average 5.4-23.1 MeV Proton Count Rates in Spin Sector 4 (K24)

K24

10-minute average KET proton count rates in spin sector 4 (of 8) between 5.4 and 23.1 MeV

Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= K21-K28 120 On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a "calibration mode" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter.

PT10M

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0.0

1000000

-707

COSPIN/KET 10-Minute Average 5.4-23.1 MeV Proton Count Rates in Spin Sector 5 (K25)

K25

10-minute average KET proton count rates in spin sector 5 (of 8) between 5.4 and 23.1 MeV

Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= K21-K28 120 On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a "calibration mode" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter.

PT10M

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0.0

1000000

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COSPIN/KET 10-Minute Average 5.4-23.1 MeV Proton Count Rates in Spin Sector 6 (K26)

K26

10-minute average KET proton count rates in spin sector 6 (of 8) between 5.4 and 23.1 MeV

Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= K21-K28 120 On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a "calibration mode" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter.

PT10M

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0.0

1000000

-707

COSPIN/KET 10-Minute Average 5.4-23.1 MeV Proton Count Rates in Spin Sector 7 (K27)

K27

10-minute average KET proton count rates in spin sector 7 (of 8) between 5.4 and 23.1 MeV

Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= K21-K28 120 On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a "calibration mode" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter.

PT10M

s^-1

0.0

1000000

-707

COSPIN/KET 10-Minute Average 5.4-23.1 MeV Proton Count Rates in Spin Sector 8 (K28)

K28

10-minute average KET proton count rates in spin sector 8 (of 8) between 5.4 and 23.1 MeV

Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= K21-K28 120 On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a "calibration mode" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter.

PT10M

s^-1

0.0

1000000

-707

COSPIN/KET 10-Minute Average 5.4-23.1 MeV Proton Spin-Averaged Count Rates (P4)

P4

10-minute average KET spin-averaged proton count rates between 5.4 and 23.1 MeV

Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= P4 120 On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a "calibration mode" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter.

PT10M

s^-1

0.0

1000000

-707

COSPIN/KET 10-Minute Average 34.1-125.0 MeV Proton Spin-Averaged Count Rates (K3)

K3

10-minute average KET spin-averaged proton count rates between 34.1 and 125.0 MeV

Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= K3 70.0 On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a "calibration mode" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter.

PT10M

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0.0

1000000

-707

COSPIN/KET 10-Minute Average 125.0-320.0 MeV Proton Spin-Averaged Count Rates (K34)

K34

10-minute average KET spin-averaged proton count rates between 125.0 and 320.0 MeV

Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= K34 152.0 On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a "calibration mode" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter.

PT10M

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0.0

1000000

-707

COSPIN/KET 10-Minute Average 320.0-2100.0 MeV Proton Spin-Averaged Count Rates (K12)

K12

10-minute average KET spin-averaged proton count rates between 320.0 and 2100.0 MeV

Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= K12 3300.0 On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a "calibration mode" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter.

PT10M

s^-1

0.0

1000000

-707

COSPIN/KET 10-Minute Average >2100.0 MeV Proton Spin-Averaged Count Rates (K10)

K0

10-minute average KET spin-averaged proton count rates >2100.0 MeV

Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= K10 N/A On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a "calibration mode" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter.

PT10M

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0.0

1000000

-707

COSPIN/KET 10-Minute Average 6.0-20.4 MeV/n Helium Spin-Averaged Count Rates (K2)

K2

10-minute average KET spin-averaged helium count rates between 6.0 and 20.4 MeV/n

Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= K2 120 On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a "calibration mode" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter.

PT10M

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0.0

1000000

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COSPIN/KET 10-Minute Average 34.2-125.0 MeV/n Helium Spin-Averaged Count Rates (K33)

K33

10-minute average KET spin-averaged helium count rates between 34.2 and 125.0 MeV/n

Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= K33 70.0 On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a "calibration mode" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter.

PT10M

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0.0

1000000

-707

COSPIN/KET 10-Minute Average 125.0-320.0 MeV/n Helium Spin-Averaged Count Rates (K29)

K29

10-minute average KET spin-averaged helium count rates between 125.0 and 320.0 MeV/n

Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= K29 88.0 On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a "calibration mode" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter.

PT10M

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0.0

1000000

-707

COSPIN/KET 10-Minute Average 320.0-2100.0 MeV/n Helium Spin-Averaged Count Rates (K31)

K31

10-minute average KET spin-averaged helium count rates between 320.0 and 2100.0 MeV/n

Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= K31 3200.0 On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a "calibration mode" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter.

PT10M

s^-1

0.0

1000000

-707

COSPIN/KET 10-Minute Average >2100.0 MeV/n Helium Spin-Averaged Count Rates (K30)

K30

10-minute average KET spin-averaged helium count rates >2100.0 MeV/n

Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= K30 N/A On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a "calibration mode" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter.

PT10M

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0.0

1000000

-707

COSPIN/KET 10-Minute Average 2.5-7.0 MeV Electron Count Rates in Spin Sector 1 (K13)

K13

10-minute average KET electron count rates in spin sector 1 (of 8) between 2.5 and 7.0 MeV

Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= K13-K20 N/A On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a "calibration mode" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter.

PT10M

s^-1

0.0

1000000

-707

COSPIN/KET 10-Minute Average 2.5-7.0 MeV Electron Count Rates in Spin Sector 2 (K14)

K14

10-minute average KET electron count rates in spin sector 2 (of 8) between 2.5 and 7.0 MeV

Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= K13-K20 N/A On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a "calibration mode" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter.

PT10M

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0.0

1000000

-707

COSPIN/KET 10-Minute Average 2.5-7.0 MeV Electron Count Rates in Spin Sector 3 (K15)

K15

10-minute average KET electron count rates in spin sector 3 (of 8) between 2.5 and 7.0 MeV

Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= K13-K20 N/A On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a "calibration mode" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter.

PT10M

s^-1

0.0

1000000

-707

COSPIN/KET 10-Minute Average 2.5-7.0 MeV Electron Count Rates in Spin Sector 4 (K16)

K16

10-minute average KET electron count rates in spin sector 4 (of 8) between 2.5 and 7.0 MeV

Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= K13-K20 N/A On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a "calibration mode" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter.

PT10M

s^-1

0.0

1000000

-707

COSPIN/KET 10-Minute Average 2.5-7.0 MeV Electron Count Rates in Spin Sector 5 (K17)

K17

10-minute average KET electron count rates in spin sector 5 (of 8) between 2.5 and 7.0 MeV

Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= K13-K20 N/A On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a "calibration mode" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter.

PT10M

s^-1

0.0

1000000

-707

COSPIN/KET 10-Minute Average 2.5-7.0 MeV Electron Count Rates in Spin Sector 6 (K18)

K18

10-minute average KET electron count rates in spin sector 6 (of 8) between 2.5 and 7.0 MeV

Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= K13-K20 N/A On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a "calibration mode" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter.

PT10M

s^-1

0.0

1000000

-707

COSPIN/KET 10-Minute Average 2.5-7.0 MeV Electron Count Rates in Spin Sector 7 (K19)

K19

10-minute average KET electron count rates in spin sector 7 (of 8) between 2.5 and 7.0 MeV

Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= K13-K20 N/A On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a "calibration mode" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter.

PT10M

s^-1

0.0

1000000

-707

COSPIN/KET 10-Minute Average 2.5-7.0 MeV Electron Count Rates in Spin Sector 8 (K20)

K20

10-minute average KET electron count rates in spin sector 8 (of 8) between 2.5 and 7.0 MeV

Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= K13-K20 N/A On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a "calibration mode" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter.

PT10M

s^-1

0.0

1000000

-707

COSPIN/KET 10-Minute Average 2.5-7.0 MeV Electron Spin-Averaged Count Rates (E4)

E4

10-minute average KET spin-averaged electron count rates between 2.5 and 7.0 MeV

Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= E4 N/A On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a "calibration mode" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter.

PT10M

s^-1

0.0

1000000

-707

COSPIN/KET 10-Minute Average 7.0-170.0 MeV Electron Spin-Averaged Count Rates (K11)

K11

10-minute average KET spin-averaged electron count rates between 7.0 and 170.0 MeV

Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= K11 N/A On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a "calibration mode" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter.

PT10M

s^-1

0.0

1000000

-707

COSPIN/KET 10-Minute Average >170.0 MeV Electron Spin-Averaged Count Rates (K32)

K32

10-minute average KET spin-averaged electron count rates >170.0 MeV

Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= K32 N/A On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a "calibration mode" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter.

PT10M

s^-1

0.0

1000000

-707

COSPIN/KET 10-Minute Average D10 Detector Counting Rate (D10)

D10

10-minute average KET D10 detector counting rate

Rate channel D10 includes all particles depositing energy greater than the minimum discriminator level.

PT10M

s^-1

0.0

1000000

-707

COSPIN/KET 10-Minute Average D20 Detector Counting Rate (D20)

D20

10-minute average KET D20 detector counting rate

Rate channel D20 includes all particles depositing energy greater than the minimum discriminator level.

PT10M

s^-1

0.0

1000000

-707

COSPIN/KET 10-Minute Average C10 Detector Counting Rate (D10)

C10

10-minute average KET C10 detector counting rate

Rate channel C10 includes all particles depositing energy greater than the minimum discriminator level.

PT10M

s^-1

0.0

1000000

-707

COSPIN/KET 10-Minute Average C20 Detector Counting Rate (D10)

C20

10-minute average KET C20 detector counting rate

Rate channel C20 includes all particles depositing energy greater than the minimum discriminator level.

PT10M

s^-1

0.0

1000000

-707

COSPIN/KET 10-Minute Average A01 Detector Counting Rate (A01)

A01

10-minute average KET A01 detector counting rate

Rate channel A01 includes all particles depositing energy greater than the minimum discriminator level.

PT10M

s^-1

0.0

1000000

-707