Summary: The difference in the V1 and V2 high energy counting rates appears to be real.

When plotted vs time, the V1 and V2 high energy proton rates are close to each other from 1977 to mid 1981, then again from late 1982 to early 1983. Then V2's rate increases faster than V1's and remains higher than V1's rate until the V1's crossing in 2012. When plotted vs radial distance, the two rates were close until about 9AU, around the Saturn encounter, then they diverge as V2's rate increases sharply. V2's rate started decreasing around 23AU and dipped below V1's rate around 32AU, after the V2 Neptune encounter. V2's rate increased above V1's rate by 40AU but gaps in the data make it hard to determine when. When plotted against solar ecliptic latitude, the V2 rates generally decrease from -36 deg to -3 deg. The V1 rates are fairly flat from +3 deg to +22 deg and rise slowly until roughly +32deg where there is a sharp decline followed by a steep rise.

The trends in our V1 and V2 high energy proton rates are similar to the trends in the V1 and V2 CRS Penetrating High Gain rates. Our V1 H > 211 MeV rate is suppressed when compared to the corresponding CRS rate starting around 55AU (1994) Our V2 H > 213 MeV rate is suppressed compared to the corresponding CRS rate starting around 80AU (late 2006).

V1's SAR rate is noisy, getting slightly better after 2010. V2's ALAR rate failed on 9/15/1986

Misc. notes: Our high energetic proton rates from voflux match the Fund. Tech. P31 rates well. The energetic proton rates have fewer outliers after cruise5a begins. Cruise-5a telemetry mode begins on 8/8/1990 (d220) for V1, and 6/1/1990 (d152) for V2. Plots of P31 from ftec and our CH31 rate in 1997 when both go to 0 for a few days and in 2005 show that the ftec data align with our data with no shift in time required.

When plotted vs time, the V1 and V2 high energy proton rates are close to each other from 1977 to mid 1981, then again from late 1982 to early 1983. Then V2's rate increases faster than V1's and remains higher than V1's rate until the V1's crossing in 2012. When plotted vs radial distance, the two rates were close until about 9AU, around the Saturn encounter, then they diverge as V2's rate increases sharply. V2's rate started decreasing around 23AU and dipped below V1's rate around 32AU, after the V2 Neptune encounter. V2's rate increased above V1's rate by 40AU but gaps in the data make it hard to determine when. When plotted against solar ecliptic latitude, the V2 rates generally decrease from -36 deg to -3 deg. The V1 rates are fairly flat from +3 deg to +22 deg and rise slowly until roughly +32deg where there is a sharp decline followed by a steep rise.

The trends in our V1 and V2 high energy proton rates are similar to the trends in the V1 and V2 CRS Penetrating High Gain rates. Our V1 H > 211 MeV rate is suppressed when compared to the corresponding CRS rate starting around 55AU (1994) Our V2 H > 213 MeV rate is suppressed compared to the corresponding CRS rate starting around 80AU (late 2006).

V1's SAR rate is noisy, getting slightly better after 2010. V2's ALAR rate failed on 9/15/1986

Misc. notes: Our high energetic proton rates from voflux match the Fund. Tech. P31 rates well. The energetic proton rates have fewer outliers after cruise5a begins. Cruise-5a telemetry mode begins on 8/8/1990 (d220) for V1, and 6/1/1990 (d152) for V2. Plots of P31 from ftec and our CH31 rate in 1997 when both go to 0 for a few days and in 2005 show that the ftec data align with our data with no shift in time required.