|
PPS and Protons are very similar, but each
model has its own advantages and disadvantages. The primary
limitation in both models is that they do not predict the flux of
particles accelerated by shocks far from the Sun. If such an
interplanetary shock
is present, corrections must be made to the model to provide more
accurate results. PPS
does not current provide for this correction, though Protons does. Interplanetary
MHD
codes are currently being developed to generate better SEP models with
or without the presence of an interplanetary
shock.
Protons
can be used to forecast space weather (with limited accuracy).
The sole use of flare and/or radio burst intensities to
determine SEP fluxes is probably a source of significant error. Protons also assumes that all
flares occur at the Solar Equator, which highlights the need for a
better understanding of
the spatial variation of SEP events.
The primary advantage of PPS
is its ease of use, and the availability of an "Expert Mode."
These models are currently available only through their authors.
|
|
Protons
|
PPS
|
Inputs
|
-
Type
of Data: Radio or X-Ray
-
Peak/Integrated Flux
Values
-
Radio/X-Ray Band
-
Event Start Time and Time
of Maximum Flux
-
Peak X-Ray Flare
Classification or
Magnitude, if Applicable
-
Flare Lattitude and
Longitude
- Was
there an Interplanetary Shock Within 24 Hours Prior to the Event?
|
-
Type
of Data: Radio or X-Ray
-
Peak/Integrated Flux
Values
-
Radio/X-Ray Band
-
Event Start Time and Time
of Maximum Flux
-
Peak X-Ray Flare
Classification or
Magnitude, if Applicable
-
Flare Lattitude and
Longitude
- Expert
Mode: Override Default System Parameters
|
Outputs
|
-
Maximum
Day/Night Polar Riometer Absorption and Time of Maximum
-
Maximum Dose Rate at 70,000 Feet
Above Polar Regions and Time of Maximum
-
Maximum
Dose Rate for Polar LEO Orbit Behind STS and EMU Shielding and Time of
Maximum
- When
>5, 10, and 50 MeV Particle Fluxes Exceed 10/(cm^2 s sr): Duration,
Time of Maximum Flux, and Fluence
- Differential
and Integral Proton Fluxes for Various Energy Ranges at Geosynchronous
Altitudes
|
|
