Table of Contents ECSS Model Page
Background Information Radiation sources and effects
Solar particle models

SPENVIS can run solar particle peak flux models to predict instantaneous fluxes. The models yield fluxes outside the magnetosphere, which are then corrected for magnetic shielding.

In order to run these models, a spacecraft trajectory is needed. If no trajectory has been generated yet, the orbit generator should be run first.

The input parameters and options for the solar particle peak flux models are described below. When the input form has been completed, pressing the button will start the calculation and bring up the "Results" page.

The button calls up the model selection page for consecutive runs of multiple models. This feature is available for advanced users only.

Warning: using these buttons deletes all existing output from the solar particle peak flux models and from any model that uses this output, in order to ensure consistency in the outputs.

Input parameters

Model selection

The following models for solar particle peak fluxes are available in SPENVIS:

Fluxes can be obtained for the whole ion range from H up to U.

Magnetic shielding

Solar particle fluxes are shielded by the planet's magnetic field if present. This shielding effect can be turned off to simulate the environment outside the magnetosphere.

The magnetic shielding of solar particles is lower during stormy conditions than for a quiet magnetosphere. A selection between these conditions is available only for Earth.

Interplanetary missions

Currently in SPENVIS, for interplanetary missions the solar particle peak fluxes are scaled by a factor calculated as the mean value over the mission: r-2 for r < 1AU and 1 for r > 1AU.

Results

The solar particle peak flux models produce the files listed in the table below. A description of the file formats can be brought up by clicking on their description in the table.

The report file spenvis_sepflare.html contains the input parameters and summary tables. The spectrum file spenvis_sefflare.txt contains the flux spectrum, and the spenvis_seoflare.txt file contains the attenuation factor for each orbital point and for each energy.

Output files generated by the solar particle peak flux models
File name Description
spenvis_sepflare.html Report file
spenvis_sefflare.txt Flux spectra for NEWUPSETO, MULASSIS
spenvis_seoflare.txt Attenuation factor

To generate plots, select the plot type(s), options and graphics format, and click the or button. The current page will be updated with the newly generated plot files.

The button calls up the output page for consecutive runs of multiple models. This button only appears when the solar particle peak flux models have been included in the combined model run selection. This feature is available for advanced users only.

References

Adams, J. H., Cosmic Ray Effects on Microelectronics, Part IV, NRL Memorandum Report 5901, Washington, D.C., 1986.

Tylka, A.J., Dietrich, W.F. and Boberg, P.R., Probability Distributions of High-Energy Solar-Heavy-Ion Fluxes from IMP-8: 1973-1996, IEEE Trans. on Nucl. Sci., 44, 2140-2149 (1997)

Xapsos, M.A., R J Walters, G P Summers, J L Barth, E G Stassinopoulos, S R Messenger, E A Burke,Characterizing solar proton energy spectra for ra-diation effects applications, IEEE Trans. on Nucl. Sci , 47, no. 6, pp 2218-2223, Dec. 2000.

Jiggens, P., Varotsou, A., Truscott, P., Heynderickx, D., Lei, F., Evans, H. & Daly, E., The Solar Accumulated and Peak Proton and Heavy Ion Radiation Environment (SAPPHIRE) Model, IEEE Transactions on Nuclear Science, Volume 65, Issue 2, 2018.


Last update: Wed, 25 Apr 2018