1. SEPEM ODI D.Heynderickx DH Consultancy BVBA, Leuven, Belgium
12/11/2018
Final Presentation Day, ESTEC, The Netherlands
D.Heynderickx
DH Consultancy BVBA, Leuven, Belgium
E. De Donder, N. Messios
Royal Belgian Institute of Space Aeronomy, Ukkel, Belgium

2. Project overview Contract No.: 4000115930/15/NL/HK
Funding programme: Engineering Support Tools (EST)
Contract value: €35,000 CCN
Consortium
DH Consultancy, Belgium (D. Heynderickx, team prime)
Royal Belgian Institute for Space Aeronomy (E. De Donder, N. Messios)
ESA Technical Officer: P. Jiggens (TEC-EES)
12/11/2018
Final Presentation Day, ESTEC, The Netherlands

3. Objectives
Upgrade of the SEPEM system (ESA Contract No 20162/06/NL/JD)
Replace the current spacecraft data database by an ODI instance
Update the H reference dataset
Include updates to heliospheric model extrapolation based on updates to SOLPENCO-2 from a parallel contract (SOL2UP /15/NL/HK) performed by University of Barcelona
Improve the web page layout
Improve the quality of the graphical outputs
Perform validation of new model outputs
Integrate system updates from Energetic Solar Heavy Ion Environment Modelling (ESHIEM) parallel contract ( /12/NL/AK)
Integration in the ESA SSA Space Weather portal
12/11/2018
Final Presentation Day, ESTEC, The Netherlands

4. The SEPEM system SEPEM: Solar Energetic Particle Environment Modelling
Database of H, He and heavy ion datasets
Raw data
Cleaned data
Cross calibrated data (H and He reference datasets)
Abundance ratio tables to scale He to heavy ion fluxes
Treatment of magnetospheric shielding
Calculation of radiation effect quantities
TID, TNID, SEU rates, spacecraft shielded flux
Mulassis for H, IRONSSIS for He and heavy ions
Creation of event lists
Implementation of statistical models
Time above threshold, event duration
Probability curves of total mission and worst event quantities
Error propagation
Heliospheric H models (distance dependent)
12/11/2018
Final Presentation Day, ESTEC, The Netherlands

5. SEPEM databases
SEPEM used a single MySQL database to store spacecraft data as well as user account information and user generated content (event lists, response functions, model runs, …)
Spacecraft data are now stored in a separate database, an ODI instance (see later presentation)
New, extended and consistent metadata
Consistent variable naming, e.g. FPDO for differential omnidirectional proton flux (COSPAR/PRBEM standard)
Make use of existing ODI download and storage mechanisms
Streamlined procedure for adding new datasets and updating existing ones
Harmonisation with other ESA tools (e.g. SEDAT)
Transparent to the user
12/11/2018
Final Presentation Day, ESTEC, The Netherlands

6. SEPEM datasets IMP-8 datasets: GME, CPME, CRNC
GOES/SEM/EPS H and He datasets (1974–2017)
Original (uncorrected 5 min) data
Cleaned data (removal of spikes, gap filling)
SEPCALIB cross calibration with IMP-8/GME H and He datasets -> contiguous reference H and He datasets (background correction)
ACE datasets: SIS, ULEIS, SEPICA
Other datasets
HELIOS-A,B/E6/E7
SOHO/ERNE H, He, ions (processed in EC FP7 SEPServer project)
Wind/EPACT/LEMT ion data
Kp index (used with geomagnetic shielding calculations)
User generated datasets of radiation effect quantities calculated on H time series data
12/11/2018
Final Presentation Day, ESTEC, The Netherlands

7. Update of the H reference dataset
GOES/SEM H datasets
GOES 5, 7, 8, 11, 13 ASCII data: 1986–2017
Complemented with SMS 1,2 and GOES 1, 2, 3, 5 binary FITS files from 1974 onward
Read and re-bin telemetry data
Output in same format as 5 min ASCII files
One additional solar cycle of H, He, X-ray and magnetic field data
12/11/2018
Final Presentation Day, ESTEC, The Netherlands

8. GOES/SEM data overview
Spacecraft
Start Time
End Time
Usage
SMS01
Jul 1974
Oct 1975
Jul 74 – Oct 75
SMS02
Feb 1975
Mar 1978
Nov 75 – Mar 77
GOES01
Jan 1976
May 1978
Apr 77 – Jul 77
GOES02
Aug 1977
May 1983
Aug 77 – May 83
GOES03
Jul 1978
Dec 1979
Not used
GOES05
Jan 1984
Mar 1987
Jan 84 – Feb 87
GOES06
Dec 1994
May 83 – Dec 83
GOES07
Aug 1996
Mar 87 – Feb 95
GOES08
Jan 1995
Jun 2003
Mar 95 – May 03
GOES09
Apr 1996
Aug 1998
GOES10
Jul 1998
Dec 2009
GOES11
Jul 2000
Feb 2011
Jun 03 – Jan 11
GOES12
Jan 2003
Sep 2010
GOES13
May 2010
Dec 2017
Feb 11 – 2017
12/11/2018
Final Presentation Day, ESTEC, The Netherlands

9. GOES data calibration
SEPCALIB method to re-define GOES energies using IM8/GME data
Re-bin cleaned GOES data into 11 standard energy bins (5–280 MeV), per spacecraft
Combine the re-binned datasets into a single time history (1974–2017)
Perform background subtraction
Reference SEPEM datasets
RDS v2.0: H without background subtraction, He with background removed
RDS v2.1: H and He with background removed
12/11/2018
Final Presentation Day, ESTEC, The Netherlands

10. RDS v2.1 H data
12/11/2018
Final Presentation Day, ESTEC, The Netherlands

11. March 2012 event
12/11/2018
Final Presentation Day, ESTEC, The Netherlands

12. SOLPENCO2 helioradial H event list
12/11/2018
Final Presentation Day, ESTEC, The Netherlands

13. Abundance ratios New ratio tables based on
SEPEM He RDS as a baseline
ACE/SIS ion data (C, N, O, Ne, Mg, Si, Fe): cleaned, gap filled 1 hour averages for 14 events
Extended to all other elements Li-U based on Reames (1998) or Asplund et al. abundance data (2009)
Calculation of uncertainties
12/11/2018
Final Presentation Day, ESTEC, The Netherlands

14. Magnetospheric shielding
Fortran magnetic shielding code
Interpolates from extensive new database of Geant4/ MAGNETOCOSMICS geomagnetic cut-off maps for different positions, epochs and Kp
12/11/2018
Cut-off rigidities interpolated and extrapolated to all space within the magnetosphere, linear interpolation in time/date, Kp
Calculation of uncertainties
Uses spacecraft trajectories to define transmission factors as a function of rigidity
Collaboration with Shea & Smart (RCINTUT3 program)
Final Presentation Day, ESTEC, The Netherlands

15. IRONSSIS Fast ion shielding model Developed as extension to MULASSIS
Simplified particle transport - 1D multi-layer shielding for any material(s), straight-ahead continuous slowing down approach (CSDA)
Similar outputs and interfaces to traditional MULASSIS
12/11/2018
Final Presentation Day, ESTEC, The Netherlands

16. Uncertainty propagation
Calculate and propagate the range of potential uncertainties in the SEPEM calculation process, addressing:
Cross-calibration of GOES/EPS and SMS/EPS data to IMP-8/GME
ACE/SIS-derived abundance ratios (C, N, O, Ne, Mg, Si and Fe)
Abundance ratios extended to all other elements Li-U based on Reames (1998) or Asplund et al abundance data (2009)
Limited proton and He event data (>260 SPEs) giving rise to uncertainties in fit parameters
Magnetospheric shielding calculation
Physical shielding calculation: Monte Carlo statistics for protons and systematic errors for non-Monte-Carlo CSDA approximation
12/11/2018
Final Presentation Day, ESTEC, The Netherlands

17. Validation of SEPEM against SPENVIS (4.6.8)
ESP proton and heavy ion fluence spectra
SEU
TID and TNID
12/11/2018
Final Presentation Day, ESTEC, The Netherlands

18. 15 yr near Earth orbit mission Event based (H + ions) – SEPEM reference event list ESP fluence – 95% CL – active years only
12/11/2018
Final Presentation Day, ESTEC, The Netherlands

19. 15 yr near Earth orbit mission Event based (H + ions) – SEPEM reference event list ESP fluence – 95% CL – active years only
12/11/2018
Final Presentation Day, ESTEC, The Netherlands
Differences in the heavy ion fluence behaviour above 60 MeV are due to the scaling with He in SEPEM while in the PSYCHIC model the scaling is with H.
The CREME96 derived abundances are not good but this is mainly because the He fluxes are too low, so to compensate the heavier ion abundances are much higher which is why the SPENVIS (ESP) and SEPEM (ESP+TRAD) outputs are so far below the SEPEM with use of CREME96.

20. SEU simulations (with previous generated ESP fluences) Unshielded SAMSUNG 16M (3.3 V DRAM) x 3.14 x 0.1 (µm) Si box S = 1.85 L0 = 0.60 MeV·cm2/mg W = MeV·cm2/mg σlim = 9.87E-08 cm2/bit A = 1.17 MeV - B = 0.92 MeV
12/11/2018
Final Presentation Day, ESTEC, The Netherlands
The proton induced and heavy ion (including the full range from He up to Fe) induced rates are comparable. Differences in the direct ionisation SEUs are likely due to differences in the calculated LET spectrum and adopted algorithm for calculating the deposited energy/charge inside the device during crossing. For  the latter SPENVIS uses the CREME method whereby the maximum LET of the stopping ion is applied over its entire path length in the sensitive volume.
SEPEM
(events/bit)
SPENVIS-4.6.8
Proton induced SEU
8.885e-3
8.918e-3
Direct ionization (He-Fe) SEU
0.839
1.177

21. TID and TNID simulation for H SEPEM: IRONSSIS (Mulassis mode for H) SPENVIS: MULASSIS v1.2.3 Primary fluence/flux: event based (H + ions) option - SEPEM reference event list 2 layer slab: 0.2 cm Al μm Si
SPENVIS
SEPEM
12/11/2018
Final Presentation Day, ESTEC, The Netherlands

22. ErrorTotalNID [MeV/g]
TID response function comparison for slab geometry
SEPEM
SPENVIS
SPENVIS new
Layer 1
Layer 2
Thickness [cm]
2.00E-01
1.00E-05
Density [g/cm3]
2.70E+00
2.33E+00
TID [rad]
1.04E-07
9.51E-08
1.45E-06
1.50E-06
1.07E-07
Error TID [rad]
2.22E-09
5.95E-09
9.49E-10
5.68E-09
6.78E-11
4.06E-10
12/11/2018
TNID response function comparison for slab geometry
SEPEM
SPENVIS
SPENVIS new
Layer 1
Layer 2
Thickness [cm]
2.00E-01
1.00E-05
Density [g/cm3]
2.70E+00
2.33E+00
TotalNID [MeV/g]
2.14E-03
1.88E-03
3.16E-02
2.79E-02
2.26E-03 
2.00E-03 
ErrorTotalNID [MeV/g]
5.78E-05
1.16E-04
2.46E-04
8.31E-06 
1.76E-05 
ProNID [MeV/g]
2.13E-03
3.15E-02
2.78E-02
2.25E-03 
1.99E-03 
ErroProNID [MeV/g]
5.75E-05
5.79E-05
8.30E-06 
NeutNID [MeV/g]
6.37E-06
6.43E-06
1.01E-04
1.12E-04
7.20E-06
8.00E-06 
ErrorNeutNID [MeV/g]
4.34E-06
5.87E-06
5.07E-06
4.19E-07 
3.62E-07 
PionNID [MeV/g]
0.00E+00
0.00E+00 
ErrorPionNID [MeV/g]
EleNID [MeV/g]
6.27E-07
3.69E-07
4.48E-08 
2.64E-08 
ErrorEleNID [MeV/g]
4.41E-07
2.52E-07
3.15E-08 
1.80E-08 
Final Presentation Day, ESTEC, The Netherlands
The difference between SPENVIS and SEPEM results is because of the energy spectrum normalisation applied for the SPENVIS results. One can get a good agreement between the two set of results by for example dividing the SPENVIS output by that normalisation factor (= SPENVIS new)

23. 12/11/2018
Demonstration
Final Presentation Day, ESTEC, The Netherlands