New Proton Low Altitude Radiation Belt Model RENELLA MS2b
A detailed overview of the RENELLA MS2b model developed to study the low altitude trapped proton environment, including objectives, model requirements, data coverage, and prime datasets for analysis. The model aims to cover a specific altitude and energy range, with a focus on various flux types and directionalities, as well as factors like geomagnetic field changes and atmospheric density effects.
Download Presentation
Please find below an Image/Link to download the presentation.
The content on the website is provided AS IS for your information and personal use only. It may not be sold, licensed, or shared on other websites without obtaining consent from the author.If you encounter any issues during the download, it is possible that the publisher has removed the file from their server.
You are allowed to download the files provided on this website for personal or commercial use, subject to the condition that they are used lawfully. All files are the property of their respective owners.
The content on the website is provided AS IS for your information and personal use only. It may not be sold, licensed, or shared on other websites without obtaining consent from the author.
E N D
Presentation Transcript
31/10/2018 A New Proton Low Altitude Radiation Belt (LARB) Model RENELLA MS2b, ESTEC, The Netherlands D. Heynderickx DH Consultancy, Leuven, Belgium 1
Project 31/10/2018 Radiation ENvironment at Extremely Low Latitude and Altitude (RENELLA) ESA Contract No 4000118058/16/NL/LF/hh Consortium RadMod Research (UK, F. Lei): prime contractor DH Consultancy (Belgium, D. Heynderickx) SPARC (Greece, I. Sandberg, C. Papadimitriou, S.A. Giamini) Kallisto Consultancy (UK, P. Truscott) CSR/UCL (Belgium, M. Cyamukungu, S. Borisov) RBISA (Belgium, N. Messios, E. De Donder) RENELLA MS2b, ESTEC, The Netherlands 2
RENELLA objectives 31/10/2018 XIPE (proposed X-ray mission) environment specification validation Dataset production Selection of primary datasets Ingestion in ODI database Cross-calibration Definition of new LARB (Low Altitude Radiation Belt) proton model Reconstruct PSB97 model for fast revision of XIPE radiation environment Develop methodology for detailed new model development Algorithms for propagation of fluxes to lower altitudes, uni<>omni, differential<>integral, East-West asymmetry Secular change in IGRF, solar cycle PLANETOCOSMICS for modelling support and validation Production of new LARB model (<1,000 km) and implementation in SPENVIS and IRBEM RENELLA MS2b, ESTEC, The Netherlands 3
Model requirements 31/10/2018 To construct a low altitude trapped proton model covering: Altitude range: [100,1000] km Energy range: [0.1,1000] MeV Differential and integral flux Unidirectional (pitch angle dependence) and omnidirectional flux 2D directionality (polar and azimuthal angle) Secular change in geomagnetic field Atmospheric density effects RENELLA MS2b, ESTEC, The Netherlands 4
Data coverage 31/10/2018 Prime datasets Low energy(directional): S3-3/PT (0.1 2.2 MeV) Intermediate energy (directional): SAMPEX/PET (20 400 MeV), RBSPA/REPT/L3 (21 208 MeV), AZUR/EI-88 (2 70 MeV), CRRES/PROTEL (1.5 83 MeV) High energy (omnidirectional): RBSPA/RPS/L2 (58 1,300 MeV) Auxiliary datasets PROBA1/SREM (12.4 220 MeV) PROBAV/EPT (11 273 MeV) S3-3/PT and AZUR/EI-88 data averages are used to extend spectra to low energies RENELLA MS2b, ESTEC, The Netherlands 5
Data coverage: SAMPEX/PET 31/10/2018 RENELLA MS2b, ESTEC, The Netherlands 6
Data coverage: RBSPA/REPT 31/10/2018 RENELLA MS2b, ESTEC, The Netherlands 7
Data coverage: RBSPA/RPS 31/10/2018 RENELLA MS2b, ESTEC, The Netherlands 8
Data coverage: CRRES/PROTEL 31/10/2018 RENELLA MS2b, ESTEC, The Netherlands 9
LARB model definition 31/10/2018 Classic method using (L, 0) maps breaks down How to combine data from different epochs How to use the model with recent magnetic field models Atmospheric effects are not represented TREND method: (K,nhmin) map Kauffman K = I B Atmospheric density at lowest mirror point Advantages hmin is proxy of L* (invariant to secular variation of magnetic field) Using n incorporates atmospheric driving K squares the flux maps Data from different epochs can be combined Only 1 model map is needed (per energy) RENELLA MS2b, ESTEC, The Netherlands 10
Calculating n at hmin hmin is found by tracing the drift shell This is time consuming Generate yearly (L, 0) -> (I,K,hmin) maps (using mid-year IGRF and updated magnetic field model) with UNILIB Fit hmin(I) dependence as a parabola and store the fit parameters Use inverse fit to derive 0c(104 km) Data binning (per energy channel) Calculate (L,I,K, 0) for each data record Calculate hmin(I) using the stored parabolic fit coefficients Calculate n(hmin) Bin in (K,n(hmin)) grids 31/10/2018 RENELLA MS2b, ESTEC, The Netherlands 11
Atmospheric density model 31/10/2018 COSPAR reference model is MSISE-00, depending on altitude, latitude, longitude, day of year, hour of day, Ap, F10.7 (current day and 81 day average) Pfitzer [1990] used a simplified atmosphere model (developed by McDonnell Douglas Astronautics Co.), depending only on altitude and F10.7 (7 day and 90 day average) ? = ?0 exp RENELLA MS2b, ESTEC, The Netherlands ? 120 ? ? 103 ?10.7+ ?10.7A 110 ? = 0.99 + 0.518 Excellent approximation of MSISE-90 nhmin 12
East-West effect 31/10/2018 Since TREND-3, no additional low altitude data with azimuthal dependence have become available Therefore, use the azimuthal dependence model derived in TREND-3 Integrate the ANISO code into the model suite When running the model, calculate omnidirectional flux at each time step RENELLA MS2b, ESTEC, The Netherlands 13
Model maps: SAMPEX/PET 31/10/2018 RENELLA MS2b, ESTEC, The Netherlands 14
Model maps: RBSPA/REPT 31/10/2018 RENELLA MS2b, ESTEC, The Netherlands 15
Model maps: RBSPA/RPS 31/10/2018 RENELLA MS2b, ESTEC, The Netherlands 16
Model maps: CRRES/PROTEL 31/10/2018 RENELLA MS2b, ESTEC, The Netherlands 17
SAMPEX/PET SAA: altitude 31/10/2018 RENELLA MS2b, ESTEC, The Netherlands 18
