Monitoring solar energetic particles with ESA SREM units
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1 Monitoring solar energetic particles with ESA SREM units I. Sandberg Institute for Space Applications and Remote Sensing National Observatory of Athens, Greece The 10th Hellenic Astronomical Conference 5-8 September 2011, Ioannina
2 Collaborators I.A. Daglis, A. Anastasiadis and G. Balasis Institute for Space Applications and Remote Sensing, NOA M. Georgoulis Research Center of Astronomy and Applied Mathematics, Academy of Athens P. Nieminen and E. Daly Space Environments and Effects Section, ESA/ESTEC Extension of ESA contract number 21480/08/NL/NR
3 Outline ESA Standard Radiation Monitor The ESA SREM missions Solar energetic particles and events SREM detection principle Unfolding SREM data Validation of method The solar energetic particle flux tool
4 ESA Standard Radiation Environment Monitor GIOVE-B PROBA-1 INTEGRAL ROSETTA HERSCHEL PLANCK
5 ESA Standard Radiation Monitor Charged particle detector based on three solid state Si crystals Detects high-energy charged particles: e - E e >1 MeV, p + : E p >10 MeV Monitors spacecraft radiation environment Provides functions related to space weather hazards for the host spacecraft and its payload Provides data associated to various physical processes.
6 Orbits Missions Sources SREM multipoint measurements Radiation Belts Solar Particle Events Cosmic Rays
7 Sources of solar energetic particles Impulsive events Gradual events Associated Source Solar flares CMEs Particles electrons, 3 He, heavy ions Proton rich Occurrence frequency ~10 3 /y during solar maximum ~10/y during solar maximum Duration ~ hrs ~ days Heavy isotope abundances Ionization state Enhanced compared to coronal populations Enhanced compared to coronal populations Similar to coronal populations Similar to coronal populations Net fluence < particles/cm 2 ~ 10 9 particles/cm 2
8 Solar particle event NOAA definition: the period of time when the integral flux of protons with energy greater than 10 MeV exceeds 10 particles/sec/cm 2 /sr.
9 SREM/SEP data Mission Data Orbit PROBA1 INTEGRAL Rosetta Herschel Planck GIOVE-B LEO (sun synchronous) HEO (highly eccentric) Interplanetary L2 L2 MEO (near-circular) GIOVE-B PROBA-1 INTEGRAL ROSETTA HERSCHEL PLANCK
10 SREM: Principle of detection SREM consists of three solid-state Si detectors (d1 & d2, d3) Charged particle interacts with band electrons and creates e - -hole pairs Collected charge is proportional to the energy loss of incident particles Pre-amplified pulses are scrutinized and registered in 15 counters
11 SREM counters
12 INTEGRAL/SREM Response functions
13 Unfold SREM data: Counts to fluxes Fredholm integral equation of the first kind -> Ill-posed problem: non-unique solution, solution is not a continuous function of counts The numerical solution of the discrete problem is widely oscillating SREM channels have strongly overlapping energy ranges Proton/electron contamination effects finite spectral resolution/calibration errors noise in measurements log(f p ) E p
14 Unfold SREM data: regularization [Höcker A. and Kartvelishvili V., Nucl. Inst. Phys. Res. A 372, (1996)]
15 Regularized solution log(f p ) low energies E p
16 SREM/INTEGRAL data during January 2005
17 Non-suppressed regularized solutions 1. Unfold SREM data for different energy ranges
18 Non-suppressed regularized solutions 2. Select the maximum values for each energy level
19 Non-suppressed regularized solutions 3. Apply a small correction factor if needed-
20 Non-suppressed regularized solutions 4. Comparisons with independent methods/datasets SREM/SVD GOES11/EPS SREM/SCF
21 SREM/INTEGRAL data during January 2005
22 January 2005 SEPE: Proton fluxes
23 January 2005 SEPE: Reconstruction
24 January 2005 SEPE: Comparison SEPEM: ESA Solar Energetic Particle Environment Modelling database
25 January 2005 SEPE: Validation
26 SREM/INTEGRAL data during October-November 2003
27 October-November 2003 SEPEs
28 October-November 2003 SEPEs
29 SEP multipoint measurements I Magnetic connectivity effects: September 2005 SEPEs
30 SEP multipoint measurements II August 14, 2010: 1 st SEP of Solar Cycle 24 C4.4 Flare Start: 09:38:00 Peak: 10:05:00 End: 10:31:00 Location: N17 W52
31 SEP multipoint measurements II Halo Effects
32 ISARS/NOA SREM activities provide proton flux profiles to Herschel team on a weekly basis since begin of 2011 provide calculations of the total fluence of Rosetta mission develop and operate SEPF tool Derive SREM proton flux database for INTEGRAL, Rosetta, Herschel and Planck missions
33 SEPF tool
34 SEPF tool
35 SREM proton fluxes: database
36 Summary-Conclusions Data from SREM units on-board multiple ESA spacecraft offer a unique opportunity for multipoint observation of SEPE A novel method for unfolding SREM data has been developed The derived proton flux datasets have been validated with fully processed, corrected, cleaned, inter-calibrated, scientific datasets SEPF: A near-real time monitor of solar proton fluxes has been released and operated by ISARS/NOA The proton flux SREM database is under preparation containing multipoint measurements (MEO,LEO,L2,HEO,IP) Novel properties of past and coming SEPEs will be revealed
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