Components of soft X-ray and extreme ultraviolet in flares observed by LYRA I. E. Dammasch, M. Dominique, M. Kretzschmar (ROB/SIDC), P. C. Chamberlin (NASA/GSFC)

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Components of soft X-ray and extreme ultraviolet in flares observed by LYRA I. E. Dammasch, M. Dominique, M. Kretzschmar (ROB/SIDC), P. C. Chamberlin (NASA/GSFC) SCSL / PROBA2 Splinter Meeting ESWW8, Namur, 29 Dec 2011 LYRA the Large-Yield Radiometer onboard PROBA2

LYRA: the Large-Yield RAdiometer 3 instrument units (redundancy) 4 spectral channels per head 3 types of detectors, Silicon + 2 types of diamond detectors (MSM, PIN): - radiation resistant - insensitive to visible light compared to Si detectors High cadence up to 100 Hz

SWAP and LYRA spectral intervals for solar flares, space weather, and aeronomy LYRA channel 1: the H I nm Lyman-alpha line ( nm) LYRA channel 2: the nm Herzberg continuum range (now nm) LYRA channel 3: the nm Aluminium filter range incl the He II 30.4 nm line (+ <5nm X-ray) LYRA channel 4: the 6-20 nm Zirconium filter range with highest solar variablility (+ <2nm X-ray) SWAP: the range around 17.4 nm including coronal lines like Fe IX and Fe X

LYRA spectral response channel 2-3 (Aluminium filter) channel 2-4 (Zirconium filter) pre-launch calibration at BESSY additional SXR components <5 nm, <2 nm for comparison: GOES nm

Data product definition (“Level 0”, telemetry from PROBA2, internal) Level 1 = full raw data (counts/ms) Level 2 = calibrated physical data (W/m²) (Caution: preliminary status. Require versioning.) Level 3 = processed products (e.g. averages) Level 4 = plots of products Level 5 = event lists (optionally with plots)

New (well, more or less new) LYRA products … resulting from calibration attempts: Level 2 FITS files Level 3 FITS files (Level 4) One-day overviews (Level 4) Three-day overviews (Level 5) Flare lists (Level 5) GOES vs. LYRA proxies (preliminary) … available here at the P2SC website:

one-day overview

three-day overview

GOES vs. LYRA proxies For more information on this subject, please see the talk by David Berghmans, Automated flare detection and localization with PROBA2 Session 4A, Thursday 01 December 2011, 12:20

monthly overview

Example: M1.1 flare, 28 Feb 2011 start to rise at same time parallel in impulsive phase GOES peaks earlier LYRA decreases slower linear factor in pure flare irradiance

Flare components ch2-3 = SXR+EUV “SXR”: emission with log(T)>7 “EUV residual”: emission with 6<log(T)<7 “little bump”: emission with log(T)<6 Compare with SDO/EVE:

Thermal evolution plot based on: solar spectra observed by SDO/EVE contribution functions from the CHIANTI atomic database

Lyman-alpha signal LYRA in early 2010 signal peaks in rising phase log(T)<6

0.03 MK 0.7 MK 1.4 MK 3.7 MK 7.7 MK

May 2010 EVE vs. LYRA

M1.2 flare 05 May :19 UTC GOES ( nm) ~0.012 mW/m ² LYRA (0 - 2 nm) ~0.7 mW/m ² LYRA (0 - 5 nm) ~1.0 mW/m² EVE (0 - 7 nm) ~2.0 mW/m²

Feb/Mar 2011 EVE vs. LYRA