LYRA Calibration using TIMED and SORCE I. E. Dammasch, ROB/SIDC Solar EUV Irradiance Working Group Inter-Calibration and Degradation of EUV Instruments.

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Presentation transcript:

LYRA Calibration using TIMED and SORCE I. E. Dammasch, ROB/SIDC Solar EUV Irradiance Working Group Inter-Calibration and Degradation of EUV Instruments ROB, Brussels, Belgium, Apr 2013 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 pre-flight spectral responsivity (filter + detector, twelve combinations)

Calibration- Problem: 2010 according to TIMED/SEE

Calibration-Problem: 2010 according to LYRA

Speculation on spectral degradation (Edge could actually be steeper between 17nm and 20nm)

First Light acquisition (06 Jan 2010) … no degradation so far …

Start with “First Light”…

…estimate and subtract dark currents…

… fit the degradation …

… and add it Plausibility: - Artifacts in channels 1 and 2 - Non-degraded SXR in channels 3 and 4 Disadvantages: - Underestimate EUV in channels 3 (and 4) - Distortion of occultations

Formal: i = is + id i=measured photocurrent is=solar photocurrent id=dark current is = A/T ∫ ∫ E(λ,t) F(λ) D(λ) dλ dt t λ λ=wavelength A=detector surface T=total exposure time E(λ,t)=solar spectral irradiance F(λ)=filter transmittance D(λ)=detector spectral responsivity

LYRA Radiometric Model, ch1-1 simulated

Observed vs. LRM-simulated values (head 1) ch1-1 ch1-2 ch1-3 ch1-4 sim nA nA nA nA obs ~1300.0counts/ms 620.0counts/ms 24.0counts/ms 37.5counts/ms dc -9.0counts/ms -6.6counts/ms -6.8counts/ms -7.2counts/ms VFC,resis. => => => => nA nA nA nA +81.3% +13.3% +11.2% +14.3%

LYRA Radiometric Model, ch2-4 simulated

Observed vs. LRM-simulated values (head 2) ch2-1 ch2-2 ch2-3 ch2-4 sim nA nA nA nA obs 500.0counts/ms 710.0counts/ms 23.0counts/ms 45.0counts/ms dc -8.0counts/ms -6.5counts/ms -6.4counts/ms -7.5counts/ms 492.0counts/ms 703.5counts/ms 16.6counts/ms 37.5counts/ms multiplied by VFC-parameter in V/(counts/ms), divided by resistance in Giga-Ohm => * * * * /10.37 / /1.016 /10.30 obs nA nA nA nA +91.2% +22.8% +17.6% -2.0%

LYRA Radiometric Model, ch3-3 simulated

Observed vs. LRM-simulated values (head 3) ch3-1 ch3-2 ch3-3 ch3-4 sim nA nA nA nA obs 930.0counts/ms 552.0counts/ms 280.0counts/ms 36.2counts/ms dc -10.0counts/ms -6.5counts/ms -6.4counts/ms -6.2counts/ms VFC,resis. => => => => nA nA nA nA +3.3% +18.0% +11.2% +15.4%

Formal: Ecal = iuncal – id + corr Ecal(FL) iuncal(FL)-id(FL) Ecal,Ecal(FL) = LYRA-channel spectral irradiance in W/m2 (FL=First Light) iuncal,iuncal(FL)= observed effect of solar irradiance in counts/ms (proportional to solar photocurrent in nA) Ecal(FL) = iuncal(FL)-id(FL) ∫ Es(FL) dλ is(FL) Es(FL) = solar spectral irradiance from TIMED&SOLSTICE is(FL) = simulated photocurrent in nA (proportional to count rate)

Resulting conversion to physical units +81.3% +13.3% +11.2% +14.3% (1) +91.2% +22.8% +17.6% -2.0% (2) +3.3% +18.0% +11.2% +15.4% (3) => ? (0.0%) => +18.0% => +13.3% => +9.2% ch*-1 ch*-2 ch*-3 ch*-4 ( nm) ( nm) (17-80&0-5nm) (6-20&0-2nm) W/m² W/m² W/m² W/m² ? (0.0%) +18.0% +13.3% +9.2% => W/m² W/m² W/m² W/m² which corresponds to counts/ms 703.5counts/ms 16.6counts/ms 37.5counts/ms (Example: Head 2, dark currents subtracted) Degradation added. Simple linear conversion.

Solar EUV irradiance according to LYRA LYRA channel 2-3 (17-80nm degraded(?) plus <5nm) LYRA channel 2-4 (6-20nm plus <2nm) Jan 2010 – Apr 2013, versus GOES (scaled)

Possible error sources First-Light-Day calibration (selection of “significant” values, difference among LYRA units, measured/modeled channel response, difference among TIMED and SORCE, short wavelengths modeled, hardly info below 1nm) Degradation estimation Simple addition (spectral degradation in channels 3 and 4) Dark current estimation Simple linear conversion (different response in SXR and EUV)

Next steps Is the long-term development consistent ? Cross-calibration with LYRA units 1 and 3 Cross-calibration with TIMED and SORCE Cross-calibration with SDO/EVE (others?) What do the flares consist of (spectral, thermal) ?