Solar Irradiance Observations Solar Irradiance Observations with LYRA on PROBA2 with LYRA on PROBA2 (An Introduction) (An Introduction) I. E. Dammasch, M. Dominique & the LYRA Team I. E. Dammasch, M. Dominique & the LYRA Team Royal Observatory of Belgium LYRA the Large-Yield Radiometer onboard PROBA2
54
Embed
Solar Irradiance Observations with LYRA on PROBA2 (An Introduction) I. E. Dammasch, M. Dominique & the LYRA Team Royal Observatory of Belgium LYRA the.
This document is posted to help you gain knowledge. Please leave a comment to let me know what you think about it! Share it to your friends and learn new things together.
Transcript
Solar Irradiance ObservationsSolar Irradiance Observationswith LYRA on PROBA2with LYRA on PROBA2
(An Introduction)(An Introduction)
I. E. Dammasch, M. Dominique & the LYRA TeamI. E. Dammasch, M. Dominique & the LYRA Team
Royal Observatory of Belgium
LYRAthe 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
• Royal Observatory of Belgium (Brussels, B)Principal Investigator, overall design, onboard software specification, science operations
• PMOD/WRC (Davos, CH)Lead Co-Investigator, overall design and manufacturing
• Centre Spatial de Liège (B)Lead institute, project management, filters
• IMOMEC (Hasselt, B)Diamond detectors
• Max-Planck-Institut für Sonnensystemforschung (Lindau, D)calibration
• science Co-Is: BISA (Brussels, B), LPC2E (Orléans, F)…
LYRA highlights
LYRA highlights
4 spectral channels covering a wide emission temperature range
Redundancy (3 units) gathering three types of detectors Rad-hard, solar-blind diamond UV sensors (PIN and MSM) AXUV Si photodiodes
2 calibration LEDs per detector (λ = 465 nm and 390 nm) High cadence (up to 100Hz) Quasi-continuous acquisition during mission lifetime
Ly Hz Al Zr
Unit1 MSM PIN MSM Si
Unit2 MSM PIN MSM MSM
Unit3 Si PIN Si Si
SWAP and LYRA spectral intervalsfor solar flares, space weather, and aeronomy
LYRA channel 1: the H I 121.6 nm Lyman-alpha line (120-123 nm)LYRA channel 2: the 200-220 nm Herzberg continuum range (now 190-222 nm)LYRA channel 3: the 17-80 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
Occultations: Study atmospheric absorption; high temporal resolution needed Input for atmospheric models: NRT and calibrated data needed
Flares
LYRA observes flares down to B1.0
LYRA flare list agrees with GOES14&15
Flares are visible in the two short-wavelength channels
Exceptionally strong and impulsive flares are also visible in the Lyman- alpha channel (precursor)
Example: C4.0 flare, 06 Feb 2010, 07:04 UTC
M2.0 flare, 08 Feb 2010, 13:47 UTC
Comparison with GOES flare
Example: M1.8 flare, 20 Jan 2010, 10:59 UTC
ComparisonwithGOES flare
Example:C5.4 flare,15 Aug 2010,18:30 UTC
LYRA flare size
LYRA background-subtracted flux in Zr (channel 2-4)LYRA observes all GOES flares in both Al and Zr channelsInitially also Lyman-alpha contribution for strong impulsive flaresSimilar onset, different peak times in different pass bandsGood correlation to GOES, better temporal resolution
GOES vs. LYRA proxies
(new website under construction)
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
Sun-Moon eclipse
…demonstrating the inhomogeneous distribution of EUV radiation across the solar surface
Eclipses as seen with SWAP
swap_eclipse_15Jan2010.mp4
swap_eclipse_11Jul2010.mp4
And we have a fifth channel at 17.4nm...
... called SWAP
(using “SWAVINT”)
Jan - Sep 2010
SWAVINT and LYRA
look quite similar
LYRA shows flares
in addition to EUV
SWAP and LYRA observing together
20100607_proba2_movie.mp4
July 2010: LYRA vs. ESP (SDO/EVE)
July 2010: LYRA vs. GOES
Next steps
Cross-calibration (internal/external) Produce calibrated data automatically (OK,
but regular updates necessary) Publish first results (in process) Advertise data products Get another extension from ESA (2012: OK)
How to be involved?
Scientists are welcome touse PROBA2 datapropose special observation campaigns
Guest Investigator Program welcomes proposals for dedicated (joint) observations in the frame of a science project:Funds available for a stay at PROBA2 Science CenterScientist can take part in the commanding of the instrumentsWill gain expertise in the instrumental effects
Next announcement (for 2011-12): May 2011Proposal deadline and selection: June 2011First visits: September 2011 onwards