COSPAR ‘06, Beijing 19 July 2006 UV solar disc imagers of Kuafu-A Pierre Rochus ° Jean-François Hochedez * Jean-Marc Defise ° Pierre-Alexandre Blanche ° Udo Schuehle “ ° Centre Spatial de Liège, CSL, Belgium * SIDC- ROB, Royal Observatory of Belgium “ MPS, Lindau, Germany

COSPAR ‘06, Beijing - 19 July 2006J.-F. Hochedez, ROB-SIDC International Telescope Suite for the Investigation of Solar Eruptive Events ITSISEE (It’s easy! … SpW forecast…) EDI (or ELATE?) Euv + Lyman-Alpha Telescope + Guide Telescope MOSES Multi Order Solar EUV Spectrograph LyCo Lyman-alpha Coronagraph ViCo Visible light Coronagraph ITSISEE is an observatory for Solar Weather forecast and nowcast

COSPAR ‘06, Beijing - 19 July 2006J.-F. Hochedez, ROB-SIDC EDI = EUV + Lyman Alpha Telescopes 19.5 nm, Fe XII & Fe XXIV – Focal length 1200 mm – ~1 nm FWHM – Pupil = 33 mm diameter nm, H Ly  – Focal length 1200 mm – Purity: >70%, goal = 90% – Pupil mm TBC 2 filtergraph telescopes – FOV > 45 Arcmin – Pixel < 2.6 Arcsec, viz. 1k x 1k or more – 1 minute non-stop cadence ! – More if possible, where/when useful – 1 Gbit/day per telescope TBC

COSPAR ‘06, Beijing - 19 July 2006J.-F. Hochedez, ROB-SIDC The EUV Telescope (1/2) SoHO-EIT (Jan. 1996) and Proba2-SWAP (Sep. 2007) heritage – CSL + ROB in Belgium Off-axis Ritchey-Chretien

COSPAR ‘06, Beijing - 19 July 2006J.-F. Hochedez, ROB-SIDC The EUV Telescope (2/2) Lighter mirrors Absence of external baffle (There is room for internal baffling) Mirrors – Multi-layer – super-polished Smaller filters (at the entrance pupil)

COSPAR ‘06, Beijing - 19 July 2006J.-F. Hochedez, ROB-SIDC Proba2-SWAP (1/2) A new EUV solar telescope for the ESA PROBA2 mission

COSPAR ‘06, Beijing - 19 July 2006J.-F. Hochedez, ROB-SIDC New technologies: - APS CMOS detector - Off-axis optical design - Onboard image processing Proba2-SWAP (2/2)

COSPAR ‘06, Beijing - 19 July 2006J.-F. Hochedez, ROB-SIDC The Lyman-  Telescope Quasi-identical optical design as the EUV one Heritage from TRC but off-axis – Transition Region Camera, R. M. Bonnet, 1980 Multilayer coatings on the 2 mirrors – Al/MgF2/B4C or Al/MgF2 optimized for 1215 Å. >70% purity (FWHM<7nm) – ACTON RESEARCH filters (+ solarblind detector?)

COSPAR ‘06, Beijing - 19 July 2006J.-F. Hochedez, ROB-SIDC Solar science addressed by the EUV telescope 195 (1.6MK) is an established “General Purpose” coronal channel Observable in still images: – Coronal Holes (CH are the source of the fast wind) – Active Regions & Filaments (AR are flare & CME sites) – Sigmoids, EUV flares, post-eruptive arcades… Observable in image sequences: – Eruption/CME on-disc signatures EIT waves & dimmings, CME mass estimates Filament instabilities leading to their eruption Forecasting better – Progress about physics of event precursors – Inputs to SpW data assimilation codes

COSPAR ‘06, Beijing - 19 July 2006J.-F. Hochedez, ROB-SIDC Solar science addressed by the Ly  telescope Ly-a solar images have never been monitored – Not even by SDO-AIA (which has He II  synergies), Preparation for S.O. – Brightest line allows fast cadence – Emission mechanisms (typ K but actually K) Ly-a solar images will reveal (cf VAULT rocket experiment) – dense prominences in absorption and in emission (mass estimation) – … CH, jets, spicules (like in H  ) – Cool magnetic field lines over the photosphere at the limb (not seen in H  ) – Chromospheric response to Corona and flares, “moss”, Moreton waves… EUV emission always associated with Ly-a emission – but not the reverse  observe inside CH Will improve solar irradiance models – Main energetic contribution to Earth lower ionosphere – Sources of Ly-a irradiance variability – Imaging give access to irradiance in the heliosphere  Planetary aeronomy With ideas from Dr. A. Vourlidas (VAULT PI)

COSPAR ‘06, Beijing - 19 July 2006J.-F. Hochedez, ROB-SIDC Anticipated improvements of ELATE over SOHO-EIT Use of CMOS imaging detector – 2k x 2k? Solarblind AlGaN CMOS detectors? – Smart camera schemes, optimal SNR Improved calibrations – Optical element robustness improved – On-ground, in-flight (UV LEDs) Polarimetry at Ly-alpha – Bommier, V.; Sahal-Brechot, S.; Leroy, J. L. Optimised lossy image or movie compression schemes – 15x and up to 200x !  1 min cadence or better – Moderate the concern of being at L1 (cf. telemetry) Data filtering – Since SOHO, main progress is with CPU and algorithmic – Autonomous operations e.g. triggering sub-field high cadence acquisition

COSPAR ‘06, Beijing - 19 July 2006J.-F. Hochedez, ROB-SIDC Mission complementarities (1/2) Timeline & Missions complementarities Soho C IR C IR C IR C IR Stereo CI S Solar B III SDO IR PROBA2 IR PROBA3 CCC KUAFUCI S? S.O. CI I : UV imaging C: Coronagraph R: UV Radiometer S: stereo ability S: stereo ability??

COSPAR ‘06, Beijing - 19 July 2006J.-F. Hochedez, ROB-SIDC 2 ideas for Kuafu-A ITSISEE well tailored for CME forecast but less so for flares’ (often CME-associated) – Need for a full-sun wide range spectrograph or spectro-imager Array of 10 one-mirror low-resolution multilayer telescopes? Spectro-heliograph design (cf. Coronas-F mission) – Interest for such an instrument exists in Europe (B, CH…) Stereoscopy? – L1 brings constraints but could bring an extremely valuable bonus: stereoscopy in coordination with the LWS mission SDO (AIA). Parallax of possible L1 orbits to be assessed

COSPAR ‘06, Beijing - 19 July 2006J.-F. Hochedez, ROB-SIDC Conclusions  UV solar disc imagers of Kuafu-A (ELATE)  Rest of the RS suite (ITSISEE)  Whole scientific payload of the Kuafu mission Inescapable for  solar physics  Solar Weather monitoring in and beyond