1. EUS - Science, JCV,RAL, March 2006 1 Solar Orbiter EUI/SOLAR ORBITER Report of the Science WG T. Appourchaux, F. Auchère, L. Harra, E. Marsch, L. Teriaca, J.-F. Hochedez, U. Schühle J.-C. Vial

2. EUS - Science, JCV,RAL, March 2006 2 EUI / Solar Orbiter Our Mandate (1) : Definition of scientific objectives through building observing programs detailing : targets, wavelengths, spatial and spectral resolution, cadence, exposure time, duration, data selection · Collecting the photometric information from the Photometry WG · Liaising with other instruments Science Teams (EUS, VIM, COR, in situ) to investigate the common objectives and the joint science to be made (i.e. possible). ·

3. EUS - Science, JCV,RAL, March 2006 3 EUI / Solar Orbiter Our Mandate (2) : · Building complete observing scenarii (target, FOV, cadence, etc.) covering the whole perihelion duration in liaison with the Compression and Data Selection WG · Prioritizing the objectives/programs · Translating the prioritization in terms of instruments parameters (wavelengths, etc...) · Liaise with the Radiometry, Functionality of Electronics, Compression and Data Selection, Coatings and Mirrors WGs

4. EUS - Science, JCV,RAL, March 2006 4 EUI / Solar Orbiter Call for proposals (Spring 2005, from inside the consortium) 14 proposals, more or less elaborated and following two different formats 12 for HRI, 1 for HRI and FSI, 1 for FSI All HRI proposals use the close-up capability (spatial resolution) + co-rotation + polar view HRI proposals combine with EUS and/or VIM observations

5. EUS - Science, JCV,RAL, March 2006 5 HRI coronal proposals (1) Science IssueTime Res. Lines (nm)SO objectives Signatures of nanoflare heating JCV < 1 min 30.4, 19.5, 33.5 (Fe XVI) or 121.6, 17.1, 28.4 2.2.2 Acceleration and heating (fast wind) 2.2.3 Sources of slow wind 2.3.3.2 Transient events The quiet Sun small- scale activity LT 10 sec 121.6, 17.32.2.2 Acceleration and heating (fast wind) 2.2.3 Sources of slow wind 2.3.3.2 Transient events Intermittence in the Solar Corona EB 1 min 30.4, 19.5, 36.4 (Fe XII at 7 10 6 K ?) 2.2.2 Acceleration and heating (fast wind) 2.2.3 Sources of slow wind 2.3.3.2 Transient events Origin of the solar wind turbulence SG 1 min 30.4, 19.5, 36.4 or 121.6, 2.2.2 Acceleration and heating (fast wind) 2.2.3 Sources of slow wind EB: E. Buchlin, SG : S. Galtier, LT : L. Teriaca, JCV : J.-C. Vial

6. EUS - Science, JCV,RAL, March 2006 6 HRI coronal proposals (2) Science Issue Time Res. Lines (nm)SO objectives Fine structure prominences / filaments NL ~10 sec 121.6, 30.4, 17.3 2.2.4 Sources and dynamics of eruptive events ? 2.1.3 Influence of CMEs on the structure of the inner heliosphere ? Flares and filaments eruptions LH 10 sec 30.4, 17.1 Spectro- Imager 2.2.4 Sources and dynamics of eruptive events 2.1.3 Influence of CMEs on the structure of the inner heliosphere Emerging flux regions and magnetic helicity LG 30 min 17.1, 19.5 Spectro- Imager 2.3.3.1 Flux emergence and its consequences 2.4.4. Flux emergence at high latitudes Flare-induced active-region loop oscillation DW 20 sec 17.1 Spectro- Imager 2.3.3.3 wave activity from the photosphere to the corona LH : L. Harra, NL: N. Labrosse, DW : D. Williams, LG : L. Gesterlyi

7. EUS - Science, JCV,RAL, March 2006 7 HRI coronal proposals (3) Science IssueTime Res. Lines (nm)SO Objectives Seismology of various structures : plumes, loops, prominences FB 30 secCool / Hot lines2.3.3.3 wave activity from the photosphere to the corona Coronal hole plumes GDZ 10-30 sec Fe VIII (16.8 nm ?), 17.1, 19.5 Spectro- Imager 2.3.1 How is the polar high speed wind generated and how does it relate to polar plumes ? Origins of the solar wind SM ~ min.30.4, 17.1 Spectro- Imager 2.2.3 Sources of slow solar wind, temporal and spatial variation 2.3.1 How is the polar high speed wind generated and how does it relate to polar plumes ? FB : F. Baudin, GDZ : G. Del Zanna, SM : S. Matthews

8. EUS - Science, JCV,RAL, March 2006 8 HRI/FSI coronal proposals (4) Science IssueTime Res. Lines (nm)SO Objectives Quasi-rigid rotation of coronal holes and origins of the slow solar wind SM ~ min 30.4, 17.1 Spectro- Imager 2.3.2 Nature of coronal hole boundaries, evolution and projection in the heliosphere The streamers as source of slow solar wind SP ~minHRI : 30.4 (or 121.6), 19.5, 46.5 (Ne VII)? FSI : 17.1 2.2.3 Sources of slow solar wind, temporal and spatial variation Polar plumes + irradiance anisotropies FA 30.4 or 17.1 or 33.5 2.3.1 How is the polar high speed wind generated and how does it relate to polar plumes ? FA : F. Auchère, SM : S. Matthews, SP : S. Parenti

9. EUS - Science, JCV,RAL, March 2006 9 Solar Orbiter Summary (1) All need high resolution Interest for co-rotation (long-term observations (AR), oscillations, correlation with in-situ,...) Interest for polar observations Quite universal interest in velocity measurements : Range ? Wavelengths,.... Issue of pointing/tracking specific features (AR,..)

10. EUS - Science, JCV,RAL, March 2006 10 Solar Orbiter Summary (2) HRI : Need for cool, hot and (for micro-scales programs) very hot lines Interest expressed in spectro-imagery (MOSES-type): essentially in 30.4 nm FSI : Context for EUI and EUS observations But also specific programs (large-scale structures, oscillations,..) 17.1 (or 19.5 nm) Interest for a second (cool) line

11. EUS - Science, JCV,RAL, March 2006 11 Solar Orbiter EUI December 2005 meeting HRI : imaging only Lalpha channel ? FSI : one or two wavelengths ? Spectro-imagery (Moses-type) ??

12. EUS - Science, JCV,RAL, March 2006 12 Solar Orbiter Actions Getting the community involved : Call for contributions : to be issued Attached document (+ www) http://www.ias.u-psud.fr/tpl2page.php?pageID=702 providing a template for proposals providing a Table from Photometry WG establishing a continuous link between the consortium and the community, including news about the output of their inputs

13. EUS - Science, JCV,RAL, March 2006 13 Solar Orbiter Conclusions For a proper definition of EUI : * Continue the work on science priorities, adressing issues such as : What the SO priorities within the SO objectives ? What is unique in SO as compared with STEREO, SolarB and SDO ? Some common wavelengths with EUS ! * Take into account the instruments / S/C capabilities (compression, photometry, pointing/tracking of AR,...) * Build 15 days of observations scenarii (taking into account TM rates vs. distance to the Sun )