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LYOT, SFSA, Juillet 20071 LYOT : LYman Orbiting Telescopes à bord de la mission franco-chinoise SMESE (Small Explorer for solar Erupions) Frédéric Auchère,

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Presentation on theme: "LYOT, SFSA, Juillet 20071 LYOT : LYman Orbiting Telescopes à bord de la mission franco-chinoise SMESE (Small Explorer for solar Erupions) Frédéric Auchère,"— Presentation transcript:

1 LYOT, SFSA, Juillet LYOT : LYman Orbiting Telescopes à bord de la mission franco-chinoise SMESE (Small Explorer for solar Erupions) Frédéric Auchère, Jean-Claude Vial Institut d’Astrophysique Spatiale T. Appourchaux, K. Bocchialini, M. Derouich (I.A.S.) P. Lamy (L.A.M.), S. Koutchmy (I.A.P.) U. Schühle (MPS), E. Antonucci, S. Fineschi (Obs. Turin), M. Romolli (Univ. Florence) Autres collaborations : ORB, CSL, RAL, LESIA, LERMA, …

2 LYOT, SFSA, Juillet 20072

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4 4 Mécanisme d’initiation des CMEs et Eruptions : reconnexion magnétique from Anzer et Pneumann (1982)

5 LYOT, SFSA, Juillet Initiation des Coronal Mass Ejections (CMEs) (1) Source instability which leads to the CME ? 4 critical parameters concerning the acting forces: * initial acceleration * non-radial motions * transverse (latitudinal) expansion * initial radial expansion Must be measured below 2 Rs

6 LYOT, SFSA, Juillet Initiation des Coronal Mass Ejections (CMEs) (2) Source instability which leads to the CME ? Several models (e.g. flux rope, Amari et al. 2003, breakout model, Aulanier et al. 2001) None have been validated

7 LYOT, SFSA, Juillet Magnetic field in the corona Corona cannot be fully understood without the magnetic field Measured at the surface Not measured in the corona

8 LYOT, SFSA, Juillet Measurements of the coronal magnetic field Bommier & Sahal (1982) Rotation polarisation Dépolarisation (B < 50 G pour L) Hanle effect

9 LYOT, SFSA, Juillet Further studies Structure of the transition between chromosphere and corona Spatial and temporal variability of the La irradiance Origin of solar energetic particles (SEPs) Factor 3 variability at 30.4 nm (~L) SEM/SOHO

10 LYOT, SFSA, Juillet LYOT Why a L coronagraph ? Why a L imager ?

11 LYOT, SFSA, Juillet LYOT (and SMESE payload) performances Wavelength / Energy Field of View Spatial (pixel) resolution Watching -mode Cadence Event- mode cadence Daily data volume LYOT : L  imager nmFull Disk1.1 arcsec10 s0.2 s LYOT : L  coronagraph nm5*5 solar radii 2.3 arcsec20 s2 s29 Gb DESIR : Infra-red Telescope 35 ≤ 1 ≤ 80  m 100≤ 2 ≤ 250  m Full Disk50 arcsec at 35  m 100 ms 5 Gb HEBS10-500keV 200keV-10MeV 10MeV-600MeV Full DiskFull disk1 s32 ms1.75 Gb

12 LYOT, SFSA, Juillet Mission Requirements (1) Continuous observations : SS (6-18) orbit Altitude : 650 – 750 km (radiation belts vs. geocorona) TM : compatible with continuous imaging at 10 s rate (+ compression) : ~ 35 Gbits/day Power : 100 W Volume : ~ 60*60*30 cm 3

13 LYOT, SFSA, Juillet Mission Requirements (2) P/L mass :< 70 kg Sun-pointed stabilized platform Pointing stability : 0.4 arcsec/s for LYOT ; with a dedicated internal P/L servo mechanism, a platform stability of 36 arcsec/s is OK. Pointing accuracy : 30 arcsec Roll of the S/C (polarization measurements) : ~ twice a week

14 LYOT, SFSA, Juillet Mission Requirements (3) Duration : 2 years minimum; 3 optimum Time : ASAP after solar maximum of cycle 24 « scheduled « for ? Operations : no special requirement but internal reactivity to events (flag signal thru an Internal Data Handling Processor; mass memory ~16 Gb) Data available ASAP to the community through SMC

15 LYOT, SFSA, Juillet Situation du projet Proposition LYOT : avril 2000 (7 ans déjà …) Prospective CNES : > 2004 Mars-Septembre 2006 : Phase 0/A Septembre 2006 – Juin 2007 : Phase A PRR : 7 juin 2007 Steering Committee : 6 juillet 2007 Phase B en 2008 ? Lancement en ? Cf. le calendrier solaire

16 LYOT, SFSA, Juillet SMESE and the Sun’ calendar (courtesy D. Biesecker, 2007) ?

17 LYOT, SFSA, Juillet LYOT

18 LYOT, SFSA, Juillet

19 LYOT, SFSA, Juillet The SMESE French-Chinese Team China: PMO : Purple Mountain Observatory, CAS NJU : Nanjing University CSSAR : Center for Space Science and Applied Research (Beijing) NAOC : National Astronomical Observatory, CAS (Beijing) CNSA : Chinese National Space Agency France : LESIA/OP : Laboratoire d’Etudes Spatiales et d’Instrumentation en Astrophysique (Paris Observatory) IAS : Institut d‘Astrophysique Spatiale (Orsay) CNES : Centre National d‘Etudes Spatiales Collaborations with other Institutes (LAM, LPCE, Torino/Firenze, CSL, ORB, RAL, SSL, Brazil, GSFC...)

20 LYOT, SFSA, Juillet /06/2007SMESE PRR - LYOT Instrument20 LYMAN ALPHA CORONAGRAPH IMAGER (LACI) OPTICAL DESIGN Raytracing LACI A. Millard


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