Nice 03/12/2008 THE HELIOSEISMOLOGY PROGRAM OF PICARD T. Corbard, O.C.A. T. Appourchaux, I.A.S. P. Boumier, I.A.S. B. Gelly, THEMIS R.A. Garcia, S.J. Jiménez-Reyes, J. Provost, T. Toutain, S. Turck-Chièze, et al

Nice 03/12/ Why? Scientific objectives 2.How? Helioseismic measurements with PICARD 3.Specifications (SODISM performances) Heliosismology with PICARD

Nice 03/12/2008 Why? Scientific objectives 1.Structure and dynamic of the nuclear core (limb helioseismology and integrated irradiance data ) 2.The solar Dynamo, tachocline and torsional oscillations (Intensity Medium-l program or "Macro Pixels" program) 3.Fundamental (f) modes and the solar radius

Nice 03/12/2008 Scientific objective 1 : Structure and dynamics of the nuclear core  The main interest of this part of the spectra is that these modes are more sensitive to the deepest layers that remain poorly known both in terms of their structure and their dynamic.  The knowledge of the solar core properties is crucial to understand the dynamical evolution of the Sun and Stars and to set new constraints on neutrino physics.  All the measurements that will be obtained by PICARD for helioseismology are for improving our knowledge of the low frequency domain of the solar oscillation spectra (low and intermediate degree modes).

Nice 03/12/2008 Garcia et al, 2007: core rotation up to 3-5 times that of the radiative region ? Tracking Solar Gravity Modes Talks from T. Appourchaux, D. Salabert / R. Garcia, G. Grec

Nice 03/12/2008 How? g-modes search with PICARD: take advantage of limb-amplification Toner et al This limb amplification is understood theoretically (Toutain et al. (1999)) and it has been observed for p- modes using MDI images and LOI guiding pixels. (Appourchaux et al. 96) PICARD will have a resolution and a stability allowing us to use this amplification factor for searching low frequency modes. 22 pixels PICARD Talk from J. Provost / T. Toutain

Nice 03/12/2008 limb-amplification Toner, Jefferies & Toutain 1999 Seismic Radius and f-modes: Talks from H.M Antia and S. Lefebvre Leaks problem: Talk from M.C. Rabello-Soares

Nice 03/12/2008 Scientific objective 2 : Solar dynamo, tachocline and torsional oscillations  One of the major challenges in solar physics is to understand the origin of the magnetic activity cycle of the Sun.  Helioseismology does not give direct access to the internal magnetic field strength but it is a very powerful tool to infer the internal rotation rate, and some useful information on the magnetic field can also be deduced from its predicted interaction with the observed velocity field.

Nice 03/12/2008 The internal Rotation Inverse Problem angular degree, l Frequency, mHz

Nice 03/12/2008 Tachocline Corbard, 1998  The tachocline is a thin shear layer at the interface between the convection zone and the radiative interior, in which it is likely that a strong magnetic field is built as a result of the dynamo Ω-effect  From the study of the tachocline properties (structure, extent, precise location and latitudinal shape) we can derive not only the precise profile of the rotational shear but also get some hints on the shape and strength of the magnetic field at this depth  The tachocline is sensed mostly by p modes with degrees 20 < l < 60 but higher modes are also needed for inversion. Tachocline

Nice 03/12/2008 Torsional Oscillations in the convection zone  When compared to the time averaged profile, angular velocity shows bands of enhanced rotation rate that migrate toward the equator during the increasing phase of activity  It is very likely that we have here a direct observation of the back reaction of the dynamo magnetic field on the rotational profile, from which the toroidal field originates within the tachocline  Allows us to constrain our models of the interplay between magnetic field and convection

Nice 03/12/2008 Scientific objective 2 : Solar dynamo, tachocline and torsional oscillations  Detecting modes up to l=250 and measuring frequencies and splittings should allow us to probe the tachocline and most of the convection zone.  All these objectives are also major objectives for SDO.  In this field SDO is expected to provide much better data with more resolution, better signal to noise ratio (in velocity)…  It is however interesting to have both Intensity and velocity signals and to have measurements from two different instruments Talk of T. Straus

Nice 03/12/ How? Helioseismic measurements with PICARD Instrument DataFilter [band] CadenceExposure time SODISM22" wide rings of 1" pixels across the limb nm [0.5] 2 mn8 s SODISM256x256 Images of 8" macro- pixels nm [0.5] 1 mn8 s PREMOSSpectral Irradiance 215 nm [7] 0.1s PREMOSSpectral Irradiance 268 nm [7] 10s PREMOSSpectral Irradiance nm [0.5] 10s PREMOSSpectral Irradiance nm [0.8] 10s PREMOSSpectral Irradiance nm [1.7] 10s SOVAPBolometric Measurements NA10s SOVAPTotal Irradiance NA3 mn10s PREMOSTotal Irradiance NA2 mn20s Helioseismology With Irradiance data: Talk of W. Finsterle

Nice 03/12/2008 Intensity Medium ℓ program of PICARD  Images 256x256 (8"x8" Macro Pixels) with non destructive compression and no Gaussian mask. 1mn Cadence. 77% DC expected. (very demanding for available TM. Higher resolution was favored against the possibility of Gaussian masking )  The pipeline is under development in collaboration with Sebastian Jimenez-Reyes based on the pipeline he developed for LOWL.  Tests are being performed using MDI intensity images corrected for limb distortion and provided by Cliff Toner  Heliosismology Quick look Software for the mission center have been devilered (Beta versions). Talk of D. Salabert Talk of C. Renaud

Nice 03/12/2008 l-nu diagram from 1-day MDI intensity 128x128

Nice 03/12/2008 l-nu diagram from 1-day MDI intensity 128x128

Nice 03/12/2008 l-nu diagram from 1-day MDI intensity 128x128

Nice 03/12/2008 l-nu diagram from 1-day MDI intensity 128x128

Nice 03/12/2008 l-nu diagram from 1-day MDI intensity 128x128

Nice 03/12/2008 l-nu diagram from 1-day MDI intensity 128x128

Nice 03/12/ x170

Nice 03/12/ x256

Nice 03/12/2008 l-nu diagram from 1-day MDI intensity 170x170 (no mask)

Nice 03/12/ x170 (Gaussian mask)

Nice 03/12/2008 Final Choice: 256x256 (no mask)

Nice 03/12/2008 Relative differences between destructive and non destructive compression

Nice 03/12/2008 OPERATIONAL MODE  Nominal: no satellite manoeuvres, no calibration phase, no physical events. Limb: 1 image every 2 minutes; MP: 1 image per minute. But: MP: LCO (4%), diameter (10%), FFL + FCO (0.14%), loss (0.27%)  duty cycle (MP) ~ 85.5%. (Limb loss estimated < 0.8%).

Nice 03/12/2008 NOMINAL MODE Thanks to CNES

Nice 03/12/2008 CALIBRATION MODES  Optical distorsion: - optics and CCD calibration; a 30 arsec-step roll of the satellite, once a month. - duration: 937 minutes (JPM; 22/10/2007)  loss of 2.2% of duty cycle  Stellar: - angular/pixel relationship calibration; pointing toward the barycenter of 2 stars, 4 times per year minutes per operation: 0.07% loss.

Nice 03/12/2008  Absorption: - line of sight crosses the Earth atmosphere at an altitude lower than 40 km; a several-day period twice a year (just before and after the night mode). - 9 minutes at maximum, for each orbit, during which a single wavelength wide limb will be measured. 10 days  0.2%.  Night: - eclipses (Sun hidden by Earth); 3 months once a year. - 2 phases in the perturbation: night itself (maximum of 18 minutes per orbit for a 700-km altitude), and a thermal reequilibrium after the satellite left the shadow (14 minutes at maximum). MODES CONSTRAINED BY THE EPHEMERIS

Nice 03/12/ km scenario Limb: loss = 3.5 % MP : loss = 6.2 %

Nice 03/12/2008 Observational window operating modes: nominal, eclipses, calibrations (stellar, distorsion, …) Limbe Hélio : duty cycle = 93 %

Nice 03/12/2008 Macropixels : duty cycle = 78 % 50 mn aliases

Nice 03/12/2008 Macropixels : haute fréquence In principle OK, but be careful in case of large excursions of the signal (from the mean)

Nice 03/12/2008 Specifications – instrumental noise Sampling 3 years  10 nHz resolution for a 100 μHz peak (limb): 100 ppm for a 3 mHz peak (MP): 3 ppm  maximum drift over the whole mission: ~ ppm drift compensation of the on-board clock: once a week: < 80 ms

Nice 03/12/2008 simulations with systems input; a 1 ms jitter on the 1-minute sampling + 20 ms/week trend + systematic errors + margins. Redistribution of the spectral energy of sinewaves < 10 -3

Nice 03/12/2008 Specifications – instrumental noise Sampling 3 years  10 nHz resolution for a 100 μHz peak (limb): 100 ppm for a 3 mHz peak (MP): 3 ppm  maximum drift over the whole mission: ~ ppm drift compensation of the on-board clock: once a week: 80 ms at maximum Note: reference time is TUC, not TAI  leap second possible No trouble for peak detection but, be careful in case of phase difference analysis and cross-correlation with contemporaneous data (SDO, SoHO).

Nice 03/12/2008 Photometry (Integration*gain) A tenth of solar noise  σI/I ~ 9 ppm If only shutter noise: σt ~ ms

Nice 03/12/2008 Integration time: simulations of a 50  s (sigma) shutter noise White noise level: ppm 2 /  Hz, OK ! If necessary, possibility of reducing this level by a factor 5 using the measure of the integration time sinewaves amplitude: from 1 to 10 ppm

Nice 03/12/2008 Pointing Modeling  0.1 stability during the integration time (fine pointing by SODISM) Digitization Modeling  14 digits are OK.

Nice 03/12/2008 Conclusion  Performances seem OK; many thanks to the project team (CNES + labs).  Algorithms strategy (gap filling for MP ?)  Modelling for scientific interpretation + inversion  Coordination of the collaboration with SDO  Working groups in charge of: - In flight performances validation - validation of each level of data  CO-I and G-I proposition to the CS