PICARD: Simulataneous measurements of the solar diameter, differential rotation, solar constant and their variations

Damé, Luc; Hersé, M.; Thuillier, G.; Appourchaux, T.; Crommelynck, D.; Dewitte, Steven; Joukoff, A.; Fröhlich, C.; Laclare, F.; Delmas, Christian; Boumier, P.

doi:10.1016/s0273-1177(99)00502-5

Cited by 21 publications

(13 citation statements)

References 10 publications

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“…The PICARD mission, due for launch in late 2009 (Damé et al 1999), will be sensitive not only to the displacement, but also to intensity fluctuations induced by temperature perturbations, like those detected by with the VIRGO/LOI or by Toner et al (1999) with SOI/MDI. PICARD will have the capability of making observations of displacement and intensity fluctuations at the limb of the Sun, where the perturbations appear to have higher amplitude than those observed in the disc.…”

Section: Observablesmentioning

confidence: 99%

“…Toner et al (1999) showed that the oscillation signal increases as the distance to the limb decreases. This property will be used by the SODISM instrument on the PICARD mission to try to detect modes at the limb (Damé et al 1999;Corbard et al 2008). Thomson et al (1995) used magnetic field and particle data collected by the Ulysses mission.…”

Section: Solar Diametermentioning

confidence: 99%

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The quest for the solar g modes

Appourchaux

Belkacem

Broomhall

et al. 2010

Astron Astrophys Rev

127

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A ce compte, toutes les sciences ne seraient que des applications inconscientes du calcul des probabilités ; condamner ce calcul, ce serait condamner la science tout entière." "From this point of view all the sciences would only be unconscious applications of the calculus of probabilities. And if this calculus be condemned, then the whole of the sciences must also be condemned."Henri Poincaré, 1914, La Science et l'hypothèseAbstract Solar gravity modes (or g modes) -oscillations of the solar interior for which buoyancy acts as the restoring force -have the potential to provide unprecedented inference on the structure and dynamics of the solar core, inference that is not possible with the well observed acoustic modes (or p modes). The high amplitude of the g-mode eigenfunctions in the core and the evanesence of the modes in the convection zone make the modes particularly sensitive to the physical and dynamical conditions in the core.Owing to the existence of the convection zone, the g modes have very low amplitudes at photospheric levels, which makes the modes extremely hard to detect. In this paper, we review the current state of play regarding attempts to detect g modes. We review the theory of g modes, including theoretical estimation of the g-mode frequencies, amplitudes and damping rates. Then we go on to discuss the techniques that have been used to try to detect g modes. We review results in the literature, and finish by looking to the future, and the potential advances that can be made -from both data and data-analysis perspectives -to give unambiguous detections of individual g modes. The review ends by concluding that, at the time of writing, there is indeed a consensus amongst the authors that there is currently no undisputed detection of solar g modes.

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Section: Observablesmentioning

confidence: 99%

Section: Solar Diametermentioning

confidence: 99%

The quest for the solar g modes

Appourchaux

Belkacem

Broomhall

et al. 2010

Astron Astrophys Rev

127

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“…it means that a p-mode with an amplitude of 1 ppm in full disk is observed with an amplitude of 4 ppm at the limb (cf. Damé et al, 1999). Analyses of Toutain et al (1999) and Toner et al (1999) confirmed such an amplification factor of 5.…”

Section: Oscillationsmentioning

confidence: 88%

A solar diameter metrology measurement: the Picard microsatellite program

Damé¹,

Brun²,

Cugnet³

et al. 2017

International Conference on Space Optics — ICSO 2000

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“…PICARD satellite (Damé et al, 1999) will be launched in 2009 and it is expected to get a milliarcsecond accuracy in the solar radius variations.…”

Section: Secular Variations Of Solar Radiusmentioning

confidence: 99%

Solar Radius Variations Measured in Central Eclipses

Sigismondi¹

2008

AIP Conference Proceedings

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Abstract. Data on Baily beads observed in total eclipse of March 29, 2006 (Egypt) and those of annular eclipses of September 22, 2006 (French Guyana) and October 3, 2005 (Spain) are used to evaluate the variations of solar radius with respect to its standard value during a whole draconitic year. A portable observatory has to be set on the shadow limit of central eclipses, where lunar limb is grazing to the solar one and the number of beads is large. The observation of solar corona during Egyptian eclipse for several minutes during maximum eclipse on shadow's limits is studied in parallel with the eclipse observed by Clavius in 1567. From fall 2005 to fall 2006 the solar radius does not show significant changes (0.00 to -0.01 arcsecs) with respect to its standard value of 959.63 arcsec within errorbars of 0.17 arcsecs. This is its value at minimum of cycle 23 of solar activity.

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PICARD: Simulataneous measurements of the solar diameter, differential rotation, solar constant and their variations

Cited by 21 publications

References 10 publications

The quest for the solar g modes

The quest for the solar g modes

A solar diameter metrology measurement: the Picard microsatellite program

Solar Radius Variations Measured in Central Eclipses

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