SCLERA: an Astrometric Telescope for Experimental Relativity

Oleson, James R.; Zanoni, C. A.; Hill, H. A.; Healy, A. W.; Clayton, Paul D.; Pätz, Daniel

doi:10.1364/ao.13.000206

Cited by 14 publications

(3 citation statements)

References 4 publications

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“…For instance a putative g-mode amplitude of 1 mm s −1 at a frequency of 100 µHz would induce a peak-to-peak variation of 4.3 µarcsec as seen from the Earth, whereas for a p-mode amplitude of 30 cm s −1 (at a frequency of 3000 µHz) would induce a variation of 43 µarcsec. In the 1970's, the SCLERA 15 instrument was used in an attempt to detect p modes and g modes alike (Oleson et al 1974;Hill 1985Hill , 1992. The detection of displacement was performed by observing the change in diameter of the Sun (Brown et al 1978), and signals with typical amplitude of the order of 5 marcsec were observed.…”

Section: Observablesmentioning

confidence: 99%

The quest for the solar g modes

Appourchaux

Belkacem

Broomhall

et al. 2010

Astron Astrophys Rev

124

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%

The quest for the solar g modes

Appourchaux

Belkacem

Broomhall

et al. 2010

Astron Astrophys Rev

124

127

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“…Most of the results discussed in this section were obtained from data acquired with an instrument, originally designed to measure the deflection of starlight by the sun (Oleson et al, 1974). At the Santa Catalina Laboratory for Experimental Relativity by Astrometry (SCLERA) the solar diameter measurements consist of accurately referenced scans available at https://www.cambridge.org/core/terms.…”

Section: Measurements At the Limbmentioning

confidence: 99%

Global Oscillations of the Sun

Deubner

1980

Highlights astron.

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The topic of this Joint Discussion has received enormously increased interest in the last couple of years, owing to its potential for the investigation of the structure of the interior of the sun, including related topics like the structure of the convection zone, solar metal abundance, and the still unsettled neutrino problem.The first stimuli came from the startling observations of Hill et al. (1976) in Arizona, Severny et al. (1976) on Crimea, and Brookes et al. (1976) in Birmingham, accompanied by a large volume of theoretical papers, the details of analysis of which soon went beyond the actual status of the observational facts.We then witnessed, however, the success of considerable refinements of the techniques of observation, together with an obvious widespread temptation to push the interpretation of many of the new results to the limits of optimism. Yet, despite of the still increasing body of data suggesting the reality of the solar origin of the observed phenomena, much scepticism was prompted by the complicated statistics and the intricate numerical procedures involved in the data analysis, as well as by the great uncertainty about the significance and the amounts of “noise” contributed to the signal by electronics, changes of the conditions of the ray path within the telescope, terrestrial atmospheric inhomogeneities and solar quasi-stationary motions.

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“…The positions on the limbs are determined by the Finite Fourier Transform Definition (FFTD) (see Hill et al, 1975; and the relative changes in the edge separation recorded interferometrically. A detailed description of the data-taking procedure is found in these earlier works and a description of the facility is provided by Oleson et al (1974).…”

Section: Observationsmentioning

confidence: 99%

Detection of individual normal modes of oscillation of the Sun in the period range from 2 hr to 10 min in solar diameter studies

Bos

Hill

1983

Sol Phys

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New observations of solar oscillations are reported. Power density spectra derived from these observations reveal narrow-band oscillations that are spatially global, have spatial symmetry properties that are either symmetric or antisymmetric for reflection about the center of the solar disk and also about the solar equator, and have coherence times ~> 41 days. Large-scale differential refraction effects have been reduced by a factor of l0 S over that found in previous solar diameter studies by the design of the experiment; thus, these effects are eliminated as a possible source of the oscillations. A discussion is presented of this reduction as well as other features of the observing and analysis program. It is concluded that the probability is very high that individual normal modes of oscillation of the Sun have been detected in the period range, from 2 hr to 10 min.

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SCLERA: an Astrometric Telescope for Experimental Relativity

Cited by 14 publications

References 4 publications

The quest for the solar g modes

The quest for the solar g modes

Global Oscillations of the Sun

Detection of individual normal modes of oscillation of the Sun in the period range from 2 hr to 10 min in solar diameter studies

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