Observations of solar oscillations with periods of 160 minutes

Scherrer, P. H.; Wilcox, John M.; Kotov, V. A.; Severny, A. B.; Tsap, T. T.

doi:10.1038/277635a0

Cited by 59 publications

(25 citation statements)

References 2 publications

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“…Figs.l and 2 of Scherrer et al(1979) show in more detail the very close phase correlation holding between the Crimean and the Stanford observations over the past three years, leading to a precisely determined period of 160.OlO min which slightly but significantly differs from an integer fraction of 1/9 of a day. Severny et al(1978) illustrates a correlation observed between the infrared brightness of the disk and the velocity signal found by Koutchmy and Kotov, revealing fluctuations of the solar limb darkening function with a relative amplitude of 2.5xlO~4, being practically in phase with the velocity.…”

Section: Disk Observationsmentioning

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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Section: Disk Observationsmentioning

confidence: 99%

Global Oscillations of the Sun

Deubner

1980

Highlights astron.

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“…They analysed differences in the solar radial velocity recorded at disc centre, and further out toward the limb. Observations were made at the Stanford Solar Observatory (Scherrer et al 1979), and at the Crimean Astrophysical Observatory (Severnyi et al 1976). The length of the time series was 105 days, but with a duty cycle of only 10%.…”

Section: Radial Velocitymentioning

confidence: 99%

The quest for the solar g modes

Appourchaux

Belkacem

Broomhall

et al. 2010

Astron Astrophys Rev

125

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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“…Oscillations of the Sun with the period of 160 first observed in Crimea in 1974 and described in a set of papers by Tsap (Severny et al 1976, 1978;Kotov et al 1978) were observed also by Brookes et al (1976) and have been afterwards observed during the last three years in Stanford (Scherrer et al 1979) and Kitt Peak (Snider et al 1978). This fact excludes possible instrumental origin of the effect.…”

mentioning

confidence: 88%

Solar Pulsations

1980

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Oscillations of the Sun with the period of 160 first observed in Crimea in 1974 and described in a set of papers by Kotov, Severny and Tsap (Severny et al. 1976Kotov et al. 1978) were observed also by Brookes et al. (1976) and have been afterwards observed during the last three years in Stanford (Scherrer et al. 1979) and Kitt Peak (Snider et al. 1978). This fact excludes possible instrumental origin of the effect. Moreover, the phase coherence (after elimination of integer number of 160 -periods) between these four observatories makes the assumption of Earth atmospheric origin of the oscillations (Fossat and Grec 1978) very unlikely. Besides that, (1) the dependence of amplitude of oscillations on the phase of solar rotation and (2) slow, synchronous (at Crimea and Stanford) drift of the phase of maximum from year to year, pointing to a true period slightly higher 160 (160 0.1), make the "telluric hypothesis" of the effect completely inconsistent. In Figure 2 we see the dependence of amplitude of the oscillations versus the phase of solar rotation. Figure 3 shows the yearly drift of phase of the velocity maximum according to our (C) and Stanford (S) observations. The regression line on this graph leads to the period P = 160 m .010. This period is too long for purely radial pulsations of a standard model adopted at the present time. It would be in good agreement with the period of such pulsations for an almost homogeneous sphere (polytrope n ~ 0.5), but such a model would not produce the observed luminosity and would possess Rayleigh-Taylor instability. It is well known, as was pointed out by Cowling, that quadrupole oscillation described by spherical harmonics % = 2 in the case of a fluid sphere has a period 186 . Christensen-Dalsgaard, Dilke and Gough showed that 453

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Observations of solar oscillations with periods of 160 minutes

Cited by 59 publications

References 2 publications

Global Oscillations of the Sun

Global Oscillations of the Sun

The quest for the solar g modes

Solar Pulsations

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