Download Problems of Solar and Stellar Oscillations: Proceedings of by D. O. Gough (auth.), D. O. Gough (eds.) PDF
By D. O. Gough (auth.), D. O. Gough (eds.)
D. O. GOUGH Institute of Astronomy. Madingley highway. Cambridge. U. okay. IAU Colloquium sixty six on 'Problems of sun and Stellar Oscillations' was once held on the Crimean Astrophysical Observatory, U. S. S. R. , on 1-5 September, 1981. The significant objective of the colloquium used to be to check the low-amplitude oscillations of the solar and, to a lesser volume, to think about comparable oscillations of alternative stars. a lot of the emphasis of the discussions was once at the diagnostic worth of the oscilla tions. within the previous couple of years we've turn into acutely aware that the frequencies of the five-minute modes of excessive measure, which represent the foremost part of the oscillations found 20 years in the past through Evans and Michaud, can be utilized to place particularly tight bounds at the stratification of the sun convection sector. those allow a calibration of sun versions computed from so-called normal evolution concept. Modes of low measure penetrate underneath the convection quarter to the center of the solar, and will in precept try out the evolution idea. hence there has been enormous curiosity within the stories of the newest observations of such modes. frequently, these observations make certain the cali bration by means of the high-degree modes, yet there stay a few systematic discrepancies that call for a few revision of the idea. in addition to the gross elements of evolution idea, there also are extra problematic info to be understood.
Read or Download Problems of Solar and Stellar Oscillations: Proceedings of the 66th IAU Colloquium held at the Crimean Astrophysical Observatory, U.S.S.R., 1–5 September, 1981 PDF
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Additional resources for Problems of Solar and Stellar Oscillations: Proceedings of the 66th IAU Colloquium held at the Crimean Astrophysical Observatory, U.S.S.R., 1–5 September, 1981
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1979, 1980) have helped to obviate the first two problems. The third has not yet been solved. This report is of a more detailed analysis of the observations. We start the analysis by combining the observations obtained at the Stanford Solar Observatory (for the observational arrangement see Scherrer et al. (1983» during the summers of 1977 through 1980 with those obtained at the Crimean Astrophysical Observatory by V. A. Kotov, A. B. Severny, and T. T. Tsap during the summers 1974 through 1979.
The weighting function has been chosen to minimize the effects of seeing on the edge location, yet remain sensitive to changes in the limb darkening. Roughly, the weighting function measures a second derivative averaged over the interval. The behavior of the FFTD is documented by a well developed theory and empirical tests. The FFTD has been previously implemented as part of the telescope requiring the choice of a single interval size. However, the FFTD can be employed more effectively for oscillations studies if multiple definitions with different intervals can be applied simultaneously.
The South Pole has received considerable attention as a site where extended observations might be possible. Currently, the Sacramento Peak program is developing a South Pole telescope designed for the observing technique and data analysis proven in Sunspot. A review of pertinent South Pole site parameters is given here for other workers who may be considering South Pole observations. Observing sequences longer than 150 hr are possible, though rare. Data sets of this duration are very attractive for solar oscillation studies.