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Solar Oscillations Instrument at an Infrared Wavelength of 1.6 μm at Yunnan Observatory

  • Li Rufeng (a1), Ye Binxum (a1), Chen Hailin (a1), Liu Shaohua (a1), Deng Bailian (a1), Ma Jagu (a1), H. A. Hill (a2) and P. H. Oglesby (a2)...

Abstract

A photometric solar seismograph, as part of an international network, was installed at Yunnan Observatory, the Chinese Academy of Sciences, and put into operation in the spring of 1991. This instrument is used to detect solar oscillations by measuring the continuum radiation intensity on the solar disk with a spatial resolution of 50 arcsec, in heliocentric coordinates, for research on p-modes and g-modes when l < 50, where l is the angular degree of the eigenfunction. The solar oscillations can be observed simultaneously at two wavelengths of the detector with a sensitivity of 10 of the average intensity. This paper reports on the optical system of the instrument. Also introduced in this paper is the compensation system for the noise signals produced by the changes in the transparency of the Earth's atmosphere. This is based on solar photometry at wavelengths of 0.55 mm and 1.6 mm.

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References

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Deubner, F. L.: 1975, Astron. Astrophys. 44, 371.
Grec, G., Fossat, E., and Pomerants, M. A.: 1983, Solar Phys. 82, 55.
Hill, H. A., and Rosenwald, R.: 1986, NATO Advanced Workshop, Logan, Utah Proceedings.
Hill, H. A., Stebbins, R. T., and Brown, T. M.: in Sanders, J. H. and Wapstra, A. H. (eds.), Atomic Masses and Fundamental Constants, 5, Plenum, New York, p. 622.
Leibacher, J. W., and Stein, R. F.: 1971, Astrophys. J. (Letters) 7, 191.
Leighton, R. B., Noyes, R. W., and Simon, G. W.: 1962, Astrophys. J. 135, 474.
Oglesby, P. H.: 1987, Ph.D. dissertation, University of Arizona.
Ulrich, R. K., and Rhodes, E. J.: 1977, Astrophys. J. 218, 521.

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