In the time interval 1749-1818 a great part of missing daily relative sunspot numbers was reconstructed by nonlinear two-step method of interpolation. In the first step directly interpolated were gaps not longer than five days. In the second step the data were sorted in the so called Bartels scheme, i.e. in rows of a length of 27 days
subsequently ranged in a matrix. In thís step the missing data of longer gaps were interpolated columnwise, i.e. missing value at any position was interpolated from the data at same column positions of preceeding and folloving rows. The interpolation was limited to sequences of no more than four missing data. The procedure enables interpolate long gaps and simultaneously respect the 27-day variation of solar activity. A part of missing data in the intervals, where the frequency of observations was very low and has not fullfilled the limitations of the interpolation method. was
not interpolated. Annual tables of daily data are given in Appendix A, monthly and annual means in Appendix B, and annual plots of daily data in Appendix C. The differences between monthly and annual means of the primary observations and of the data completed by interpolation fluctuate around zero. The amplitude of fluctuations
depends inversely on the frequency of observations. Most conspicuous are the deviations in the time interval 1776-1795, when the frequency of observations was wery low or almost zero. The dispersion of monthly differences σ is ±13.7 R and
of annual differences ±9.3 R. The results give insight on the reliability of relative sunspot numbers in the investigated time interval. and Součástí článku jsou 2 apendixy:
- Appendix A Daily relative sunspot numbers 1749-1818
(s. 7-42)
- Appendix B Monthly and annual means of relative sunspot numbers 1749-1818 (s. 43-66)
The missing daily relative sunspot numbers in the time interval 1818-1848 were reconstructed by the nonlinear two-step method of interpolation. In the first step directly interpolated gaps were not longer than five days. In the second step, the data were sorted in the so called Bartels scheme, i.e. in rows of the length of 27 days
subsequently ranged in a matrix. The missing data of longer gaps were interpolated columnwise, i.e. the missing value at any position was interpolated from the data at the same positions of preceeding and following rows. The procedure enables to interpolate long gaps and simultaneously respect the 27-day data variation. The Appendix A contains annual tables of daily data, Appendix B gives monthly and annual means and Appendix C presents simutaneously annual plots of primary data and of those reconstructed by interpolation. The differences between the monthly and annual means of primary data and of data completed by interpolation are small and fluctuate around zero. Only in the time interval 1835-1842, when the frequency of observations was lowered, the amplitude of fluctuations is enhanced. The dispersion of monthly differences σ is ±4.3 R and of annual means ±1,1 R. The two-step method of interpolation was tested on the daily data series in the time interval 1918-1948. The sequence of missing daily data in the years 1818-1848 represents a masking function. The differences between the monthly and annual means of primary and modified data are small with fluctuations around zero and with dispersion σ for monthly differences ±2.7 R and for annual differences ±0.6 R. The small dispersion gives evidence about a high reliability of relative sunspot numbers derived from observations in the years
1818-1848 and also about the effectivity of the two-step method of interpolation. and Materiál obsahuje 3 (nestránkované) apendixy:
- Appendix A Daily relative sunspot numbers 1818-1848 [s. 6-22]
- Appendix B Monthly and annual means of relative sunsppot numbers 1818-1848 [s. 23-24]
- Appendix C Plots of daily relative sunspot numbers 1818-1848
[s. 25-56]
Observations of the total radio flux of the Sun are presented for the period 1962-1986, ciovering two 11-year cycles of solar activity, -i.e. nos 20 and 21. Daily averages of the radio fluxes for the period in question are used for graphical and numerical representation. The minimum values fo the total radio flux of the Sun of wavelength 115 cm (260 MHz), corresponding to the solar activity minima in 1964, 1976 and 1986 are given.