Influences of the change of the solar activity upon the meteorological phenomena are investigated. The solar influences on the general circulation appears distinctly 2 months after the maximum of monthly mean sunspot number; anomaly of monthly zonal mean at 500 mb height increases in high latitudes and decreases in low latitudes. By means of harmonic analysis for the sunspot number, solar constant, zonal index at 500 mb height, and air temperature at Tokyo, it is found that a 4.8-month periodicity in these elements is statistically significant and they are stable. Concerning the 4.8-month periodicity, it is found that
(1) Phase angles for the sunspot number are equal to the ph ase angles for the zonal index. This equivalent to saying that time change of the sunspot number and the zonal index are parallel to each other.
(2) Phase angles for the solar constant are equal to 90° plus phase angles for the zonal index.
Results of the harmonic analysis for the zonal mean 500 mb height anomaly at each latitude show that there is a modal line at about 50°N, that is, the height anomalies on both side of the line are in negative correlation.
Next, solar influences are investigated by using 5-day mean values of various elements, such as 10 km wind speeds at Tateno and 500 mb height at 70°N 120°E and 60°N 150°E, and they are found to be statistically significant. The composite maps of the difference of 5-day mean 500 mb height anomaly over the northern hemisphere at sunspot maximum and minium are calculated. The pattern on the composite map is similar to the pattern of the anomaly of normal 500 mb height from zonal mean.
Solar in f l uences are also analysed by using 25-day periodicity in the meteorological elements and the index of the solar activity. Distribution of the phase angles of these periodicities for 500 mb height anomaly of the northern hemisphere shows that wave number 2 in the westerlies is sensitive for changes in the solar activity. An empirical rule that meridional components of the general circulation intensify after the increase of the solar activity is derived from these analyses. This rule harmonizes with the analysis of the solar influences on the meteorological phenomena made by many authors.
The present analysis concludes that the sunspot number is a better index than K-index for the detection of the solar influences on the atmosphere. This is inconvenient for the corpuscular theory. And the ultraviolet theory is found to be more reasonable.

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The random fluctuations of t he weather signals about the average value limit the accuracy of the information obtained from the signals. The averaged echo intensity will indicate a more accurate value than the non-averaged signal. This, paper describes the probability dis tribution of the averaged signal from the logarithmic I.F. amplifier indicating the relation of the averaged value, the peak value and the calculated value from the radar equation. The instrument whic h produces an averaged iso-echo contouring PPI using a quartz delay line is briefly mentioned.

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A new ozone station was established in Kashmir (34°N) in 1955 in a region where double tropopauses are frequent in winter and spring. In this paper, a comparison is made of the ozone amounts measured at Delhi (28¹/₂°N) and Srinagar (34°N) in India and at Tateno (36°N)in Japan in 1957-58. The ozone amounts at Tateno are much larger than at Srinagar although the latitude of Tateno is only 2° greater than that of Srinagar. It is recalled that at Zi-Ka-Wei and Cairo, which are at lower latitndes than Srinagar, significantly higher ozone values had been recorded in winter. It is thus evident that there is a large geographical influence on the total ozone amount measured at a place. Apparently, the Himalayas and the Indian summer monsoon exert a strong depressing influence on the ozone amount south of the Himalayas and incursions of the cold Siberian anti-cyclone tend to bring with it larger amounts of ozone over China and Japan.
The seasonal variation of ozone over N. India was o f an unusual character in 1957.

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The heat production in the earth's upper atmosphere due to the collision between the air atoms and the solar corpuscular radiation is discussed. The fundamental processes are treated semi-classically to get approximate formulae for the quantitative discussion. The atmospheric model given by Miller is employed to get the numerical values of the atmospheric elements. The intensity and the energy spectra of solar corpuscular radiation at the top of the atmosphere are estimated from the recent rocket measurements. About sixty per cent of the total energy loss of primary radiation is transformed into thermal energy for the heating of the atmosphere. The vertical profile of the heating rate is sensitively affected by the energy spectra of the primary radiation.

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A new simple current meter is presented which will record both the current speed and its direction on two smoked glass plates. Experiments in the field show that the vertical profiles of ocean currents can be determined successfully and rapidly. Some theoretical considerations are applied to the above current profiles, and the magnitudes of the order of the surface and bottom frictions at low wind velocities are estimated to be about 0.4 and 1.0 g/cm/sec².

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[in Japanese]

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