No abstract available

[en] The following characteristics of the proportional counter carried on No. 3 scientific satellite ''Taiyo'' for the observation of solar soft X-ray (1 to 2A) are described: (1) incident X-ray intensity vs. pulse height characteristic, (2) incident X-ray intensity vs. pulse pile-up characteristic. The effect of these two is neglected in weak X-ray measurement, but can not be neglected in the measurement of strong X-ray such as solar X-ray. The incident X-ray intensity vs. pulse height characteristic is a phenomenon that the pulse height decreases as the incident X-ray intensity increases. This characteristic is theoretically discussed quantitatively and compared with experimental results. It seems to be in good agreement. The incident X-ray intensity vs. pulse pile-up characteristic is a phenomenon in which the pulses made by two photons simultaneously came into the detector are superposed and observed as if one higher energy X-ray came in. The quantitative consideration on it also well explains the analysis of experiments. This is also confirmed by the fact that a few results obtained in the experiment using ⁵⁵Fe X-ray well agrees the results of numerical integration of 6 keV incident X-ray pulses by reading it on an oscilloscope and using distribution function. The above examination will be applied to the analysis of data obtained from the proportional counter carried on the satellite ''Taiyo''. (Wakatsuki, Y.)

[en] In No. 3 scientific research satellite ''Taiyo'' for studying the organic connection of the ionosphere and the magnetosphere, SXR was intended to observe solar high-energy soft X-ray. The satellite on its orbit over 1.000 km above the earth enters the Van Allen radiation belt, where high energy particles as the background interferes with the observation. During the orbiting of 'Taiyo' for about an year since 1975, the intensity distribution of high energy particles (Electrons and protons) in lower Van Allen radiation belt was able to be observed. The results of the observation are described. (Mori, K.)

[en] Five times of the simultaneous observation of visible light and hard X-ray of Sco X-1 were performed from 1970 to 1972 in India. The observation is reviewed, and a few problems on Sco X-1 are discussed in association with the observed results. The thermal radiation from several keV to 40 keV emitted from Sco X-1 has been observed. The photon scattering by electrons is an important process in hot and high density plasma causing it. From the theoretical investigation of the observed results, it is predicted that the physical parameters of the hot plasma vary with the variation of the intensity of visible light and X-ray. Especially, the plasma density increases at the time of the flare of visible light and X-ray, and the photon scattering by electrons becomes more important. It results in the variation of the spectrum of thermal radiation. (Yoshimori, M.)

No abstract available

[en] The correlation between photons and X-ray was studied by using the data taken by the satellite Hakucho. Among soft transient X-ray sources, Cen X-4 and Aq1 X-1 emit the type 1 X-ray bursts. The correlation between photons and X-ray from these stars was good. The properties of X-ray bursters and bulge sources can be investigated by Sco X-1. The X-ray bursts of MXB 1636-536 were observed together with photons in 1979 and 1980. The profiles of photons and X-ray were similar mutually. The bursts of photons were delayed by a few second as compared to the X-ray bursts. The delay time of each burst was not a constant. The temperature of light in the bursts varied in the range between 2 x 10⁴ and F7 x 10⁴ K.F The photons may be emitted through the reprocessing of gas by X-ray. The simulataneous observations of photons and X-ray of Cyg X-1 and GX 339-4 were performed. The mode of emission of photons and X-ray depended on the stars. Most of photons were emitted by the reprocessing, however, some of photons were emitted by other processes. (Kato, T.)

[en] We propose a new concept of X-ray microscopes with a coded aperture imaging mask. This makes use of X-ray images through many pinholes, but requires neither reflection nor diffraction properties of X-rays. When an object is irradiated by a diffuse X-ray source, many objects images geometrically enlarged through coded holes can be deconvoluted to one image. The precision of the image is dependent on the size of each pinhole. The material and thickness of the coded mask constrain the energy of available X-rays for the present X-ray microscope. (author)

[en] The x-ray spectrum of the Orion Nebula derived from observations made with the gas scintillation proportional counters onboard the Tenma satellite is described. The continuum spectrum is fitted well with a thermal bremsstrahlung model with kT = 3.7 ± 0.3 keV. An x-ray emission feature at energy of 6.69 ± 0.06 keV having equivalent width of 640 ± 120 eV, which is attributed to transitions of Fe xxv ions, is clearly detected in the spectrum. It is suggested that the x-ray emission comes from an optically thin hot plasma at temperature of 4 x 10⁷ K. Possible origins of the high-temperature thermal component are briefly discussed. (author)

[en] We present the results of a four day observation of the Seyfert galaxy NGC 4151 by Ginga. The level of the X-ray continuum shows slow drifts on timescales down to ∼0.5d, a mode of behaviour which appears to be characteristics of this object. There is also evidence for a significant, albeit small, change in softness ratio over the course of the observation which we attribute to a random variation in the effective line-of-sight column density. The soft X-ray excess reported in earlier measurements remains a feature of the X-ray spectrum of NGC 4151 and we consider the competing models of this component. Combining the Ginga results with earlier satellite measurements we find that the effective iron abundance as determined from the depth of the 7.1-keV edge feature is 1.8±0.2 and that the intensity of the 6.4-keV iron line has remained close to 2.2±0.2 x 10^-4 photons cm^-2s^-1 over a period of several years. (author)

[en] Four long X-ray bursts were observed from GX 17 + 2 in 1981 and 1982. Their profiles are characterized by the rise times of about 1.5 s, durations of 3-15 min, burst peak flux values somewhat smaller than the persistent flux values, and spectral softening in the tails. No other bursts were observed from Hakucho pointings on this source in 27d in 1981-1982. The uniqueness of these bursts in comparison with many other bursts is described. (author)