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Results of rocket observations of SCO X-1 over the spectral range of 2∼20 keV are presented. The observations have been performed partly in India and partly in Japan under the collaboration of the three groups. The present results are compared with results of similar observations carried out by the LRL (Lawrence Radiation Laboratory) group. Some of these X-ray observations were accompanied by simultaneous optical observations. Relationships between the hardness of the X-ray spectrum and the X-ray intensity and between the hardness and the optical luminosity are compiled. The relationships among the parameters (temperature, density and size) which characterize the postulated isothermal cloud model of SCO X-1 are given. They indicate that SCO X-1 is characterized by a temperature of about 107–108K, a density of about 1016–1017 cm−3 and a radius of about 108–109 cm respectively. We further show that the temperature is inversely correlated with the size of the source; an increase in temperature corresponds to a decrease in the radius and an increase in density.

繊維の密度-水分率曲線から,(p+c) を求める式を導いた。ここにpは繊維内部 (有機媒質の浸入しない部分) の吸着水と全吸着水との質量比で, cは繊維1gあたりの外部 (有機媒質の浸入する部分) 吸着水の容積収縮に自由水の密度をかけたものである。木綿, レーヨン, 羊毛, 絹および合成繊維について,(p+c) と水分率との関係を求め, これらの繊維の吸湿性について論じた。さらに, 水中で測定した密度について論じ, cはpに比してかなり小さいことを結論した。

I shall review recent observational results on discrete X-ray sources and on the diffuse background component. Thus far, approximately forty sources have been reported. It is to be noted that the sources can not be classified in only one or two categories and that there are a variety of the sources. Figure 1 shows the situation.

酢酸繊維素繊維および皮膜の吸湿による密度の変化を有機媒質を用いて浮沈法で測定し, さらに水中の密度も測定した。他の繊維の場合と同じように, 密度は数%の吸湿量で極犬を示す。これらの結果から, 試料内部 (有機媒質の入れない部分) の吸湿量pと全吸湿量xの関係を求めた。三酢酸繊維素繊維 (酢化度61.8%) は二酢酸繊維素繊維 (酢化度54%) よりpが少ない。これは前者の結晶化度が高いためであろう。未処理の三酢酸繊維素皮膜 (酢化度60.5%) は二酢酸繊維素皮膜 (酢化度54.7%) とほとんど同じpの値をもつ。これは両皮膜が似た結晶化度をもつためであろう。また, 繊維, 皮膜とも, p-x曲線は徐々に飽和値まで増大する。

The apparent molal volume of amino acids in aqueous solutions increases with the ionic strength of other simple ions. The relation between molal volume and ionic strength was explained according to Kirkwood's theory. From the fact that this relation is equal for various α-amino acid, it was concluded that the hydration of hydrocarbon part was not accompanied with the electrostriction. Thus the two kinds of hydration are epxected for amino acids, or, more generally, for all water-soluble organic substances.

ビニロン製造工程中の3種類のポリビニルアルコール繊維 (D. P. 1600, 3d), すなわち未処理のもの (A), 熱処理したもの (B), およびさらにホルマール化したもの (C) について, 吸湿による密度の変化を浮沈法により測定した。吸湿量0のA, B, Cの密度は25℃でそれぞれ1.298, 1327, 1, 2789/ccであった。密度一吸湿量の関係でA, Bは吸湿量約2%のところに密度の極大があり, 吸湿量の増えるに従って徐々に密度が減少する。しかしCには極大がないようで, また密度の減少する勾配がA, Bより急である。これらの挙動はポリビニルアルコール繊維の吸着水について若干の示唆を与える。

The present status of observations of the diffuse cosmic X-rays is discussed. The energy spectrum in the energy range 1–100 keV has been well established. The flux around 0.25 keV appears to be rather high. The basis of the classical argument that the integration of normal galaxies in the universe is not sufficient to explain the diffuse X-ray flux is re-examined. Recent observations around 0.25 keV are discussed and results are compiled.

We performed a couple of balloon experiments to measure the size and the location of Cyg-X-1 using the techniques of the modulation collimator [1]. The angular periods of the modulation collimator were 26′ and 10′ for the respective flights corre­sponding to the approximate angular resolutions of the size determination and location, 3′ and l′ respectively. Preliminary results of the experiment with 3′ resolution are reported here.*

Modulation collimators have been used in recently reported work to determine the angular sizes and celestial positions of the X-ray sources Sco X-1 and Taurus XR-1 (Crab Nebula) with precisions of 15″ to 30″. The measurements were made by means of four-grid collimators, star photography and optical imaging of the collimators. In the present paper we discuss (1) the principles and uses of various forms of the modulation collimators as they pertain to X-ray astronomy, (2) several methods for determining the celestial positions of X-ray sources with these collimators, (3) the techniques for the alignment and calibration of these detection systems, (4) an image-forming collimator, and finally, (5) some of the optical properties of these grid systems. The modulation collimator is quite versatile and is particularly suited for measurements from spacecraft with relatively poor pointing capability. Thus it should be a useful tool in X-ray astronomy for some years to come.

THE purpose of this article is to present a preliminary report on a new cosmic X-ray source. The source was observed near Sco X-1 during recent rocket flights to observe Sco X-1 simultaneously with ground-based optical telescopes. It is very likely that we observed the source reported to have appeared between July 6 and July 9 by Conner et al. in an IAU telegram issued on July 30, 1969.

Angular diameters of X-ray source regions in Scorpio and Sagittarius constellations by rocket measurement with collimator

Collimator with wide fields of view detectors designed for extraterrestrial X-ray source measurements

X-ray source in Crab Nebula size and position, showing visible light distribution having common center within 15-inch precision of measurement and finite angular extent

THE discovery of galactic X-rays by Giacconi et al.1, confirmed by Friedman et al.2, which was quite unexpected from our present understanding of physical processes in astronomical objects, has induced a variety of theoretical investigations3. Among various mechanisms so far proposed to explain the X-ray sources, the neutron-star hypothesis suggested by several authors4 seems to present a reasonable combination of the radiative power, the distance, the life and the frequency of occurrence of the X-ray sources although the existence of neutron stars is still open to question.

Optical identification of position of X-ray astronomical source Sco X-1, noting similarity of certain properties with old novae