The hard solar X-ray burst of 18 September 1963

A hard solar X-ray burst was observed by J-P. Legrand on 18 September 1963, 13:56 UT, at balloon altitude. It lasted a few minutes; a steep increase was followed by an exponential decay. During its declining phase a weak radio burst was observed on 3 and 10 cm, not on longer wavelengths.Maximum radio intensity occurred two minutes after that of the X-ray burst. The X-ray and radio bursts ended almost simultaneously. Optically a small shortlived (some minutes) flare point occurred simultaneously with the X-ray burst in a magnetically interesting part of the active region of September 1963. The X-burst photons seem to have had an energy of about 0.5 MeV. The burst was therefore of a fairly rare type, since very few other bursts with similar photon energies have been detected up to now.It is suggested that a mass of gas, magnetically confined to a volume of about 5·10²⁵ cm³ in the low corona, containing about 3·10³⁵ electrons was accelerated to energies of about 0.5 MeV. The gas gradually expanded, partly also to higher levels. The gyro-synchrotron radiation, emitted by the plasma became observable after about two minutes. At the lower radio frequencies the radiation was absorbed by overlying undisturbed coronal matter. Quantitative computations justify this model. A detailed summary of the events, and some numerical data are given in the concluding Section 8 and in Table V.     

On the ratio between the mechanical fluxes in- and outside the solar chromospheric mottles

Available information about the relative areas on the quiet and active parts of the sun covered with magnetic elements, together with theoretical results on the relation between the photospheric mechanical flux and the consequent coronal electron density, allows one to conclude that the mechanical flux generated in the photospheric magnetic elements is about seven times as large as the flux generated in non-magnetic regions.     

On the behaviour of the hydrogen Lyman series in flares

The Lyman spectrum of hydrogen has been computed for a number of flare models, characterized by the column density of hydrogen atoms in the ground state (N ₁), the electron density (n _e) and the electron temperature (T _e). Broadening by the thermal Doppler effect and by Stark effect has been accounted for. The source functions for the individual lines of the series have been derived from non-LTE calculations of the excitation in hydrogen flares. The aim of the investigation is to evaluate the use of the intensities in between two successive Lyman lines for a determination of the value for N ₁, which is a physical parameter of the flare for which only indirect determinations are available. Whilst in principle this method could give reliable results, its practical application meets with difficulties which hardly can be overcome. Therefore, one probably has to base the N ₁ determination on the highest line resolvable in the spectrum.     

Extended dust shells around carbon stars resolved by “HIRAS”

We have examined forty-two carbon stars which show excess emission at 60 and/or 100µm by applying maximum-entropy image reconstruction techniques to the IRAS 60µm survey data. Thirteen stars are found to be extended in the reconstructed images. Four of them show a detached ring centered on the stellar position. In particular, U Ant may have a double detached dust shell. The implications of our results are discussed concerning the variation of mass loss on the AGB evolution.     

The effect of solar pressure on the motion and stability of interconnected satellites in orbit

The paper deals with the effect of solar pressure on the motion and stability of two satellites connected by an inextensible string in a central gravitational field of force. A system of nonlinear, nonhomogeneous, and non-autonomous equations under the rotating frame of reference in Nechvíle's coordinate system have been obtained. The general solution of the above system of equations is beyond our reach. The particular solutions have been obtained.The particular solution in which the system lies, wholly along the radius vector joining the attracting centre and the centre of mass of the system under the central attracting force along was found to be stable (Singh, 1973). Naturally we got interested in examining the effect of solar radiation pressure on the stability of this particular solution.     

云南省怒江傈僳族自治州经济发展战略研究

怒江傈僳族自治州是云南省最贫困的民族自治州。本文在认真分析、正确认识州情和改革开放形势的前提下,提出经济发展的指导思想和资源开发脱贫型的战略模式,制定了战略目标、战略步骤和战略重点。在产业结构方面,确定以铅锌为主的有色金属工业,以大理石为主的建材工业,以林副产品为主的生物资源综合开发作为三大主导产业。为保证战略目标的实现,提出重视科学技术和教育事业;改善交通、解决能源、搞活流通:绝不放松粮食生产,慎重解决人口问题;高度重视水土保持,维持生态平衡;采取特殊政策和灵活措施等。     

REE Characteristics of the Kalatongke Cu-Ni Deposit, Xinjiang, China

On the basis of the study on the REE geochemistry of the ore minerals and host rocks of the Kalatongke Cu-Ni deposit, Xinjiang, it is indicated that the major ore minerals, sulfides, were sourced from the host mafic-ultramafic magma. Characterized by low REE content of sulfide, such a Cu-Ni sulfide deposit occurring in the orogen is obviously different from that on the margin of the craton. Because the mafic-ultramafic rocks from the Cu-Ni sulfide deposit occurring in the orogen is water-rich and the REEs of some sulfides show a particular "multiple-bending" pattern, which suggests coexistence of multiple liquid phases (fluid and melt), the sulfide melt possibly contains a great deal of hydrothermal fluids and increasingly developed gases and liquid-rich ore-forming fluids after the main metallogenic epoch (magmatic segregation stage).     

海拉尔盆地贝尔凹陷布达特群水力破裂的岩石学特征及其成因探讨

海拉尔盆地贝尔凹陷布达特群凝灰质泥岩中发育大量凝灰质泥岩角砾。岩芯及透射光显微镜观察发现,这是一种水力破裂体系中流体和岩石作用的产物一水压碎屑岩。水压碎屑岩的岩石学特征表现为：角砾之间具有可拼合性、岩芯横切面上发育大量“T”型垂直裂缝、微细纤维状铁白云石脉对壁生长。水力破裂作用的成因主要与布达特群岩性组合特征、构造-流体作用有关。     

风沙流中沙粒浓度分布的实验研究

利用粒子图像测速技术（PIV）,在风洞内对与天然沙接近的石英沙风沙流沙颗粒浓度沿高度分布进行了研究。对 3种不同轴线风速研究结果表明,风沙流中沙粒浓度沿水平方向基本不变,而随高度呈指数衰减,而且其衰减速率与风速密切相关。风速越大,衰减速率越慢;风速越小,衰减速率越快。风沙运动一旦发生时,靠近沙床表面的沙粒浓度随风速变化很小,可以认为趋于稳定,达到最大值。