三元体系RECl_3（RE＝Dy，Yb）－HOAc－H_2O（30℃）的研究     

李亚红  王惠  王林溪 《盐湖研究》1996,(Z1)

测定了三元体系ＲＥＣｌ３（ＲＥ＝Ｄｙ，Ｙｂ）－ＨＯＡｃ－Ｈ２Ｏ（３０℃）的平衡态的溶度数据并绘制了相应的溶度图。在两个体系中分别得到了ＤｙＣｌ３·６Ｈ２Ｏ和ＹｂＣｌ３·６Ｈ２Ｏ两种固相。依据ＨＯＡｃ对ＤｙＣｌ３·６Ｈ２Ｏ和ＹｂＣｌ３·６Ｈ２Ｏ有盐抗作用这一结论得到了一种制备ＤｙＣｌ３·６Ｈ２Ｏ和ＹｂＣｌ３·６Ｈ２Ｏ的ＨＣｌ—ＨＯＡｃ法。同时，在分析测定酸的重量百分浓度时，利用“差减法”得到了Ｈ＋的准确含量。  相似文献   

Reassessment of the garnet-clinopyroxene Fe−Mg exchange thermometer: II. Thermodynamic analysis     

R. G. Berman  L. Ya Aranovich  D. R. M. Pattison 《Contributions to Mineralogy and Petrology》1995,119(1):30-42

 The garnet (Grt)-clinopyroxene (Cpx) Fe-Mg exchange thermometer has been re-evaluated through analysis of phase equilibrium experiments defining the Fe-Mg exchange between Grt and Cpx, Grt and Ol (Ol=Olivine), and Cpx and Ol, together with thermophysical and other phase equilibrium constraints on solid solution and individual end-member properties. Results show that all data are mutually compatible if the heterogeneity range of Grt and Cpx in run products previously obtained by Pattison and Newton (PN) are accounted for in assessing equilibrium Grt-Cpx compositions. Derived mixing properties are in good agreement with results from numerous recent phase equilibrium studies. Application of the newly calibrated thermometer to a number of amphibolite to granulite facies terrains indicates temperatures between 70 and 200 ° C above PN’s thermometer, and general compatibility with independent temperature estimates. Received: 3 September 1993 / Accepted: 16 June 1994  相似文献   

Geophysical investigations on manned spacecrafts     

K. Ya. Kondratyev  O. I. Smokty 《Pure and Applied Geophysics》1969,72(1):227-246

Summary Review has been made of the first results and perspectives of investigations in geophysics and bordering sciences (geology, geography, agrobiology, etc.) by means of manned orbital space laboratories. Relatively detailed discussion is given to the problems of the interpretation of terrain feature pictures from space. Attentively considered are the technique and results of the photometric processing of atmospheric photographs near the horizon with the purpose of studying atmospheric optical non-homogeneities (in particular, aerosol layers). The possible investigations based on the use of data about the outgoing radiation spectra are mentioned. (, , .) . . ( , ) . .  相似文献   

Inverse problems of satellite meteorology     

K. Ya. Kondratyev  Yu. M. Timofeyev 《Pure and Applied Geophysics》1968,71(1):164-180

Summary The paper presents a review of the possibilities of using meteorological satellites for investigating various atmospheric phenomena and obtaining data on the physical condition of the atmosphere required for realizing the numerical methods of weather forecast, the synoptical analysis and other purposes. To avoid repetition the review does not include the much important material in the field of satellite meteorology which had been dealt with in earlier reviews.

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Vlf experiment with the interkosmos-5 satellite     

František Jiříček  Pavel Tříska  Jaroslav Vojta  Ya. I. Likhter  V. V. Korobovkin  Reviewer V. Bumba 《Studia Geophysica et Geodaetica》1973,17(1):49-58

Summary The Interkosmos5 VLF experiment consisted of a spectrum analyser with twelve narrow-band channels and broadband measurements between0.07 and20 kHz using an analogue telemetry with a tape recorder on board. The apparatus used in the experiment is shortly described, some examples ofVLF phenomena observed are given and a review of all analogue data recorded is shown in a graphical calendar.  相似文献   

Accretion and early degassing of the Earth: Constraints from Pu-U-I-Xe Isotopic systematics     

I. Ya. Azbel  I. N. Tolstikhin 《Meteoritics & planetary science》1993,28(5):609-621

Abstract— A review of problems related to Xe isotopic abundances in meteorites and terrestrial materials leads to four postulates which should be taken into account to build a model of the Earth's accretion and early evolution. 1. The pre-planetary accretion time scale was shorter than the ¹²⁹I half-life, 17 Ma, so the initial ratio of ¹²⁹I/¹²⁷I had not been decreased considerably when planetary accretion started; therefore, this must also be the case for the ²⁴⁴Pu abundance. 2. The initial relative abundance of involatile refractory ²⁴⁴Pu in proto-planetary materials should be the same as in chondrites, that is, ²⁴⁴Pu/²³⁸U = 0.0068; this value corresponds to initial ²⁴⁴Pu 0.30 ppb in the bulk silicate earth. In contrast, I is a highly volatile element; its initial abundance, accretion history and even the present-day mean concentrations in principal terrestrial reservoirs are poorly known. 3. There is much less fission Xe in the upper mantle, crust, and atmosphere than is predictable from the fission of ²⁴⁴Pu (Xe(Pu)) based on the above argument. Therefore, Xe(Pu) has been mainly released from these reservoirs. 4. A mechanism for Xe(Pu) escape from the complementary upper mantle-crust-atmosphere reservoirs, for example, atmospheric escape via collisions of a growing Earth with large embryos and/or hydrodynamic hydrogen flux, etc., operated during the Earth's accretion. These postulates have been used as a background for a balance model of homogeneous Earth accretion which envisages: growth of the Earth due to accumulation of planetesimals; fractionation inside the Earth and segregation of the core; degassing via collision and fractionation; and escape of volatiles from the atmosphere. During the post-accretion terrestrial history, the processes described by the model are continuous fractionation, degassing and recycling of the upper mantle and crust. The lower mantle is considered as an isolated reservoir. Depending on the scenario invoked, the accretion time scale varies within the limits of 50–200 Ma. In the light of recent experimental data, the latter value is inferred to the most realistic version which explains a high Xe(U)/Xe(Pu) ratio in the upper mantle. Contrary to previous suggestions, the ¹²⁹I-¹²⁹Xe subsystem is considered to be meaningless with regard to the terrestrial accretion time scale. The terrestrial inventory of ¹²⁹Xe(I) is controlled by the initial abundance of volatile elements (including I and Xe) in proto-terrestrial materials and the subsequent degassing history of the Earth. The residence time of a volatile element (e.g., Xe) in the bulk mantle (bm) during accretion, < t (Xe)_bm>, is approximated by the ratio of < t (Xe)_bm> m _bm(t)/φ_{bm, mf} ≤ 10 Ma, where m _bm(t) is the mantle mass, and φ_{bm, mf} is the rate of metal/silicate fractionation, which provided segregation of the core; φ_{bm, mf} is determined by involatile siderophile element abundances in the upper mantle. This relationship implies a link between the abundance of involatile siderophile and volatile incompatible elements. A short <t(Xe)_bm> reflects a high degassing rate due to extremely high φ_{bm, mf} 10²⁰ g/year. A small ratio of the atmospheric amount of Xe over the total amount of this gas in prototerrestrial materials, ≤0.01, is in accord with the process of Xe escape and fractionation in the primary Earth atmosphere.  相似文献   

Rotational perturbations in the Friedmann cosmological model     

Ya. B. Zel'dovich  I. D. Novikov 《Astrophysics》1973,6(3):203-206

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Venus: A perspective at the beginning of planetary exploration     

M.Ya. Marov 《Icarus》1972

In situ measurements of the Venus atmosphere, made by the entry probes Venera 4, 5, 6, and 7, and data from the Mariner 5 flyby, have provided essentially new and reliable information and have powerfully contributed to our understanding of the nearest planet. The abundances of the principal atmospheric constituents and the temperature and pressure profiles down to the Venus surface were obtained for the first time. It was shown that the atmosphere is composed primarily of CO₂ and that N₂ (if any) and H₂O are relatively minor admixtures. In the region of the Venera 7 landing, the temperature and pressure at the Venus surface were established as equal to 747 ± 20°K and 90 ± 15 kgcm⁻². Space vehicles have also provided limited but quite important information on the physical properties of the Venus upper atmosphere and ionosphere, and on the interaction of the planet with the interplanetary environment. The main characteristics of the Venus atmosphere are discussed here with emphasis on the Venera results, including instrumentation, data processing, and altitude profiles.  相似文献   

Study of intensity fluctuations in cosmic rays during Forbush-decreases on the basis of the data obtained with the inzmiran scintillation supertelescope     

L. I. Dorman  I. Ya. Libin  O. V. Gulinsky 《Astrophysics and Space Science》1980,73(2):337-347

The one-minute, five-minute, and hourly values of cosmic-ray intensity obtained with a scintillation telescope at Izmiran have been used to carry out the correlational and spectral analysis of large Forbush-decreases of cosmic rays in 1978. The spectra of power obtained for the periods of interplanetary disturbances are characterized by individual spectral lines whose amplitude exceeds at least a 95% interval of reliability.  相似文献   

The interaction of matter and radiation in a hot-model universe   总被引：3，自引：0，他引：3  

Ya. B. Zeldovich  R. A. Sunyaev 《Astrophysics and Space Science》1969,4(3):301-316

In this paper we continue the investigation initiated by Weymann as to the reason why the spectrum of the residual radiation deviates from a Planck curve. We shall consider the distortions of the spectrum resulting from radiation during the recombination of a primeval plasma. Analytical expressions are obtained for the deviation from an equilibrium spectrum due to Compton scattering by hot electrons. On the basis of the observational data it is concluded that a period of neutral hydrogen in the evolution of the universe is unavoidable. It is shown that any injection of energy att>10¹⁰ sec (red shiftz<10⁵) leads to deviation from an equilibrium spectrum.Translated by Peter Foukal.  相似文献