Na-bearing Ca-Al-rich inclusions in the Yamato-791717 CO carbonaceous chondrite     

Kazushige Tomeoka  Koji Nomura  Hiroshi Takeda 《Meteoritics & planetary science》1992,27(2):136-143

Abstract Ca-Al-rich inclusions (CAIs) in the Yamato-791717 CO carbonaceous chondrite contain 5 to 80 vol% of nepheline, along with minor sodalite, and thus are among the most nepheline-rich CAIs known. The primary phases in inclusions are mainly spinel, fassaite, aluminous diopside, perovskite, and hibonite. In contrast to many CO chondrites, melilite is rare. Spinel contains variable amounts of Fe (0 to 57 mol% FeAl₂O₄) and is commonly zoned. Texture suggests that nepheline is a secondary alteration product formed by replacing mainly melilite, fassaite, and spinel; melilite is the most susceptible to alteration of the primary phases, so most of it was probably already consumed to form nepheline. The majority of inclusions are single concentric objects or aggregates of concentric objects. Lightly altered inclusions have cores of spinel surrounded by bands of nepheline (replacing fassaite), fassaite, and diopside. In moderately altered inclusions, spinel cores are replaced by nepheline. In heavily altered inclusions, the major part of internal areas (50 to 80% in volume) are replaced by nepheline. In some moderately and heavily altered inclusions, only diopside rims remain unaltered. Textural relationships indicate that the resistance of primary phases to alteration increases in the order melilite, fassaite, spinel, diopside. The alteration probably proceeded with reaction of the primary phases with the low-temperature (≤ 1000 K) nebular gas rich in Na, Fe and CI. The degree of alteration in Y791717 CAIs appears to be much higher than those in CAIs in other reported meteorites.  相似文献   

Analytical expansions of torque-free motions for short and long axis modes     

Hiroshi Kinoshita 《Celestial Mechanics and Dynamical Astronomy》1992,53(4):365-375

Torque-free motion of a rigid body is integrable and its solution is expressed in terms of elliptic functions and elliptic integrals. The conventional analytical expression of the solution, however, is complicated and not suitable for hand-calculation. Recently the rotational motions of small celestial bodies in the solar system are frequently investigated by numerically integrating the equations of motion instead of using the analytical solution, since the numerical evaluation of the analytical and exact solution is a little bit difficult. As the observational accuracy of the rotational motions of the small bodies in the solar system is quite low, what we need for the reduction of these observations are rough estimates of the period of Eulerian motion ( or the free precession period) and the amplitudes of the main periodic terms. Here we give simple analytical expansions of torque-free motions for short- and long-axis modes, which are correct up to the second-order of a small parameter. These expressions include only trigonometric functions and are easily evaluated by hand calculation for estimates of the essential quantities from which we can determine a global rotational motion of the torque-free motion. They can also be used as the zero-th order solution in a perturbation method, when the motion is perturbed by external torques.  相似文献   

Impact-induced chondrule flattening in the Allende CV3 carbonaceous chondrite: Shock experiments     

Tomoki Nakamura  Kazushige Tomeoka  Toshimori Sekine  Hiroshi Takeda 《Meteoritics & planetary science》1995,30(3):344-347

Abstract— We have carried out shock-recovery experiments on the Allende CV3 carbonaceous chondrite using a single-stage propellant gun and succeeded in reproducing oriented, flattened chondrules like those observed in some natural CV3 chondrites. The Allende samples were shocked at equilibrium pressures of 11 and 21 GPa, which are close to the highest values in shock stages S2 and S3, respectively (Stöffler et al., 1991). Chondrules are flattened nearly perpendicular to the compaction axis with mean aspect ratios of 1.34 and 1.62 at pressures of 11 and 21 GPa, respectively; thus, the degree of chondrule flattening is proportional to the shock intensity. The chondrule flattening and foliation are mainly due to collapse of pores in the matrix under shock pressure. High matrix abundance of CV3 chondrites could result in much apparent chondrule flattening relative to ordinary chondrites. Optical and electron microscope observations show that textural and mineralogical characteristics of chondrules and matrix in the shock-loaded samples are very similar to those observed in naturally shocked CV3 chondrites. Our results provide strong support for the interpretation that the chondrule flattening and foliation in CV3 chondrites were caused by shock-induced pressure due to hypervelocity impacts on the meteorite parent bodies.  相似文献   

Local time asymmetries of the SSC-associated hydromagnetic variations at the geosynchronous altitude     

Masayuki Kuwashima  Hiroshi Fukunishi 《Planetary and Space Science》1985,33(6):711-720

167 SSC events have been studied by using the data observed at the multiple-satellites at the geosynchronous altitude. The strong local time asymmetry of the SSC amplitude which was found by Kokubun (1983) has been confirmed. The pronounced local time asymmetry has also been found with the direction of the initial movement of Psc magnetic pulsations. Those local time effects are interpreted by the intensification of the magnetopause surface current during a SSC event, and by the distance between the geosynchronous satellite and the surface current. It has also been clarified that the SSC signal propagates with a speed of 400–700 km s^?1 across the field lines in the magnetosphere as suggested by Wilken et al. (1982).  相似文献   

Relations between turbulent regions of interplanetary magnetic field and Jovian decametric radio wave emissions from the main source     

Hiroshi Oya  Akira Morioka 《Planetary and Space Science》1981,29(7):783-791

Jovian decametric radio wave emissions that were observed at Goddard Space Flight Center, U.S.A. for a period from 1 October to 31 December, 1974 and data obtained at Mt Zao observatory, Tohoku University, Japan, for a period from 14 July to 6 December, 1975 have been used to investigate the relationship of the occurrence of the Jovian decametric radio waves (JDW), from the main source, to the geomagnetic disturbance index, ΣK_p. The dynamic cross-correlation between JDW and ΣK_p indicates an enhanced correlation for certain values of delay time. The delay time is consistent with predicted values based on a model of rotating turbulent regions in interplanetary space associated with two sector boundaries of the interplanetary magnetic field, i.e. the rotating sector boundaries of the interplanetary magnetic field first encounter the Earth's magnetosphere producing the geomagnetic field disturbances, and after a certain period, they encounter the Jovian magnetosphere. There are also cases where the order of the encounter is opposite, i.e. the sector boundaries encounter first Jovian magnetosphere and encounter the Earth's magnetosphere after a certain period.  相似文献   

Pyrolysis of Transvaal kerogens. II. An evaluation of vacuum pyrolysis with polyethylene,polystyrene and their mixtures with minerals     

Hiroshi Ogino  Bartholomew Nagy 《Precambrian Research》1981,15(2):113-130

A series of experiments have been conducted with polyethylene and polystyrene standards in an attempt to define the advantages and limitations of a vacuum pyrolysis—gas chromatography—mass spectrometry procedure for the characterization of kerogen and other macromolecular substances. Effects of variations in pyrolysis temperatures and times, sample sizes (weights) and thickness were evaluated together with the reproducibility of the nature and abundances of pyrolyzates. The effects of minerals (illite and quartz) admixed in the polymers were also considered with reference to the nature of the breakdown products. Optimal pyrolysis conditions, where primary pyrolyzates were sufficiently abundant and secondary products did not hinder characterization, were attained at 450°C and 60–90 min. The reproducibility of the nature and quantities of pyrolyzates was rather satisfactory at this temperature and pyrolysis time. However, relatively large samples of macromolecular matter, which is considerably volatile at this temperature, led to the synthesis of an abundant yield of secondary products, but sample thickness does not affect the nature of pyrolyzates. Admixed mineral matter affected the nature and relative abundances of the pyrolyzates but did not impede characterization of samples, as primary breakdown products were discernible. Macromolecular substances of limited volatility, heterogeneous chemical composition and containing intractable mineral matter, such as many kerogens, need to be pyrolyzed as relatively large samples. The vacuum procedure used in these studies may be to advantage, as compared with some other methods, to pyrolyze such samples. This method seems to be also suitable for the pyrolysis of volatile macromolecular matter, provided that small samples are employed.  相似文献   

Long-term behavior of the motion of Pluto over 5.5 billion years     

Hiroshi Kinoshita  Hiroshi Nakai 《Earth, Moon, and Planets》1996,72(1-3):165-173

The motion of Pluto is said to be chaotic in the sense that the maximum Lyapunov exponent is positive: the Lyapunov time (the inverse of the Lyapunov exponent) is about 20 million years. So far the longest integration up to now, over 845 million years (42 Lyapunov times), does not show any indication of a gross instability in the motion of Pluto. We carried out the numerical integration of Pluto over the age of the solar system (5.5 billion years ≈ 280 Lyapunov times). This integration also did not give any indication of chaotic evolution of Pluto. The divergences of Keplerian elements of a nearby trajectory at first grow linearly with the time and then start to increase exponentially. The exponential divergences stop at about 420 million years. The divergences in the semi-major axis and the mean anomaly ( equivalently the longitude and the distance) saturate. The divergences of the other four elements, the eccentricity, the inclination, the argument of perihelion, and the longitude of node still grow slowly after the stop of the exponential increase and finally saturate.  相似文献   

Differences of observed characteristics between impulsive bursts and post-burst increases     

Keizo Kai  Takeo Kosugi  Hiroshi Nakajima 《Solar physics》1982,75(1-2):331-339

The change of source characteristics during the transition from the impulsive phase to the post-burst phase is investigated for cm bursts on a statistical basis. The results are the following: (1) The sudden decrease of the circular polarization degree is found almost invariably at the transition; typically from 20–30% down to a few percent. (2) Some bursts show remarkable source expansions in the post-burst phase. There are no cases in which impulsive bursts have larger source size than the associated post-burst increases. (3) Type III bursts which are indicative of non-thermal phenomena are associated with the impulsive phase but not with the post-burst phase. Implications of these observed results are discussed.  相似文献   

Linear and nonlinear cyclotron instability and VLF emissions in the magnetosphere     

Hiroshi MatsumotoIwane Kimura 《Planetary and Space Science》1971

A theoretical study is made of the whistler mode cyclotron instability both in linear and nonlinear regimes in conjunction with the generation of VLF emissions in the magnetosphere. For the nonlinear treatment, a well-established quasilinear method is used and some physical processes of the cyclotron instability viz. energy conservation, mechanism of instability and frequency change of the excited emissions are clarified. The results are applied to some types of the triggered VLF emissions; whistler triggered emissions and artificially stimulated emissions (ASE). It is found that whistler triggered emissions excited around the upper cutoff frequencies of whistlers may be explained by the whistler mode cyclotron instability by a model distribution function inferred from satellite data. In order to see a nonlinear evolution of the whistler mode cyclotron instability, computer simulations were carried out and it is shown that the change of frequency with time of whistler triggered emissions as well as characteristics of ASE are well explained by resonant nonlinear behaviour of whistler mode cyclotron instability considered in the present paper.  相似文献   

Overlaying landslides distribution on the earthquake source, geological and topographical data: the Mid Niigata prefecture earthquake in 2004, Japan   总被引：4，自引：3，他引：4  

Hiroshi P. Sato  Tatsuo Sekiguchi  Ryoichi Kojiroi  Yoshinori Suzuki  Makoto Iida 《Landslides》2005,2(2):143-152

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