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排序方式: 共有113条查询结果,搜索用时 15 毫秒
1.
Flavio Scappini Cesare Cecchi-Pestellini Harvey Smith William Klemperer Alexander Dalgarno 《Monthly notices of the Royal Astronomical Society》2003,341(2):657-661
We consider sulphur depletion in dense molecular clouds, and suggest hydrated sulphuric acid, H2 SO4 · n H2 O, as a component of interstellar dust in icy mantles. We discuss the formation of hydrated sulphuric acid in collapsing clouds and its instability in heated regions in terms of the existing hot core models and observations. We also show that some features of the infrared spectrum of hydrated sulphuric acid have correspondence in the observed spectra of young stellar objects. 相似文献
2.
Gravitational wave detection through microlensing? 总被引:1,自引:0,他引:1
Roberto Ragazzoni Gianpaolo Valente Enrico Marchetti 《Monthly notices of the Royal Astronomical Society》2003,345(1):100-110
It is shown that accurate photometric observations of a relatively high-magnification microlensing event ( A ≫ 1) , occurring close to the line of sight of a gravitational wave (GW) source, represented by a binary star, can allow the detection of subtle gravitational effects. After reviewing the physical nature of such effects, it is discussed to what extent these phenomena can actually be caused by GWs. Expressions for the amplitude of the phenomena and the detection probability are supplied. 相似文献
3.
An original theoretical model has been devised to simulate mass flow over hill slopes due to gravitational sliding. The sliding mass is discretized into a sequence of contiguous blocks which are subjected to gravitational forces, to bottom friction and to surface resistance stresses that are generally negligible for subaerial flows, but are relevant for submarine slides. The blocks interact with each other while sliding down the hill flanks because of internal forces that dissipate mechanical energy and produce a momentum exchange between the individual blocks, yet conserving the total momentum of the mass. Internal forces are expressed in terms of interaction coefficients depending on the instantaneous distance between the block centers of mass, which is a measure of the deformation experienced by the blocks: the functional dependence includes three parameters, namely the interaction intensity ¯, the deformability parameter and the shape parameter , by means of which a wide range of interaction types can be fully accounted for. The time integration is performed numerically by solving the equations for the block velocities and positions at any time ti by means of the block accelerations at the previous time ti-1, and by subsequently updating the block accelerations, which allows to proceed iteratively to the following times. The model has been tested against laboratory results available from literature and by means of several numerical experiments involving a simplified geometry both for the sliding body and the basal surface, with the purpose of clarifying the influence of the model parameters on the slide dynamics. The model improves the performance of the existing kinematic models for slides, moreover preserving an equivalent numerical simplicity. Future applications and possible improvements of this model are suggested. 相似文献
4.
5.
Cesare Emiliani 《International Journal of Earth Sciences》1992,81(3):791-794
The giant impact on Earth proposed by some to generate the Moon could not have happened because the amount of carbonate rock and organic carbon present on Earth closely approximates the amount of CO2 predicted for the Earth's early atmosphere by comparison with the present atmosphere of Venus. It is suggested that the Moon may have fissioned from Mercury more than 4.4 billion years ago and may have been captured by the Earth no later than 3.2 billion years ago.A model for the origin of the Earth-Moon system that has been gaining favor recently visualizes a Marssize body impacting Earth and excavating enough material from the Earth to form the Moon (Newsome &Taylor, 1989). This giant impact not only would have sterilized the planet (Maher &Stevenson, 1988), obliterating any form of life that might have existed at the time, but also would have blown off the Earth's atmosphere (Kaula, 1990). As the story goes, Venus suffered no giant impact and conserved its CO2 atmosphere, whereas the loss of her CO2 atmosphere cooled the Earth's surface allowing the oceans to rain out (Kaula, 1990). It is widely believed that the different histories in the early evolution of their atmospheres set markedly different courses for the subsequent evolution of the two planets. I agree with this conclusion but disagree with the cause for the difference.If the giant impact really happened, it must have taken place not only after the Earth's accumulation was practically completed but also after a substantial core had formed (to account for the lesser density of the Moon).Venus has approximately 89 kg/cm2 of CO2 for a total of 4.11020kg. The Earth with a mass 1.226 greater than Venus, should have had 5.01020 kg of CO2. If entirely precipitated as carbonate, the Earth should now have 1.11021 kg of carbonate. A recent estimate (Hay, 1985) gives the total volume of carbonate rock on Earth as 276.1106 km3 which, for an average density of 2.83, corresponds to a mass of 7.81020 kg. This figure and the ratio limestone/shale/sandstone of 15/74/11 (Garrels &Mackenzie, 1971) leads to the carbonate inventory shown in Table 1. 相似文献
6.
We consider the gas-liquid first-order phase transitions and prove the existence of the critical point in white dwarf matter. The latent heat released in the liquefaction processes can be used in the interpretation of the spreading of the white dwarf sequence in H-R diagram. Some thermodynamic quantities, e.g., the saturation pressure, the latent heat, etc., are calculated along the gas-liquid coexistence curve, and their behaviour near critical point are studied. 相似文献
7.
Luigi De Cesare 《Astrophysics and Space Science》1973,25(1):133-148
For an evaluation of the superconducting critical fieldH
c as a function of the mass-density in the external layers of cold magnetic white dwarfs and in the superconducting proton fluid in neutron stars, we use the solution of a differential equation involvingH
c as a function of the pressure. The differential equation and its solution are obtained by pure thermodynamic way.Finally other thermodynamic quantities are calculated for the above superconducting astrophysical systems. 相似文献
8.
Giovanni Carraro Cesario Lia & Cesare Chiosi 《Monthly notices of the Royal Astronomical Society》1998,297(4):1021-1040
In this paper we report on pd-sph , the new tree-sph code developed in Padua. The main features of the code are described and the results of a new and independent series of 1D and 3D tests are shown. The paper is mainly dedicated to the presentation of the code and to the critical discussion of its performance. In particular, great attention is devoted to the convergency analysis. The code is highly adaptive in space and time by means of individual smoothing lengths and individual time-steps. At present it contains both dark and baryonic matter, this latter in the form of gas and stars, cooling, thermal conduction, star formation, feedback from Type I and II supernovae, stellar winds, and ultraviolet flux from massive stars, and finally chemical enrichment. New cooling rates that depend on the metal abundance of the interstellar medium are employed, and the differences with respect to the standard ones are outlined. Finally, we show the simulation of the dynamical and chemical evolution of a disc-like galaxy with and without feedback. The code is suitably designed to study in a global fashion the problem of formation and evolution of elliptical galaxies, and in particular to feed a spectrophotometric code from which the integrated spectra, magnitudes and colours (together with their spatial gradients) can be derived. 相似文献
9.
Claes G.H. Rooth Cesare Emiliani Henry W. Poor 《Earth and Planetary Science Letters》1978,41(4):387-394
Power spectrum analysis of the oxygen isotopic records of deep-sea cores cannot be directly used for correlation studies with the astronomical forcing functions because of the rapidity of the major deglaciations. The ensuing step change in the isotopic curves, repeated at somewhat irregular intervals, produces, in fact, substantial spectral energy in a wide frequency band that includes the frequencies of the precessional parameters.The isotopic fluctuations within the ramp sections of a composite core curve have been found to be highly correlated with the precessional parameters, indicating a linear response of climate to these parameters and verifying, at the same time, the essential correctness of the time scale adopted.A direct correlation of eccentricity with the major glacial/interglacial cycle is doubtful because some of the eccentricity minima have absolute values of the same order as some of the maxima, while the isotopic amplitude remains essentially constant. In order to test if the major cycle could be related to a terrestrial parameter exhibiting an asymmetric relaxation fluctuation, we have added an asymmetric saw-tooth function to an artificial curve constructed from the precessional parameters on the basis of optimal response amplitude. The curve thus generated reproduces the original isotopic curve with a similarity sufficient to warrant a close search and analysis of the relaxation process. 相似文献
10.
Cesare Marchetti 《Climatic change》1977,1(1):59-68
The problem of CO2 control in the atmosphere is tackled by proposing a kind of fuel cycle for fossil fuels where CO2 is partially or totally collected at certain transformation points and properly disposed of.CO2 is disposed of by injection into suitable sinking thermohaline currents that carry and spread it into the deep ocean that has a very large equilibrium capacity.The Mediterranean undercurrent entering the Atlantic at Gibraltar has been identified as one such current; it would have sufficient capacity to deal with all CO2 produced in Europe even in the year 2100. 相似文献