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11.
The twin STEREO spacecraft have been observing the Sun since 2006. Even though STEREO has only been active during solar minimum
conditions so far, an important number of coronal mass ejections (CMEs) and their interplanetary counterparts (ICMEs) have
been observed. Many of the ICMEs can be linked back to the corresponding CMEs on the Sun through the combination of remote-sensing
and in situ observations. This paper aims to answer the question whether a CME observed by a coronagraph will be detected in situ by a spacecraft in a specific location in the heliosphere. We use a flux-rope-like model fit to the STEREO SECCHI/COR2 data
to obtain the direction of CME propagation and its geometrical configuration in three dimensions. Based on model parameters,
we then calculate their angular widths and determine whether they should have been detected by STEREO-A, STEREO-B, Wind or ACE. We compare the results with corresponding in situ observations of ICMEs. We find that predictions of ICME detections on the base of COR2 data generally match well the actual
in situ observations. 相似文献
12.
I. S. Veselovsky A. V. Dmitriev I. A. Zhitnik A. N. Zhukov M. A. Zel’dovich S. V. Kuzin A. A. Naumkin I. G. Persiantsev A. Yu. Ryazanov Yu. S. Shugai O. S. Yakovchuk S. V. Bogachev S. V. Shestov 《Solar System Research》2005,39(3):169-175
The data of the Coronas F satellite and other spacecraft were used to show that, in October–November 2003, global variations in brightness occurred in all spectral regions of the solar electromagnetic radiation. The variations were asymmetric in heliolongitude. This phenomenon was accompanied by an extremely strong energy release in the form of coronal-mass ejections and solar flares. The most powerful of them took place on the solar side that was characterized by an enhanced brightness even before these events. As a result, superimposed corotating and sporadic disturbances, which are partly correlated, can be traced in parameters of the solar atmospheric radiation, flows of the solar-wind plasma, and heliospheric magnetic field.__________Translated from Astronomicheskii Vestnik, Vol. 39, No. 3, 2005, pp. 195–201.Original Russian Text Copyright © 2005 by Veselovsky, Dmitriev, Zhitnik, Zhukov, Zel’dovich, Kuzin, Naumkin, Persiantsev, Ryazanov, Shugai, Yakovchuk, Bogachev, Shestov. 相似文献
13.
The model calculations of 5-min solar oscillations are performed with consideration for the presence of canopy magnetic field in the solar chromosphere. It is shown that the occurrence of Alfvén resonances for 5-min oscillations in the solar chromosphere leads on the one hand to some change of the 5-min oscillation frequencies (up to a few µHz), and on the other hand to the heating of the chromosphere. The acoustic energy flux incoming to the chromosphere is of order 1 × 10 5 erg cm-2 s-1. 相似文献
14.
V. Suleimanov I. Bikmaev K. Belyakov N. Sakhibullin G. Zhukov Z. Aslan U. Kiziloglu I. Khamitov 《Astronomy Letters》2004,30(9):615-629
We present the photometric observations of the old nova V603 Aql with the RTT 150 Russian-Turkish telescope during eleven nights of 2001–2002. We show that the star at this time was in a state with positive superhumps and its photometric period of \(0\mathop .\limits^d 144 - 0\mathop .\limits^d 145\) was longer than the orbital period. We found night-to-night variations in the mean brightness of the system that are consistent with disk precession periods of \(3\mathop .\limits^d 3\) and \(3\mathop .\limits^d 0\) in 2001 and 2002, respectively. Analysis of the results and their comparison with the results of other authors using current theoretical models for disk precession lead us to suggest that the change in the disk precession period was caused by a change in the accretion rate in the system. V603 Aql in a state with negative superhumps was found to be brighter than it is in a state with positive superhumps by \(0\mathop .\limits^m 2 - 0\mathop .\limits^m 3\). We hypothesize that the transition between these states could also be caused by a change in the accretion rate. Quasi-periodic oscillations (QPOs) of the brightness with typical time scales of 9–70 min were detected on each observing night. These time scales were found to change from night to night. The detection of QPOs with a period of about 0.05 of the orbital period and its multiples on certain nights provides evidence for the model of QPO generation through accretion-rate modulation by ionization-front oscillations on the surface of the donor star near the inner Lagrangian point. 相似文献
15.
N. V. Alisov E. B. Valev Yu. V. Ilinich V. T. Zhukov N. S. Mironenko 《地理信息系统科学与遥感》2013,50(2):161-165
General problems of complex atlas mapping—selection of scales and indices for mapping, standardization of legends, establishment of appropriate levels of generalization, etc.—are addressed using the first comprehensive economic atlas of CMEA member countries as an example. The Atlas itself contains general overview maps of economic linkages of CMEA member nationa with the world economy, maps devoted to economic transactions and patterns within the CMEA as a whole, and general economic maps of the individual member nations. Translated from: Vestnik Moskovskogo Universiteta, geografiya, 1985, No. 4, pp. 3-6. 相似文献
16.
M. Mierla B. Inhester C. Marqué L. Rodriguez S. Gissot A. N. Zhukov D. Berghmans J. Davila 《Solar physics》2009,259(1-2):123-141
The data from SECCHI-COR1 and SECCHI-COR2 coronagraphs onboard the STEREO mission, which was launched in October 2006, provide us with the first-ever stereoscopic images of the Sun’s corona. These observations were found to be useful in inferring the three-dimensional structure of coronal mass ejections (CMEs) and their propagation direction in space. We apply four methods for reconstructing CMEs: i) Forward modeling technique; ii) Local correlation tracking (to identify the same feature in COR Ahead and COR Behind images) plus tie-point reconstruction technique; iii) Center of mass of the structures in a given epipolar plane plus tie-point reconstruction technique; iv) Polarization ratio technique. The four techniques are applied to three structured CMEs observed by COR1 and COR2 instruments, respectively, on 15 May 2007, 31 August 2007, and 25 March 2008. A comparison of the results obtained from the application of the four reconstruction algorithms is presented and discussed. 相似文献
17.
V. N. Soyfer V. A. Goryachev D. V. Andreev I. R. Barabanov A. P. Borisov Yu. N. Zhukov E. A. Yanovich 《Oceanology》2010,50(4):600-612
A methodology of experimental simulation of the state of spent nuclear fuel that is situated on the sea bottom as a result
of some catastrophes or dumping is developed. Data on long-term (more than 2000 days) experiments on the estimation of the
85Kr and 137Cs release rate from spent nuclear fuel (fragments of irradiated UO2 pellets) were first obtained; these estimates prove the correctness of the hypothesis put forward by us in the early 1990s
concerning an earlier 85Kr release (by one order of magnitude higher than that of 137Cs) as compared to other fission fragments in the case of the loss of integrity of a fuel containment as a result of corrosion
on the sea bottom. The method and technique of the onboard 85Kr and 137Cs sampling and extraction (as well as the sampling of tritium, a product of triple 235U fission) and their radiometric analysis at coastal laboratories are developed. Priority data on the 85Kr background in the bottom layers of the Barents and Kara Seas and the 137Cs and 3H in these seas (state of 2003) are presented. Models necessary for the estimation of the dilution of the fission products
of spent nuclear fuel and their transport on the bottom in accident and dumping regions are developed. An experimental method
for the examination of the state of spent nuclear fuel on the sea bottom (1 expedition each 2–3 years) by the 85Kr release into the environment (a leak tracer) is proposed; this release is an indicator of the destruction of a fuel containment
and the release of products of spent nuclear fuel in the case of 235UO2 corrosion in sea water. 相似文献
18.
A. F. Valeev K. A. Antonyuk N. V. Pit A. S. Moskvitin A. O. Grauzhanina D. R. Gadelshin S. V. Kolesnikov E. A. Zhuzhulina T. E. Burlakova G. A. Galazutdinov A. G. Gutaev R. Ya. Zhuchkov A. I. Ikhsanova D. G. Zhukov Arti Joshi J. C. Pandey A. F. Kholtygin G. G. Valyavin 《Astrophysical Bulletin》2017,72(1):44-50
We report the results of photometric observations of a number of magnetic white dwarfs in order to search for photometric variability in these stars. These V-band observations revealed significant variability in the classical highly magnetized white dwarf GRW+70?8247 with a likely period from several days to several dozen days and a half-amplitude of about 0. m 04. Our observations also revealed the variability of the well-known white dwarf GD229. The half amplitude of its photometric variability is equal to about 0. m 005, and the likely period of this degenerate star lies in the 10–20 day interval. This variability is most likely due to the rotation of the stars considered.We also discuss the peculiarities of the photometric variability in a number of other white dwarfs. We present the updated “magnetic field–rotation period” diagram for the white dwarfs. 相似文献
19.
Antonenko A. A. Zhukov N. M. Pavlova Z. N. Goikolova T. V. 《Geology of Ore Deposits》2020,62(4):314-331
Geology of Ore Deposits - The Varvarinskoye copper–gold deposit, large in terms of Au and small in terms of Cu, was discovered in 1979 in the western part of the Torgai trough in Kazakhstan.... 相似文献
20.
The changes in the field of the Arabian Sea level anomaly and the geostrophic currents are analyzed based on the data of satellite altimetry measurements in 1993–2008 within the framework of the AVISO project. On the intra-annual scale, the current field generally agrees with the circulation schemes published in a number earlier works. Their differences are due to the occurrence of the mesoscale eddies and jet currents revealed by the authors. 相似文献