全文获取类型
收费全文 | 290篇 |
免费 | 16篇 |
国内免费 | 2篇 |
专业分类
测绘学 | 2篇 |
大气科学 | 19篇 |
地球物理 | 103篇 |
地质学 | 103篇 |
海洋学 | 26篇 |
天文学 | 36篇 |
综合类 | 2篇 |
自然地理 | 17篇 |
出版年
2022年 | 1篇 |
2021年 | 2篇 |
2020年 | 6篇 |
2019年 | 5篇 |
2018年 | 15篇 |
2017年 | 10篇 |
2016年 | 12篇 |
2015年 | 18篇 |
2014年 | 18篇 |
2013年 | 13篇 |
2012年 | 19篇 |
2011年 | 17篇 |
2010年 | 19篇 |
2009年 | 17篇 |
2008年 | 24篇 |
2007年 | 7篇 |
2006年 | 6篇 |
2005年 | 9篇 |
2004年 | 15篇 |
2003年 | 7篇 |
2002年 | 11篇 |
2001年 | 4篇 |
2000年 | 10篇 |
1999年 | 2篇 |
1998年 | 6篇 |
1997年 | 5篇 |
1996年 | 4篇 |
1995年 | 2篇 |
1993年 | 5篇 |
1992年 | 4篇 |
1991年 | 1篇 |
1989年 | 1篇 |
1988年 | 1篇 |
1986年 | 1篇 |
1985年 | 1篇 |
1984年 | 1篇 |
1983年 | 2篇 |
1980年 | 2篇 |
1977年 | 1篇 |
1974年 | 1篇 |
1973年 | 1篇 |
1972年 | 1篇 |
1971年 | 1篇 |
排序方式: 共有308条查询结果,搜索用时 31 毫秒
201.
202.
Andrea Boattini Germano D’Abramo Giovanni B. Valsecchi Andrea Carusi Andrea Di Paola Fabrizio Bernardi Robert Jedicke Alan W. Harris Elisabetta Dotto Fiore De Luise Davide Perna Riccardo Leoni 《Earth, Moon, and Planets》2007,100(3-4):259-271
The Campo Imperatore Near Earth Object Survey (CINEOS) is an Italian survey dedicated to the search and follow-up of Near Earth Objects (NEOs). It is operated with the 90 cm f/3 Schmidt telescope at the Campo Imperatore of the Rome Astronomical Observatory (INAF-OAR) as a joint project with the Istituto di Astrofisica Spaziale and Fisica Cosmica (INAF-IASF) in Rome. Since the end of 2001 CINEOS has covered about 4,250 sq. deg to 20th magnitude in the course of about 160 nights. This effort led to the discovery of 7 Near Earth Asteroids (NEAs), 1 comet (167P/CINEOS; a member of the Centaur group) and a few other unusual objects including 2004 XH50 with a unique comet-like orbit. CINEOS has also contributed almost 2,200 preliminary designations and over 30,000 detections to the Minor Planet Center. About 20% of the survey effort was carried out at low solar elongations (LSE), although no object with an orbit interior (Inner Earth Objects, IEO class) or nearly interior to the Earth (Aten class) was found. The work at LSE was, however, very important to test survey strategies implemented with larger telescopes. We also provide the results of a CINEOS simulation on a reliable NEO population model based on the results of two larger scale surveys, Spacewatch and LINEAR. 相似文献
203.
A consistent theme in recent work on developing exploratory spatial data analysis (ESDA) has been the importance attached
to visualization techniques, particularly following the pioneering development of packages such as SPIDER and REGARD (Haslett
et al. 1990).
The focus on visual techniques is often justified in two ways: (a) the power of modern graphical interfaces means that graphics
is no longer a way of simply presenting results in the form of maps or graphs, but a tool for the extraction of information
from data; (b) graphical, exploratory methods are felt to be more intuitive for non-specialists to use than methods of numerical
spatial statistics enabling wider participation in the process of getting data insights. However, little work has been done
to decide which visualization tools might be needed to support ESDA, or how they can be most effectively implemented.
This paper briefly reviews a theoretical framework that has been suggested for addressing these issues, which comprises two
elements: firstly a data model, based on the distinction between rough and smooth properties of spatial data, that defines
what an analyst is looking for in data (Haining et al. 1998) and secondly a theoretical model for assessing the quality of
visualisation tools (Cleveland 1994). The emphasis of this paper is the use of the theoretical framework to structure an assessment
of SAGE, a software system that has been written for the spatial statistical analysis (including both exploratory and confirmatory
data analysis) of area based data linked to a GIS. The aim of the assessment is to identify the desirable features of the
system (that might be employed in other systems) whilst also highlighting what the additional requirements are thereby contributing
to the development of systems for ESDA that contain good quality scientific visualization tools for exploratory spatial data
analysis.
Received: 30 September 1998/Accepted: 17 September 1999 相似文献
204.
Paola Formenti Meinrat O. Andreae Jos Lelieveld 《Tellus. Series B, Chemical and physical meteorology》2000,52(2):678-693
As part of the 2nd A erosol C haracterisation E xperiment (ACE‐2), conducted during summer 1997 in the North Atlantic region between the Canary Islands and Portugal, we measured aerosol optical depths (AOD) at a mid‐tropospheric site, near the top of the volcanic mountain "El Teide"(28°16'N, 16°36' W, 3570 m asl). Our instrument was located at the highest altitude in a network of sunphotometers that extended down to sea level. Clear conditions dominated the ACE‐2 period, and, although suggested by back‐trajectories at 300 hPa, no evidence of anthropogenic pollution was found in our data. Three distinct dust episodes were observed. Vertical soundings and back trajectories suggested mineral dust from the Sahel region as a source. During these episodes, AOD increased an order of magnitude with respect to background conditions (from 0.017 up to 0.19 at λ=500 nm). A shift towards neutrality of the extinction spectral dependence (Ångstrom exponent α down to 0.13), indicated that the coarse mode (particle diameter >2 μm) dominated the aerosol size distribution. For 6 days during the episodes of mineral dust, a monomodal size distribution between 2 and 20 μm diameter was obtained from Mie based size distribution calculations. Estimates, at 500 nm, of the single scattering albedo ω0 (0.87–0.96), and the aerosol asymmetry parameter g (0.72–0.73) suggest that the dust layer causes a net cooling forcing at the top of the atmosphere. 相似文献
205.
Paola Rossi Gianluigi Bodo Silvano Massaglia Attilio Ferrari Andrea Mignone 《Astrophysics and Space Science》2004,293(1-2):149-155
Extragalactic radio sources are separated in two classes according to their specific luminosity: Fanaroff-Riley I and II. The origin of this dichotomy can be due either to intrinsec different properties of the AGN or to interaction of the jet with different enviroments. We assume that jets are always relativistic and supersonic close to their source, as recent observations suggest, and we explore the conditions in which the jets decelerate assuming FR I morphology. We have carried out high resolution 3D simulations for a set of parameters and in this paper we concentrate our discussion on two extreme cases. 相似文献
206.
The Zuccale fault is a gently east‐dipping normal fault exposed on Elba. Its displacement of 7–8 km occurred from the mid‐Miocene to the Early Pliocene and the fault has been exhumed from a depth of 3–6 km. A complex hydrofracture system exposed in the footwall block consists of three orthogonal vein sets: two vertical sets trending N–S and E–W and one sub‐horizontal. The veins show a crack‐and‐seal texture and mutually cross‐cut each other. Throughout the period when the Zuccale fault was active, the regional stress field was extensional with the minimum principal stress oriented E–W, consistent only with the N–S trending set of vertical hydrofractures. We attribute the three sets of orthogonal fractures beneath the low‐permeability phyllosilicate‐rich fault core to switches in the minimum compressive stress direction induced by cyclic build‐up and release of overpressure. 相似文献
207.
Piergiorgio Scarlato Paola Tuccimei Silvio Mollo Michele Soligo Mauro Castelluccio 《Bulletin of Volcanology》2013,75(9):1-8
To better understand the mechanisms leading to different radon background levels in volcanic settings, we have performed two long-term deformation experiments of 16 days using a real-time setup that enables us to monitor any variation of radon activity concentration during rock compression. Our measurements demonstrate that, in the case of highly porous volcanic rocks, the emanating power of the substrate changes as a function of the volcanic stress conditions. Constant magmatic pressures, such as those observed during dike intrusions and hydrothermal fluid injections, can result in pervasive pore collapse that is mirrored by a significant radon decrease until a constant emanation is achieved. Conversely, repeated cycles of stress due to, for example, volcano inflation/deflation cycles, cause a progressive radon increase a few days (but even weeks and months) before rupture. After rock failure, however, the formation of new emanation surfaces leads to a substantial increase of the radon signal. Our results suggest that surface deformation in tectonic and volcanic settings, such as inflation/deflation or constant magmatic pressures, have important repercussions on the emanating power of volcanic substrates. 相似文献
208.
Our Sun and planetary system were born about 4.5 billion years ago. How did this happen, and what is the nature of our heritage from these early times? This review tries to address these questions from an astrochemical point of view. On the one hand, we have some crucial information from meteorites, comets and other small bodies of the Solar System. On the other hand, we have the results of studies on the formation process of Sun-like stars in our Galaxy. These results tell us that Sun-like stars form in dense regions of molecular clouds and that three major steps are involved before the planet-formation period. They are represented by the prestellar core, protostellar envelope and protoplanetary disk phases. Simultaneously with the evolution from one phase to the other, the chemical composition gains increasing complexity. In this review, we first present the information on the chemical composition of meteorites, comets and other small bodies of the Solar System, which is potentially linked to the first phases of the Solar System??s formation. Then we describe the observed chemical composition in the prestellar core, protostellar envelope and protoplanetary-disk phases, including the processes that lead to them. Finally, we draw together pieces from the different objects and phases to understand whether and how much we inherited chemically from the time of the Sun??s birth. 相似文献
209.
Travis?J.?TennerEmail author Marc?M.?Hirschmann Anthony?C.?Withers Paola?Ardia 《Contributions to Mineralogy and Petrology》2012,163(2):297-316
The onset of hydrous partial melting in the mantle above the transition zone is dictated by the H2O storage capacity of peridotite, which is defined as the maximum concentration that the solid assemblage can store at P and T without stabilizing a hydrous fluid or melt. H2O storage capacities of minerals in simple systems do not adequately constrain the peridotite water storage capacity because
simpler systems do not account for enhanced hydrous melt stability and reduced H2O activity facilitated by the additional components of multiply saturated peridotite. In this study, we determine peridotite-saturated
olivine and pyroxene water storage capacities at 10–13 GPa and 1,350–1,450°C by employing layered experiments, in which the
bottom ~2/3 of the capsule consists of hydrated KLB-1 oxide analog peridotite and the top ~1/3 of the capsule is a nearly
monomineralic layer of hydrated Mg# 89.6 olivine. This method facilitates the growth of ~200-μm olivine crystals, as well
as accessory low-Ca pyroxenes up to ~50 μm in diameter. The presence of small amounts of hydrous melt ensures that crystalline
phases have maximal H2O contents possible, while in equilibrium with the full peridotite assemblage (melt + ol + pyx + gt). At 12 GPa, olivine and
pyroxene water storage capacities decrease from ~1,000 to 650 ppm, and ~1,400 to 1,100 ppm, respectively, as temperature increases
from 1,350 to 1,450°C. Combining our results with those from a companion study at 5–8 GPa (Ardia et al., in prep.) at 1,450°C,
the olivine water storage capacity increases linearly with increasing pressure and is defined by the relation
C\textH2 \textO\textolivine ( \textppm ) = 57.6( ±16 ) ×P( \textGPa ) - 169( ±18 ). C_{{{\text{H}}_{2} {\text{O}}}}^{\text{olivine}} \left( {\text{ppm}} \right) = 57.6\left( { \pm 16} \right) \times P\left( {\text{GPa}} \right) - 169\left( { \pm 18} \right). Adjustment of this trend for small increases in temperature along the mantle geotherm, combined with experimental determinations
of
D\textH2 \textO\textpyx/olivine D_{{{\text{H}}_{2} {\text{O}}}}^{\text{pyx/olivine}} from this study and estimates of
D\textH2 \textO\textgt/\textolivine D_{{{\text{H}}_{2} {\text{O}}}}^{{{\text{gt}}/{\text{olivine}}}} , allows for estimation of peridotite H2O storage capacity, which is 440 ± 200 ppm at 400 km. This suggests that MORB source upper mantle, which contains 50–200 ppm
bulk H2O, is not wet enough to incite a global melt layer above the 410-km discontinuity. However, OIB source mantle and residues
of subducted slabs, which contain 300–1,000 ppm bulk H2O, can exceed the peridotite H2O storage capacity and incite localized hydrous partial melting in the deep upper mantle. Experimentally determined values
of
D\textH2 \textO\textpyx/\textolivine D_{{{\text{H}}_{2} {\text{O}}}}^{{{\text{pyx}}/{\text{olivine}}}} at 10–13 GPa have a narrow range of 1.35 ± 0.13, meaning that olivine is probably the most important host of H2O in the deep upper mantle. The increase in hydration of olivine with depth in the upper mantle may have significant influence
on viscosity and other transport properties. 相似文献