全文获取类型
收费全文 | 2131篇 |
免费 | 233篇 |
国内免费 | 275篇 |
专业分类
测绘学 | 27篇 |
大气科学 | 170篇 |
地球物理 | 624篇 |
地质学 | 655篇 |
海洋学 | 174篇 |
天文学 | 706篇 |
综合类 | 21篇 |
自然地理 | 262篇 |
出版年
2024年 | 12篇 |
2023年 | 10篇 |
2022年 | 23篇 |
2021年 | 48篇 |
2020年 | 65篇 |
2019年 | 70篇 |
2018年 | 52篇 |
2017年 | 59篇 |
2016年 | 52篇 |
2015年 | 61篇 |
2014年 | 54篇 |
2013年 | 118篇 |
2012年 | 65篇 |
2011年 | 144篇 |
2010年 | 139篇 |
2009年 | 167篇 |
2008年 | 200篇 |
2007年 | 159篇 |
2006年 | 128篇 |
2005年 | 137篇 |
2004年 | 122篇 |
2003年 | 94篇 |
2002年 | 79篇 |
2001年 | 68篇 |
2000年 | 83篇 |
1999年 | 79篇 |
1998年 | 72篇 |
1997年 | 42篇 |
1996年 | 38篇 |
1995年 | 38篇 |
1994年 | 19篇 |
1993年 | 18篇 |
1992年 | 15篇 |
1991年 | 12篇 |
1990年 | 9篇 |
1989年 | 16篇 |
1988年 | 16篇 |
1987年 | 7篇 |
1986年 | 5篇 |
1985年 | 8篇 |
1984年 | 7篇 |
1983年 | 6篇 |
1982年 | 2篇 |
1981年 | 5篇 |
1980年 | 3篇 |
1979年 | 3篇 |
1978年 | 2篇 |
1977年 | 4篇 |
1976年 | 3篇 |
1973年 | 1篇 |
排序方式: 共有2639条查询结果,搜索用时 320 毫秒
261.
262.
Matthew Lockwood 《Climate Policy》2013,13(4):1097-1112
Public support for climate policies is essential to underpin their credibility, but evidence suggests that an environmental basis for that support is not strong. It has been suggested that framing climate policies in other terms, such as energy security or job creation, will build a more sustainable political basis for bold climate policies. This approach is explored using data from a survey in 157 UK marginal constituencies. Framing does make a difference to support for the expansion of renewable energy, but not to support for policies on energy efficiency and financial assistance to developing countries. The data also show key differences in levels of support for policies between different socio-demographic and voter groups. 相似文献
263.
In this study, we aim to describe the background for design characteristics of emissions trading schemes (ETS) in developing and emerging economies, with a particular focus on the case of Korea. These countries may face unique hardships such as fierce opposition from industry sectors, the presence of a power imbalance between the Ministry of Environment (MOE) and ministries that are in charge of supporting output growth, and the absence or incomplete development of financial markets and auctioning mechanisms. To overcome these hardships, the Korean government legislated laws that defined timelines for every stage of ETS development, established a strategic governance architecture to make up the weak position of the MOE, offered strong market-stabilizing measures focused on maintaining the allowance price below a certain level, and provided support packages to make the low-carbon transition easy by compensating for losses caused by the Korea Emissions Trading Scheme (KETS). Such policy instruments that made adoption of KETS easier could be obstacles to making it efficient.Policy relevanceIn the process of adopting a cap-and-trade system, both a developing economy and an emerging economy may face unique hardships, such as strong opposition from industry sectors, the presence of a power imbalance between the Ministry of Environment (MOE) and ministries that are in charge of supporting output growth, and the absence or incomplete development of financial markets and auctioning mechanisms. To make up for the weak base of Korea’s ETS, the government legislated laws that defined timelines for every stage of the ETS development, established a strategic governance architecture to make up for the weak position of the MOE, offered strong market-stabilizing measures focused on maintaining the allowance price below a certain level, and provided support packages to make the low-carbon transition easy by compensating for losses caused by the Korea’s ETS. Korea’s experiences can be shared with other developing economies that are considering adoption of a cap-and-trade scheme. 相似文献
264.
265.
Andrew F. Cheng 《Icarus》2006,184(2):584-588
Three Jupiter family comets have now been observed by spacecraft with the surprising result that these comets lack unambiguous impact craters. Large-scale topography generally appears to be softened on these comets, although sharp topography is preserved at small scales. We find that viscous relaxation of water ice may explain these observations, given reasonable assumptions about ice grain size and temperatures attained in the interiors. We suggest that both the shapes and the cratering records of Jupiter family comets may be substantially modified and no longer reflect cometary formation processes or collisional evolution in the Kuiper Belt. 相似文献
266.
267.
268.
I.D.S. Grey 《Icarus》2004,168(2):467-474
Research on the impact cratering process on icy bodies has been largely based on the most abundant ice, water. However little is known about the influence of other relatively abundant ices such as ammonia. Accordingly, data are presented studying the influence on cratering in ammonia rich ice using spherical 1 mm diameter stainless steel projectiles at velocities of 4.8±0.5 km s−1. The ice target composition ranged from pure water ice, to solutions containing 50% ammonia and 50% water by weight. Results for crater depth, diameter, volume and depth/diameter ratio are given. The results showed that the presence of ammonia in the ice had a very strong influence on crater diameter and morphology. It was found that with only a 10% concentration of ammonia, crater diameter significantly decreased, and then at greater concentrations became independent of ammonia content. Crater depth was independent of the presence of ammonia in the ice, and the crater volume appeared to decrease as ammonia concentration increased. Between ammonia concentrations of 10 and 20% crater morphology visibly changed from wide shallow craters with a deeper central pit to craters with a smoothly increasing depth from the crater rim to centre. Thus, a small amount of ammonia within a water ice surface may have a major effect on crater morphology. 相似文献
269.
Evidence of volcano-ground ice interactions on Mars can provide important constraints on the timing and distribution of martian volcanic processes and climate characteristics. Northwest of the Elysium Rise is Hrad Vallis, a ∼370 m deep, 800 km long sinuous valley that begins in a source region at 34° N, 218° W. Flanking both sides of the source region is a lobate deposit that extends ∼50 km perpendicular from the source and is an average of ∼40 m thick. Previous studies have suggested the formation of the Hrad Vallis source region was the result of explosive magma-ice interaction and that the lobate deposit is a mudflow; here we use newly available MOLA, MOC, and THEMIS data to investigate the evidence supporting this hypothesis. Within the lobate deposit we have identified 12 craters with thermal infrared signatures and morphologies that are distinct from any other craters or depressions in the region. The thermally distinct craters are distinguished by their cool interiors surrounded by warm ejecta in the nighttime THEMIS IR data and warm interiors surrounded by cool ejecta in the daytime THEMIS IR data. The craters are typically 1100-1800 m in diameter (one crater is ∼2300 m across) and 30-40 m deep, but may be up to 70 m. The craters are typically circular and have central depressions (several with interior dune fill) surrounded by ∼1 to >6 concentric fracture sets. The distribution of the craters and their morphology suggests that they are likely the result of the interaction between a hot mudflow and ground ice. 相似文献
270.
We have studied data from the Galileo spacecraft's three remote sensing instruments (Solid-State Imager (SSI), Near-Infrared Mapping Spectrometer (NIMS), and Photopolarimeter-Radiometer (PPR)) covering the Zamama-Thor region of Io's antijovian hemisphere, and produced a geomorphological map of this region. This is the third of three regional maps we are producing from the Galileo spacecraft data. Our goal is to assess the variety of volcanic and tectonic materials and their interrelationships on Io using planetary mapping techniques, supplemented with all available Galileo remote sensing data. Based on the Galileo data analysis and our mapping, we have determined that the most recent geologic activity in the Zamama-Thor region has been dominated by two sites of large-scale volcanic surface changes. The Zamama Eruptive Center is a site of both explosive and effusive eruptions, which emanate from two relatively steep edifices (Zamama Tholi A and B) that appear to be built by both silicate and sulfur volcanism. A ∼100-km long flow field formed sometime after the 1979 Voyager flybys, which appears to be a site of promethean-style compound flows, flow-front SO2 plumes, and adjacent sulfur flows. Larger, possibly stealthy, plumes have on at least one occasion during the Galileo mission tapped a source that probably includes S and/or Cl to produce a red pyroclastic deposit from the same vent from which silicate lavas were erupted. The Thor Eruptive Center, which may have been active prior to Voyager, became active again during the Galileo mission between May and August 2001. A pillanian-style eruption at Thor included the tallest plume observed to date on Io (at least 500 km high) and new dark lava flows. The plume produced a central dark pyroclastic deposit (probably silicate-rich) and an outlying white diffuse ring that is SO2-rich. Mapping shows that several of the new dark lava flows around the plume vent have reoccupied sites of earlier flows. Unlike most of the other pillanian eruptions observed during the Galileo mission, the 2001 Thor eruption did not produce a large red ring deposit, indicating a relative lack of S and/or Cl gases interacting with the magma during that eruption. Between these two eruptive centers are two paterae, Thomagata and Reshef. Thomagata Patera is located on a large shield-like mesa and shows no signs of activity. In contrast, Reshef Patera is located on a large, irregular mesa that is apparently undergoing degradation through erosion (perhaps from SO2-sapping or chemical decomposition of sulfur-rich material) from multiple secondary volcanic centers. 相似文献