The ubiquity of micrometer-sized dust grains in the dense interstellar medium

Cold molecular clouds are the birthplaces of stars and planets, where dense cores of gas collapse to form protostars. The dust mixed in these clouds is thought to be made of grains of an average size of 0.1 micrometer. We report the widespread detection of the coreshine effect as a direct sign of the existence of grown, micrometer-sized dust grains. This effect is seen in half of the cores we have analyzed in our survey, spanning all Galactic longitudes, and is dominated by changes in the internal properties and local environment of the cores, implying that the coreshine effect can be used to constrain fundamental core properties such as the three-dimensional density structure and ages and also the grain characteristics themselves.     

Search for organic compounds in the lunar dust from the sea of tranquiblity

A sample of lunar dust was examined for organic compounds. Carbon detected in concentrations of 157 micrograms per gram had a delta(13)C per mil (PDB) value of + 20. Treatment with hydrochloric acid yielded hydrocarbons of low molecular weight, suggesting the presence of carbides. The gas chromatogram of the acylated and esterified derivatives of the hydrolyzate was similar to that obtained for the Pueblito de Allende meteorite. There were no detectable amounts of extractable high-molecular-weight alkanes, aromatic hydrocarbons, isoprenoid hydrocarbons, normal alkanes, fatty acids, amino acids, sugars, or nucleic acid bases. Traces of porphyrins were found, perhaps arising from rocket exhaust materials.     

The dust grains from 9P/Tempel 1 before and after the encounter with Deep Impact

Gemini-N observed the properties of dust ejected from the nucleus of comet 9P/Tempel 1 before and after its encounter with Deep Impact. Marked changes were seen in the 7.8- to 13-micrometer spectral energy distribution and derived grain properties of the inner coma. A strong, broad silicate feature dominated by emission from amorphous pyroxene, amorphous olivine, and magnesium-rich crystalline olivine had developed by 1 hour after impact. The ejected dust mass is congruent with 10(4) to 10(6) kilograms on the basis of our models. Twenty-six hours later the silicate feature had faded, leaving a smooth featureless spectrum, similar to that observed before the impact, suggesting that the impact did not produce a new active region releasing small particles on the nucleus.     

Influence of lunar phase on daily global temperatures

A newly available data set of daily satellite-derived, lower-tropospheric global temperature anomalies provides an opportunity to assess the influence of lunar phase on planetary temperature. These results reveal a statistically significant 0.02 K modulation between new moon and full moon, with the warmest daily global temperatures over a synodic month coincident with the occurrence of the full moon. Spectral analysis of the daily temperature record confirms the presence of a periodicity that matches the lunar synodic (29.53-day) cycle. The precision of the satellite-based daily temperature record allows verification that the moon exerts a discernible influence on the short-term, global temperature record.     

Al-khwarizmi: a new-found basin on the lunar far side

Apollo 16 and Apollo 17 photographs of the far side of the moon reveal a double-ringed basin 500 kilometers in diameter centered at 1 degrees N, 112 degrees E. The structure is very old and subdued; it is probably Pre-Nectarian in age and appears to have been filled and modified by younger events. The heights of the basin's rings are based on laser altimeter data from Apollo missions 15 through 17; these data suggest a third outer ring, approximately 1000 kilometers in diameter. Laser measurements also indicate that the filled basin separates the relatively low terrain on the eastern limb of the moon from the higher, more rugged highlands to the east.     

New seismic data on the state of the deep lunar interior

Direct shear-wave arrivals from seismtic events originating on the far side of the moon are not observed at some of the stations of the Apollo seismic network. These data suggest that the material in the lunar interior at a depth of 1000 to 1100 kilometers is more dissipative for seismic shear waves than the lithosphere above, and possibly exists in a partially molten state akin to the earth's asthenosphere.     

Long-lived volcanism on the lunar farside revealed by SELENE Terrain Camera

We determined model ages of mare deposits on the farside of the Moon on the basis of the crater frequency distributions in 10-meter-resolution images obtained by the Terrain Camera on SELENE (Selenological and Engineering Explorer) (Kaguya). Most mare volcanism that formed mare deposits on the lunar farside ceased at approximately 3.0 billion years ago, suggesting that mare volcanism on the Moon was markedly reduced globally during this period. However, several mare deposits at various locations on the lunar farside also show a much younger age, clustering at approximately 2.5 billion years ago. These young ages indicate that mare volcanism on the lunar farside lasted longer than was previously considered and may have occurred episodically.     

Interannual variability of global dust storms on Mars

Global dust storms on Mars occur in some years but not in others. If the four Mars years of Viking data are representative, some distinguishing characteristics can be inferred. In years with global dust storms, dust is raised in the southern hemisphere and spread over much of the planet by an intensified Hadley circulation. In years without global dust storms, dust is raised in the northern hemisphere by relatively active mid-latitude storm systems but does not spread globally. In both cases the dusty season is winter in the north. Assuming that the cross-equatorial Hadley circulation plays a key role in the onset of global dust storms, it is shown from numerical simulations that a northen hemisphere dust haze weakens its intensity and, hence, its contribution to the surface stress in the southern hemisphere. This, in turn, reduces the possibility of global dust storm development. The interannual variability is therefore the result either of a competition between circulations in opposite hemispheres, in which case the variability has a random component, or it is the result of the cycling of dust between hemispheres, in which case the variability is related to the characteristics of global dust storms themselves.     

不同种衣剂对种子萌发率的影响

为促进中国北方石质边坡植被恢复重建,采用了保水剂、腐殖质、草炭为种衣材料,与波斯菊、沙打旺及白蜡种子按不同比例混合,通过观测种子萌发率,筛选出最佳种衣剂配方。结果表明,保水剂与草炭、种子比例为1∶10∶2时,波斯菊、沙打旺和白蜡种子萌发率分别达到90%、89%和34%,比应用田园土的萌发率分别高16%、18%和22%。其中保水剂经水稀释150倍,草炭吸水至饱和。这在干旱石质边坡的植被恢复提供了理论依据和技术支持。     

Topographic-compositional units on the moon and the early evolution of the lunar crust

The distribution of elevations on the moon determined by Clementine deviates strongly from a normal distribution, suggesting that several geologic processes have influenced the topography. The hypsograms for the near side and far side of the moon are distinctly different, and these differences correlate with differences in composition as determined by Apollo orbital geochemistry, Clementine global multispectral imaging, and ground-based spectroscopy. The hypsograms and compositional data indicate the presence of at least five compositional-altimetric units. The lack of fill of the South Pole-Aitken Basin by mare basalts suggests poor production efficiency of mare basalt in the mantle of this area of the moon.     

Apollo 12 lunar material: effects on lipid levels of tobacco tissue cultures

Tobacco tissue cultures grown in contact with lunar material from Apollo 12, for a 12-week period, resulted in fluctuations of both the relative and absolute concentrations of endogenous sterols and fatty acids. The experimental tissues contained higher concentrations of sterols than the controls did. The ratio of campesterol to stigmasterol was greater than 1 in control tissues, but less than 1 in the experimental tissues after 3 weeks. High relative concentrations (17.1 to 22.2 percent) of an unidentified compound or compounds were found only in control tissues that were 3 to 9 weeks of age.     

春小麦结实特性对穗粒数的影响

试验以19个春麦品种为材料,试图探讨影响春麦穗粒数的生育阶段。结果表明,小花数多是穗粒数多的必要不充分条件;受精前的退化小花数相对来说要少于受精败育数和成胚后籽粒的退化数,也即受精前的退化小花数并不是限制穗粒数的主要因子;增加小花数同时减少小花的退化、减少受精败育数和成胚退化数是现阶段提高春麦穗粒数的关键。对于穗粒数多于40粒的品种减少小花数的退化提高可育小花数是增加穗粒数的关键;对于穗粒数在30￣40粒之间的品种减少成胚后籽粒的退化是提高穗粒数的关键;对于穗粒数低于30粒的品种,要增加受精前的小花数,同时要针对不同的品种,采取措施减少受精败育数或成胚后籽粒的退化数才能有效地提高穗粒数。     

稻米垩白的影响因素及遗传改良

垩白是稻米重要的品质性状之一。研究垩白发生的环境条件和遗传控制,对于选育和栽培优质水稻品种均具有重要意义。本文概述了环境因素对稻米垩白形成的影响,以及农艺性状与稻米垩白的相关性;综述了垩白形成的遗传基础,展望了稻米垩白改良的前景。     

园林植被滞尘效应研究进展

选择适合城市发展的滞尘能力强的植被,是城市绿地设计的基础研究内容,也是改善城市环境质量的重要保障.要文综述了国内外国林植被滞尘效应的研究现状和研究直趋势,最后提出了今后研究的重点,为城市绿地和生态城市建设提供参考.     

不同生态点播期对小麦籽粒戊聚糖含量的影响

2001至2002年分别在河北保定、江苏徐州和姜堰3个不同的生态点,研究了播期（适播和晚播）对小麦（徐州26、皖麦38和徐州25）籽粒戊聚糖含量的影响。结果表明：晚播能极显著提高小麦籽粒戊聚糖含量。在播期、环境与基因犁凼子中,以环境对籽粒戊聚糖含量的影响最大。保定点和姜堰点的小麦籽粒戊聚糖含量明显高于徐州点。播期与生态点间、生态点与品种间存在显著的互作效应。播期相同,环境对小麦籽粒戊聚糖含量的影响大于基因型。随着纬度的升高,播期对籽粒戊聚糖含量的影响下降。小麦籽粒戊聚糖含量与气象因子密切相关,以花后气象因子的效应大。