从高空普查含气构造

莫斯科“农业资源自动化信息控制系统”科学研究中心和沃罗湟日大学的专家们，在“黑海油气”公司基地首次进行了海面红外线热探测试验．试验的目的是研究已知的、产生在天然气田之上的海面负热异常效应．     

阳光红外线也会伤皮肤

德国研究人员发现，不仅阳光中的紫外线会损害皮肤，一直以来被视为无害的红外线也会伤及皮肤。据报道，德国研究人员从分子水平上研究了红外线对皮肤产生的作用。结果显示，红外线能使细胞内产生多种反应，并在这个过程中形成所谓的“自由基”。这些自由基会攻击皮肤中的其他细胞成分，进而使皮肤结缔组织遭到破坏，导致皱纹增加。     

无名画作惊现达芬奇指印

加拿大裔收藏家彼得·西尔弗曼两年前以11400英镑（约会12.5万元人民币）的价格买下了一幅被认为创作于19世纪初的少女肖像画。     

Infrared Characteristics of Associated Sources of Water Masers

We present an analysis of the infrared properties of 1417 water masers collected from the literature published by December 2004. The associated infrared sources of the water masers were identified with IRAS and MSX (Midcourse Space Experiment) catalogues. There are 1252 water masers associated with IRAS sources within 1', which include 700 interstellar and 552 stellar sources. For 382 sources, the IRAS counterpart identification and the maser classification are new. We found the colors of the interstellar maser sources are much redder than those of the stellar ones at IRAS wavelength bands; 99% of the interstellar maser sources are above black body line, while 95% of the stellar masers are below. The distribution difference of the two kinds of masers shown in the color-color diagram is due to their different optical depths and temperature distributions of dust regions. There are 743 water masers with MSX counterparts, of which 552 are interstellar masers and 191 are stellar masers. MSX colors of the associated sources of water masers are here analyzed for the first time. The color differences among the MSX bands are small and the interstellar masers are redder than the stellar masers. There is a correlation between the intensity of the stellar water maser emission and that of the 12μm and 25μm emissions, while there is no correlation between the water maser emission and the 8 μm emission. The infrared intensity increases with increasing wavelength for the interstellar masers, while it is the opposite for stellar masers. These results may provide clues for the pumping of water maser and for the properties of the two kinds of maser emission regions.     

Comparisons of Infrared Colors and Emission-line Intensities between Two types of Seyfert 2 Galaxies

We study the relation between the infrared colors[ OⅢ] emission lines,gaseous absorbing column density(NH) ,and the detectability of the polarized (hidden)broad-line region(HBLR) in a large sample of 75 Seyfert 2 galaxies(Sy2s).From the indicators of star-formation activity,f60/f100 and LFIR/LB,we find some evidence that the Sy2s without HBLR show higher star-formation activities than those with HBLR,in agreement with previous prediction.Also,we confirm that the HBLR Sy2s tend to have a larger luminosity ratio of the core to the host galaxy,suggesting that the HBLR Sy2s display more powerful AGN activity.Howerver,the level of obscuration found in previous papers in nearly indistinguishable between the two types of Sy2s.The results support the statement that the non-HBLR Sy2s,with a weaker core component and a stronger star-formation activity component,are intrinsically different from the HBLR Sy2s,which are Sy1 systems with a hidden powerful AGN core and a low star-formation activity.The indications are that the non-HBLR Sy2s might be at an earlier evolutionary phase than the HBLR Sy2s.     

An infrared study of Be stars based on ISO SWS01 spectra

The Infrared Space Observatory （ISO） Short-Wavelength Spectrometer （SWS） spectra of 10 Be stars are presented. It can be seen that the Be stars show a diversity in their ISO SWS01 spectral classifications by Kraemer et al., from naked stars, stars associated with dust, stars with warm dust shells, stars with cool dust shells to very red sources. In addition, the Brα/HI（14-6） line flux ratio derived for the sample stars is compared with that of P Cyg, and it is found that the line ratio of Be stars which were investigated show not only lower values as suggested by Waters et al., but also larger values. Therefore, the line ratio cannot be used to judge whether a star is a Be star or not.     

The Effect of AGN and SNe Feedback on Star Formation, Reionization and the Near Infrared Background

Feedback from supernovae (SNe) and from active galactic nuclei (AGN) accom-panies the history of star formation and galaxy evolution. We present an analytic model to explain how and when the SNe and AGN exert their feedback effects on the star formation and galaxy evolution processes. By using SNe and AGN kinetic feedback mechanisms based on the Lambda Cold Dark Matter (LCDM) model, we explore how these feedback mecha-nisms affect the star formation history (SFH), the Near-Infrared Background (NIRB) flux and the cosmological reionization. We find the values of the feedback strengths, ∈AGN =1.0+0.50.3and ∈SN=0.04+0.02-0.02, can provide a reasonable explanation of most of the observational re-suits, and that the AGN feedback effect on star formation history is quite different from the SNe feedback at high redshifts. Our conclusions manifest quantitatively that these feedback effects decrease star formation rate density (SFRD) and the NIRB flux (in 1.4 - 4.0μm), and postpone the time of completion of the cosmological reionization.     

金属之王——黄金的自述

亲爱的人类朋友,我叫黄金,化学元素符号为Au,是人类人人都梦寐以求的一种贵重的稀有金属。我在地壳中的含量极低,克拉克值(平均含量)为4ppb,为丰度最低的金属。物以稀为贵,因此,目前在氧化矿床中只要每吨石头含有我0.5g,人类开采我就可以赢利了。我是人类最早发现和使用的金属之一,我以迷人的黄色金属     

同温层红外天文台（SOFIA）

红外天文概述 红外线是电磁波的一种,其波长比人眼所能看到的可见光要长。但是在天文学上,并没有十分明确的定义来确定红外线的波长范围。过去,在CCD出现之前,其下限一般界定在7000A,也就是0．7微米,这也是人眼所能感光的电磁波的波长上限。