名义上无水矿物中水的定量方法及其优缺点:FTIR方法及其存在问题

构成地幔的主要物相多是名义上无水矿物(NAMs),如橄榄石、辉石等,其晶体结构中能赋存一定量的水.水能显著地影响矿物、岩石体系的物理、化学性质乃至地球深部的许多重要地质过程.为精确获取NAMs的水含量,科学家不断开发和改进水的定量分析方法,其中傅里叶变换红外光谱法(FTIR)是测定NAMs中水含量的最主要手段,但不同研...     

Zn(OH)2-4在针铁矿(010)晶面上化学吸附结构和稳定性的理论研究

采用周期性边界条件的密度泛函理论研究Zn(OH)2-4在针铁矿(010)晶面的吸附结构和稳定性,得到了Zn(OH)2-4吸附前后键长的变化规律.计算结果表明:当Zn(OH)2-4通过共用O原子在针铁矿表面发生吸附时,平均ZnbridgeO键长较自由Zn(OH)2-4的平均Zn-O键长有增长趋势,而平均Zn-O键长则有缩短趋势;Zn(OH)24在针铁矿(010)晶面进行化学吸附时,双角DC2吸附方式为优势吸附物种.各吸附构型的稳定性顺序为DC2＞SE1＞DC1＞SC1＞SC2.     

Zn（OH）42-在针铁矿（010）晶面上化学吸附结构和稳定性的理论研究

采用周期性边界条件的密度泛函理论研究Zn(OH)42-在针铁矿(010)晶面的吸附结构和稳定性,得到了Zn(OH)42-吸附前后键长的变化规律。计算结果表明:当Zn(OH)42-通过共用O原子在针铁矿表面发生吸附时,平均ZnbridgeO键长较自由Zn(OH)42-的平均Zn-O键长有增长趋势,而平均Zn-O键长则有缩短趋势;Zn(OH)42-在针铁矿(010)晶面进行化学吸附时,双角DC2吸附方式为优势吸附物种。各吸附构型的稳定性顺序为DC2>SE1>DC1>SC1>SC2。     

Dust radiation fields and pumping of excited state OH masers in W3(OH)

I show that it is quite possible to obtain saturating amplification in the 13.44-GHz maser which is so far unique to W3(OH), using a combined radiative and collisional pumping scheme. The dominant radiative part of the pump involves far-infrared line overlap, and the far-infrared continuum is provided by dust, modelled as either a two-component mixture or composite grains. Transport of the far-infrared radiation is carried out via the accelerated lambda iteration method. The observational link between 13.44-GHz and 6035-MHz masers is reproduced by the model. Inadequate amplification in Sobolev models probably results from the optical depth limitations imposed by this approximation. I review the dust models used in far-infrared pumping models of OH masers, and conclude that the main consequence of moving from skewed blackbody functions to more sophisticated models is a selective pumping enhancement when ice mantles are included.     

河外H_2O超脉泽源的观测特性

研究了至今为止已发现的 2 0个河外H2 O超脉泽源的观测参数。多数河外H2 O超脉泽源的光度在几十至几百个L⊙ 之内 ,但TXFS2 2 2 6 - 184源的河外H2 O超脉泽源光度达 6 10 0L⊙ ,它属于射电星系类型 ,主要是由于其谱线轮廓较宽所造成的一种例外情况。所有 2 0个河外H2 O超脉泽源的系统速度约为几百到几千km·s- 1,16个河外H2 O超脉泽源的峰值流量密度小于 1Jy ,但有 4个河外H2 O超脉泽源的峰值流量密度大于 6Jy(6 .2～ 16Jy)。通过对这些河外H2 O超脉泽源的观测参数特征的分析和研究 ,得到这些观测参数之间的相关关系为 :河外H2 O超脉泽源的峰值流量密度的对数分别与系统速度的对数和距离的对数之间存在着反相关关系。而河外H2 O超脉泽源的光度的对数与距离平方和峰值流量密度乘积的对数之间存在着正相关关系     

Why every bipolar planetary nebula is 'unique'

We present the many evolutionary routes that progenitors of bipolar planetary nebulae (BPNe) can take. Overall, there are about a hundred qualitatively different evolutionary routes, hence about a hundred qualitatively different types of BPNe. Within each type there are quantitative differences as well. Adding the dependence of the appearance on inclination, we find that the number of different apparent structures of BPNe is about equal to, or even larger than, the number of known BPNe and proto-BPNe. Accordingly we argue that every BPN is a 'unique' object in its appearance, but all can be explained within the binary model paradigm. Therefore, we request a stop to the attaching of adjectives such as 'unique', 'peculiar', and 'unusual' to BPNe and proto-BPNe, thereby removing the need to invoke a new model for almost every 'unusual' BPN. As a case study we try to build a binary model for the proto-BPN OH 231.8+4.2. In our preferred model the AGB Mira-type star has a main sequence companion of mass ∼1 M_⊙, orbital period of ∼5 yr, and eccentricity of ≳0.1.     

Co-propagation of maser emission at 1720 and 4765 MHz

MERLIN observations are presented of OH 4765-MHz and OH 1720-MHz masers in the massive star-forming region W3(OH). Two of the three intense spots of maser emission at 4765 MHz are spatially coincident with two similar spots at 1720 MHz in both left-hand circular (LHC) and right-hand circular (RHC) polarizations, to an accuracy of 15 mas. The spots also overlap in velocity when allowance is made for Zeeman splitting of the 1720-MHz line. We conclude that we have found two examples of masers in different rotational levels of OH which are co-propagating through the same column of gas and experiencing competitive gain effects. The third 4765-MHz maser spot was found to have no overlapping counterpart amongst the 1720-MHz masers.     

Understanding Extragalactic Hydroxyl

Hydroxyl (OH) is one of the few molecules in space showing both maser emission and absorption. In the Milky Way, hydroxyl has been found in various environments such as stellar envelopes, star-forming regions, and HII regions, tracing the physical states of the interstellar medium. Extragalactic OH has been found to provide essential information about the dusty and obscuring material within the inner kiloparsec region of active galaxies. At angular resolution of a few tens of parsecs, OH shows a rather complicated spatial distribution and the interpretation of the circumnuclear environment is rather difficult. Based on results obtained from low- and high-resolution observations, the diagnostic tools of OH will be reviewed and the strategies to further investigate extragalactic OH will be discussed.     

Far infrared mapping of three Galactic star forming regions: W3(OH), S209 & S187

Three Galactic star forming regions associated with W3(OH), S209 and S187 have been simultaneously mapped in two trans-IRAS far infrared (FIR) bands centered at ≈140 and 200μm using the TIFR 100 cm balloon borne FIR telescope. These maps show extended FIR emission with structures. The HIRES processed IRAS maps of these regions at 12, 25, 60 & 100 ìm have also been presented for comparison. Point-like sources have been extracted from the longest waveband TIFR maps and searched for associations in the other five bands. The diffuse emission from these regions have been quantified, which turns out to be a significant fraction of the total emission. The spatial distribution of cold dust (T < 30 K) for two of these sources (W3(OH) & S209), has been determined reliably from the maps in TIFR bands. The dust temperature and optical depth maps show complex morphology. In general the dust around S209 has been found to be warmer than that in W3(OH) region.