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.     

Oh Megamasers: Circumnuclear Gas in Starbursts

OH megamaser emission is known to be associated with the most central 100 parsecs of ultra-luminous infrared galaxies (ULIRGs). The masers are probing dense concentrations of gas, which presumably have accumulated during the merger event forming the ULIRG. Here we summarize the results from primarily high resolution observations of the 18 cm OH lines in a few OH megamaser galaxies. The maser emission is commonly distributed in disks or tori, but there is also some evidence for other components such as outflows. The appearance of the observed emission strongly depends on the observing resolution, and new theoretical modeling has made important steps toward understanding the observed emission. The radio continuum in OH megamaser galaxies is generally starburst related, and detailed studies of the continuum could perhaps be used to date the merger.     

具有碳化硅拱星壳层的OH／IR星

利用ＩＲＡＳ低分辨率光谱（ＬＲＳ）观测资料,从近２０００个具有１６１２ＭＨｚＯＨ发射的ＩＲＡＳ源中,发现９个具有碳化硅特征拱星壳层的ＯＨ／ＩＲ星的候选者．进一步的研究表明其中的６个确实或极有可能既是显示１１．３μｍ碳化硅发射特征的碳星,也是表现１６１２ＭＨｚＯＨ脉泽发射的ＯＨ／ＩＲ星     

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.     

单斜辉石中缺陷OH结合机理的变温红外光谱实验研究

利用变温红外光谱及偏振实验的结果,依据晶体化学理论及键长与振动频率的关系,从热膨胀速率这一新的角度探讨了单斜辉石中缺陷OH的结合机理。单斜辉石中OH的红外吸收峰主要有3组:3600~3620cm-1、3500~3540cm-1和3445~3465cm-1。第1组峰对应的的OH结合方式是Si4 O2- 1/2H2Al3 OH-,第3组峰对应的OH结合方式是H填充M2空位。第2组峰对应的OH结合方式复杂,可能和多个位置有关。第2和第3两组OH偶极的振动方向一致,都是M1和M2的共棱O2—O1,而第1组OH偶极的振动方向则是M2的O2—O3棱。     

Atmospheric Loss Processes of Dimethyl and Diethyl Carbonate

A combined study of the OH gas phase reaction and uptake on aqueous surfacesof two carbonates, dimethyl and diethyl carbonate has been carried out todetermine the atmospheric lifetimes of these compounds. Rate coefficients havebeen measured for gas phase reactions of OH radicals with dimethyl and diethylcarbonate. The experiments were carried out using pulsed laser photolysis– laser induced fluorescence over the temperature range 263–372K and the kinetic data were used to derive the following Arrhenius expressions(in units of cm³ molecule^–1 s^–1):for dimethyl carbonate, k₁ = (0.83±0.27)×10^–12 exp [–(247± 98)/T] and fordiethyl carbonate, k₂ = (0.46±0.15)×10^–12 exp [(503± 203)/T]. At 298 K, therate coefficients obtained (in units of 10^–12 cm³molecule^–1 s^–1) are: k₁ =(0.35± 0.04) and k₂ = (2.31± 0.29). The results arediscussed in terms of structure-activity relationships.The uptake coefficients of both carbonates on aqueous surfaces were measuredas a function of temperature and composition of the liquid phase, using thedroplet train technique coupled to a mass spectrometric detection. Dimethyland diethyl carbonate show very similar results. For both carbonates, themeasured uptake kinetics were found to be independent of the aqueous phasecomposition (pure water, NaOH solutions) but dependent on gas-liquid contacttime which characterises a surface saturation effect. The uptake coefficientvalues show a slight negative temperature dependence for both carbonates.These values vary from 1.4×10^–2 to0.6×10^–2 in the temperature range of 265–279 Kfor dimethyl carbonate, from 2.4×10^–2 to0.9×10^–2 in the temperature range of 270–279 Kfor diethyl carbonate. From the kinetic data, the following Henry's lawconstants were derived between 279 and 265 K: dimethyl carbonate,H₁ = 20–106 M atm^–1; and diethyl carbonate,H₂ = 30–98 M atm^–1. The reported data showthat the OH reaction is the major atmospheric loss process of these twocarbonates with lifetimes of 33 and 5 days, respectively, while the wetdeposition is a negligible process.     

Pressure dependence of hydroxyl solubility in coesite

 The solubility of hydroxyl in coesite was investigated in multianvil experiments performed at 1200 °C over the nominal pressure range 5–10 GPa, at an f _O2 close to the Ni-NiO buffer. The starting material for each experiment was a cylinder of pure silica glass plus talc, which dehydrates at high P and T to provide a source of water and hydrogen (plus enstatite and excess SiO₂). Fourier-transform infrared (FTIR) spectra of the recovered coesite crystals show five sharp bands at 3606, 3573, 3523, 3459, and 3299 cm⁻¹, indicative of structurally bonded hydrogen (hydroxyl). The concentration of hydrogen increases with pressure from 285 H/10⁶ Si (at 5 GPa) to 1415 H/10⁶ Si (at 10 GPa). Assuming a model of incorporation by (4H)_Si defects, the data are fit well by the equation C _OH=Af ² _H2<\INF>Oexp(−PΔV/RT), with A=4.38 H/10⁶ Si/GPa, and ΔV=20.6 × 10⁻⁶ m³ mol⁻¹. An alternative model entailing association of hydrogen with cation substitution can also be used to fit the data. These results show that the solubility of hydroxyl in coesite is approximately an order of magnitude lower than in olivines and pyroxenes, but comparable to that in pyropic garnet. However, FTIR investigations on a variety of ultrahigh pressure metamorphic rocks have failed in all cases to detect the presence of water or hydrogen in coesite, indicating either that it grew in dry environments or lost its hydrogen during partial transformation to quartz. On the other hand, micro-FTIR investigations of quartz crystals replacing coesite show that they contain varying amounts of H₂O. These results support the hypothesis that preservation of coesite is not necessarily linked to fast exhumation rates but is crucially dependent on limited fluid infiltration during exhumation. Received: 23 August 1999 / Accepted: 10 April 2000     

针铁矿及其前体吸附亚砷酸根离子的反应及预处理方法的影响

观察了针铁矿及其前体对溶液中亚砷酸根离子的吸附过程和吸附性能。3种吸附剂分别为氢氧化铁凝胶、经微波真空干燥的凝胶和80℃烘干的凝胶,它们均转变成了针铁矿。氢氧化铁凝胶与亚砷酸钠溶液混和后,溶液的pH值在6min内从9.71上升到10.36,原因是亚砷酸根离子置换了针铁矿和氢氧化铁中的氢氧根;40min后开始持续下降,和亚砷酸根离子与吸附剂之间的缩合反应有关。pH值的转折点并不意味着吸附反应的结束,但代表了反应类型的转变。这两种类型的反应受温度和气体溶解组分的影响不大。吸附剂经超声波处理后,改善了其在介质中的分散性,吸附效率因此普遍提高,但也造成了固体微粒难以分离的问题。经真空微波处理的凝胶对砷阴离子的吸附率优于另外两种吸附剂,去除率分别提高了53.18%和17.22%。其主要原因可能是凝胶中的水分子在微波辐射场作用下的高频振动,使其内部在干燥脱水过程中保持了较高的孔隙度;此外,吸附剂的表面活性在微波处理过程中亦有可能得到了改善。     

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.