Molecular signatures of MHD waves

The small ion-neutral drift speeds attained in MHD waves lead to a significant increase in the rates of several important ion-molecule reactions. The effect on the deuterium chemistry of dark clouds could allow MHD wave motion to be observed directly. The results of some recent observations to test this theory are outlined.     

Vibrational states of H<Subscript>2</Subscript>O in beryl: physical aspects

Single-crystal polarized Raman spectra (3,000–4,000 cm⁻¹ at 3 ≤ T ≤ 300 K) were measured for synthetic alkali-free and natural beryl, Be₂Al₃Si₆O₁₈·xH₂O, to determine the behavior of H₂O molecules of both Type I and Type II in the cavities. At low temperature, the H₂O molecules of Type I displace from the center of cavity and give rise to very weak hydrogen bonding with the host lattice. The H₂O Type I translational motion is characterized by substantial anharmonicity and looks like a motion of “a particle in the box” with a frequency of 6.3 cm⁻¹. Water Type II is characterized by a free rotation with respect to the C ₂ molecule axis, and it makes possible the water nuclear isomers (i.e. ortho- and para-) to be observed at low temperature.

榴辉岩石榴石中的水分子团：超高压变质过程中流体的证据

通过透射电镜，我们在大别山榴辉岩的石榴石中识别出水分子团。这证明 在大陆地壳岩石俯冲的过程中，石榴石作为水的载体是可以将水携带到地幔深处。而石榴石中的水分子团为超高压变质过程中有流体存在提供了有力的证据。     

Bipolar molecular outflows

Summary Bipolar molecular outflows are a ubiquitous phenomenon in the process of star formation. We review the main observational properties of the outflows around young stellar objects, highlighting the recent wealth of information provided by the new generation of large radiotelescopes operating at millimeter wavelengths (in particular the IRAM 30-m, the NRO 45-m, and the JCMT 15-m dishes). The observations of outflows containing molecular, jet-like flows and bullets are discussed in detail, as they provide key information for understanding origin and evolution of the outflows. We also discuss a number of closely related issues: the evidence for dense shocked gas associated with the flows, the interaction of the outflows with the ambient dense cores, the evolutionary status of the sources driving the outflows, the properties of circumstellar disks, and theoretical models of the origin of the neutral winds. All these areas are important for developing a plausible scenario for the formation and evolution of the bipolar molecular outflows.This article was processed by the author using the Springer-Verlag T_EX AAR macro package 1991.     

许氏平鲉(Sebastes schlegelii)TRAF基因的鉴定及其响应杀鱼爱德华氏菌侵染的表达模式研究

TRAF是机体内一种具有信息传导作用的胞内因子, 承担多个受体家族的信号转导工作, 在固有免疫以及获得性免疫方面都发挥出重要作用。TRAF作为一类胞内接头蛋白, 对多条信号途径的活化具有一定的影响, 包括细胞的增殖、生存、凋亡、炎症反应、免疫反应等。目前已有研究表明鱼类中的TRAF基因也发挥重要的免疫防疫作用。以许氏平鲉为研究对象, 基于基因组和转录组的数据库, 进行了许氏平鲉TRAF基因家族的系统鉴定。在许氏平中共鉴定到9个TRAF基因, 并对这些TRAF基因的长度和氨基酸个数进行了统计分析。同时, 分析了这9个TRAF基因的结构特征。选取了包括许氏平鲉在内的6种鱼类进行了TRAF基因的共线性分析。结果显示, TRAF基因在硬骨鱼类中具有保守的共线性。通过系统发育分析, 更好地解析了TRAF家族基因的进化关系, 同时也证明了对其鉴定及命名的准确性。此外, 还进行了TRAF家族基因的蛋白质相互作用网络预测以及表达模式分析。通过蛋白质相互作用的网络分析, 得到TRAF基因与其互作蛋白的关联状况。在杀鱼爱德华氏菌侵染许氏平鲉后的不同时间点, 探究TRAF基因在杀鱼爱德华氏菌刺激下的表达模式。定量结果显示, 除TRAF4.1外, 其他TRAF基因在感染后均存在不同程度的上调。综上所述, 从分子水平上揭示了许氏平鲉TRAF家族基因的结构和功能, 揭示了TRAF可能依赖的免疫通路, 为进一步探究TRAF家族基因在许氏平先天免疫过程中的作用奠定了基础。     

A search for propylene oxide and glycine in Sagittarius B2 (LMH) and Orion

We have used the Mopra Telescope to search for glycine and the simple chiral molecule propylene oxide in the Sgr B2 (LMH) and Orion KL, in the 3-mm band. We have not detected either species, but have been able to put sensitive upper limits on the abundances of both molecules. The 3σ upper limits derived for glycine conformer I are  3.7 × 10¹⁴ cm⁻²  in both Orion-KL and Sgr B2 (LMH), comparable to the reported detections of conformer I by Kuan et al. However, as our values are 3σ upper limits rather than detections we conclude that this weighs against confirming the detection of Kuan et al. We find upper limits for the glycine II column density of  7.7 × 10¹² cm⁻²  in both Orion-KL and Sgr B2 (LMH), in agreement with the results of Combes et al. The results presented here show that glycine conformer II is not present in the extended gas at the levels detected by Kuan et al. for conformer I. Our ATCA results have ruled out the detection of glycine (both conformers I and II) in the compact hot core of the LMH at the levels reported, so we conclude that it is unlikely that Kuan et al. have detected glycine in either Sgr B2 or Orion-KL. We find upper limits for propylene oxide abundance of  3.0 × 10¹⁴ cm⁻²  in Orion-KL and  6.7 × 10¹⁴ cm⁻²  in Sgr B2 (LMH). We have detected fourteen features in Sgr B2 and four features in Orion-KL which have not previously been reported in the interstellar medium, but have not been able to plausibly assign these transitions to any carrier.     

Comparison of 13CO line and far-infrared continuum emission as a diagnostic of dust and molecular gas physical conditions – I. Motivation and modelling

Determining temperatures in molecular clouds from ratios of CO rotational lines or from ratios of continuum emission in different wavelength bands suffers from reduced temperature sensitivity in the high-temperature limit. In theory, the ratio of far-infrared (FIR), submillimetre or millimetre continuum to that of a ¹³CO (or C¹⁸O) rotational line can place reliable upper limits on the temperature of the dust and molecular gas. Consequently, FIR continuum data from the COBE /Diffuse Infrared Background Experiment (DIRBE) instrument and Nagoya 4-m  ¹³CO  J = 1 → 0  spectral line data were used to plot  240 μm/¹³CO  J = 1 → 0  intensity ratios against 140/240 μm dust colour temperatures, allowing us to constrain the multiparsec-scale physical conditions in the Orion A and B molecular clouds.
The best-fitting models to the Orion clouds consist of two components: a component near the surface of the clouds that is heated primarily by a very large scale (i.e. ∼1 kpc) interstellar radiation field and a component deeper within the clouds. The former has a fixed temperature and the latter has a range of temperatures that vary from one sightline to another. The models require a dust–gas temperature difference of 0 ± 2 K and suggest that 40–50 per cent of the Orion clouds are in the form of dust and gas with temperatures between 3 and 10 K. The implications are discussed in detail in later papers and include stronger dust–gas thermal coupling and higher Galactic-scale molecular gas temperatures than are usually accepted, and an improved explanation for the N (H₂)/ I (CO) conversion factor. It is emphasized that these results are preliminary and require confirmation by independent observations and methods.