New models of interstellar gas–grain chemistry – III. Solid CO₂     

Deborah P. Ruffle  Eric Herbst † 《Monthly notices of the Royal Astronomical Society》2001,324(4):1054-1062

Solid CO₂ is observed to be an abundant interstellar ice component towards both quiescent clouds and active star-forming regions. Our recent models of gas–grain chemistry, appropriate for quiescent regions, severely underproduce solid CO₂ at the single assumed gas density and temperature. In this paper, we investigate the sensitivity of our model results to changes in these parameters. In addition, we examine how the nature of the grain surface affects the results and also consider the role of the key surface reaction between O and CO. We conclude that the observed high abundance of solid CO₂ can be reproduced at reasonable temperatures and densities by models with diffusive surface chemistry, provided that the diffusion of heavy species such as O occurs efficiently.  相似文献   

Electron-impact rotational excitation of linear molecular ions     

Alexandre Faure  Jonathan Tennyson 《Monthly notices of the Royal Astronomical Society》2001,325(1):443-448

Molecular R -matrix calculations are performed to give rotational excitation rates for electron collisions with linear molecular ions. Results are presented for CO⁺, HCO⁺, NO⁺ and H₂⁺ up to electron temperatures of 10 000 K. De-excitation rates and critical electron densities are also given. It is shown that the widely used Coulomb–Born approximation is valid for Δ j =1 transitions when the molecular ion has a dipole greater than about 2D, but otherwise is not reliable for studying electron-impact rotational excitation. In particular, transitions with Δ j >1 are found to have appreciable rates and are found to be entirely dominated by short-range effects.  相似文献   

High-resolution observations of 6.7-GHz methanol masers with the Long Baseline Array     

R. Dodson  R. Ojha  S. P. Ellingsen 《Monthly notices of the Royal Astronomical Society》2004,351(3):779-790

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Nearby Protoclusters as Laboratories for Understanding Star Formation on Galactic Scales     

Philippe André 《Astrophysics and Space Science》2002,281(1-2):51-66

Detailed studies of nearby cluster-forming molecular clouds can help us understand the physical processes by which most stars form in galaxies. I review recent advances made on this subject. Submillimeter observations of nearby protoclusters suggest that stars are generally built from finite, detached reservoirs of mass inside molecular cloud cores, and point to a cloud fragmentation origin for the IMF. Much progress in this field will come from future large submillimeter instruments such as Herschel and ALMA. This revised version was published online in September 2006 with corrections to the Cover Date.  相似文献   

海洋鱼类分子系统地理学研究进展   总被引：1，自引：0，他引：1  

高天翔  任桂静  刘进贤  肖永双 《中国海洋大学学报(自然科学版)》2009,39(5)

简要叙述了分子系统地理学的发展简史、研究内容,重点介绍了Avise的5种物种分布模式及中性溯祖理论。并回顾了近年来分子系统地理学的研究进展及其在海洋鱼类研究中的应用,最后对海洋鱼类分子系统地理学研究进行了展望。  相似文献   

二纺蛛总科（蜘蛛目：新蛛下目）蜘蛛化石研究进展     

郭向博  任东 《地质论评》2022,68(5):1871-1880

二纺蛛总科包括5个现生科、5个化石科以及一些科级位置未定的化石物种,是蜘蛛目中较为古老的一个类群。目前已知最早的二纺蛛总科化石记录可以追溯到早侏罗世,但分子系统发育研究推测其起源时间为二叠纪。二纺蛛总科蜘蛛在中生代最为繁盛,化石物种相对较多,是蜘蛛化石类群的重要组成部分。而现生二纺蛛总科蜘蛛十分稀少,且主要分布在热带和亚热带地区。近年来的系统发育研究认为二纺蛛总科可能是复杂生殖器类的姐妹群,是蜘蛛演化研究的关键类群。因此,本文对二纺蛛总科分类系统的研究历史进行了回顾,总结了二纺蛛总科化石类群在不同地质历史时期的组成和分布,统计了二纺蛛总科蜘蛛化石的名录。目前,二纺蛛总科蜘蛛化石分类研究基础薄弱,部分化石类群的系统位置存疑,二纺蛛总科内部系统发育关系尚不清晰。在将来的研究中,需要利用多种技术手段获取化石材料的形态学信息,打好分类学基础;结合化石类群和现生类群进行系统发育分析;进而联系古地理、古生态、生物学行为等研究,全方位分析二纺蛛总科的自然演化历史。  相似文献   

水(冰):宇宙矿物     

陈丰  李雄耀  唐红  王世杰 《矿物学报》2015,35(2):255-266

水(冰)是最简单的化合物,也是宇宙中丰度最大的矿物。通常认为,水无嗅、无味,无处不在。然而,液态水或固态水却是异乎寻常的物质。水具有某些其它物质没有的,特别是赋予生命所要求的特殊性质,如氢键、水簇和kosmotrope离子等。本文综述水(冰)的结构、化学性质、物理性质、分布以及与生命的关系。  相似文献   

A Study on the CO Isotopic Lines of the Star Forming Region AFGL 5157     

MAO Chun-hua  YANG Ji  LU Deng-rong 《Chinese Astronomy and Astrophysics》2014

By the mapping observations simultaneously at the ¹²CO (J=1-0), ¹³CO (J=1-0), and C¹⁸O (J=1-0) lines on the area of 24’×24’ (12 pc×12 pc) of the star forming region AFGL 5157, we have obtained the distribution and averaged physical parameters for the respective ¹³CO and C¹⁸O cores of this molecu- lar cloud. At the edge of the molecular cloud, the isotopic abundance ratio is X [(¹³CO)/(C¹⁸O)] ≈ 10, close to the ratio of a giant molecular cloud. The viral masses of the ¹³CO and C¹⁸O cores are less than the masses of the molecu-lar cloud cores, so the molecular cloud cores are gravitationally unstable, and the C¹⁸O molecular cloud core is more easy to collapse. The column density distributions of the C¹⁸O molecular cloud core in the northeast and southwest directions are, respectively, 1.1 × 10²³× z^−0.43 and 4.6 × 10²⁵× z^−0.58, where z is the distance from the center of the molecular cloud core. The high velocity molecular out?ow has been con?rmed from our ¹²CO spectra, the mass loss rate of the out?ow has been estimated, and the mass-velocity relation of the out?ow is ?tted by a power-law function of m ∝ v^−1.8. The star formation rate of the ¹³CO molecular cloud core is as high as 23%, probably, under the in?uence of  相似文献   

Low velocity shock-cloud encounters I.     

András Horváth Jr.  L. Viktor Tóth 《Astrophysics and Space Science》1995,233(1-2):169-173

Shocks propagating in the interstellar medium (ISM) play an important role in the life of molecular clouds. Through a theoretical study of interaction between clouds and shocks we can understand, for example, the density distribution of observed molecular clouds and the first steps of star formation. The only way to study of interaction in detail is via a numerical hydrodynamical simulation. In this paper we present the first results of a hydrocode which is able to follow the processes after the collision between the cloud and shock front.Our main theoretical result is that the chemical processes (e.g. H₂ dissociation) can affect the dynamical processes significantly. Global parameters of the cloud are calculated for the comparision of the simulation and the observations.  相似文献   

The fragmentation of condensations of the primordial gas     

D. R. Flower 《Monthly notices of the Royal Astronomical Society》2002,333(4):763-767

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