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中国科学院地化所在嫦娥五号月壤撞击玻璃中发现多种来源的OH和分子H2O（图）
太阳风 演化 遥感探测
2024/6/25
月表水的来源和保存是月球科学研究的重要问题，对月球水资源的分布和提取利用、认识无大气天体表面水的形成演化以及类地行星水来源等问题具有重要意义。前期的遥感探测和样品分析揭示了月壤中普遍存在太阳风成因水（OH/H2O），然而太阳风成因水的演化以及月表分子H2O的存在与否仍存在争议，限制了对月表水形成和保存过程的认识，需结合月球样品分析开展深入的研究。
约50亿年后，我们的太阳将演化成一颗红巨星，巨大到将金星也并入囊中。当太阳的能量近乎消耗殆尽时，它的核心将无法逃脱塌缩的命运，而外面的气体壳层将被强大的恒星风剥离，当红巨星大部分的气体都被吹散后，其中心裸露的炙热核心辐射出强烈的紫外光子，电离这些逃逸的气体。这些吸收紫外线之后的气体释放出朦胧的光圈，环绕中央的恒星，在光学波段上呈现明亮的彩色行星状星云（Planetary Nebula; PN）。相...
中国科学院新疆天文台星系宇宙学团组王震利用65米射电望远镜L波段观测C/2013 US10彗星时，在一颗彗星的挥发气体中同时探测到1667/1665 MHz两条羟基吸收线。该成果为国内首例。奥尔特云区的彗星C/2013 US10 Catalina距离太阳约10万天文单位，包含较为丰富的太阳系星云原始遗迹物质；其轨道离心率略大于1，双曲线轨道；于2015年11月至12月距离太阳约0.8天文单位飞掠太...
羟基（OH）分子是星际介质中首次被探测到的分子，于上世纪六十年代被探测到，基态OH脉泽也是首次被探测到的天体脉泽。类似于激光是在光学波段的一种受激发射，脉泽是在微波波段的一种受激发射。目前已经探测到的天体脉泽分子种类包括：水、甲醇、氧化硅及其同位素、甲醛、氰化氢及其同位素等。OH分子的结构简单，其脉泽具有多条谱线跃迁，其中以波长在射电L波段（频率包括：1612、1665、1667和1720兆赫兹）...
Detection of OH+ and H2O+ towards Orion KL
OH+ H2O+
2014/12/20
We report observations of the reactive molecular ions OH+, H2O+, and H3O+ towards Orion KL with Herschel/HIFI. All three N = 1-0 fine-structure transitions of OH+ at 909, 971, and 1033 GHz and both fi...
Faint Extended OH Emission from the Local Interstellar Medium in the Direction l \approx 108\circ, b \approx 5\circ
OH Emission Local Interstellar Medium Cosmology and Extragalactic Astrophysics
2012/2/21
We have mapped faint 1667 OH line emission (TA \approx 20 - 40 mK in our \approx 30' beam) along many lines of sight in the Galaxy covering an area of \approx 4\circ \times 4\circ in the general direc...
Very Large Array monitoring of 1720 MHz OH masers toward the Galactic Center
Array monitoring Galactic Center
2011/10/13
We present the first variability study of the 1720 MHz OH masers located in the Galactic Center. Most of these masers are associated with the interaction between the supernova remnant SgrAEast and the...
OH Masers and the Dust Emissions Towards High Mass Protostellar Objects
stars: formation masers: OH masers millimeter
2011/9/27
Context: OH maser emission is known to be associated with high mass star forming regions. Towards some of these regions, OH masers are associated with HII regions. Towards others, believed to be in an...
The OH Masers Towards IRAS 19092+0841
stars:formation masers ISM: individual: IRAS 19092 + 0841
2011/9/27
We present high angular resolution spectral line observations of ground state OH maser emission towards the young high mass proto-stellar object IRAS 19092+0841. The two OH main spectral lines, 1665 a...
Peering through the OH Forest: public release of sky-residual subtracted spectra for SDSS DR7
Cosmology and Extragalactic Astrophysics (astro-ph.CO) Instrumentation and Methods for Astrophysics (astro-ph.IM)
2010/12/29
The Sloan Digital Sky Survey (SDSS) automated spectroscopic reduction pipeline provides >1.5 million intermediate resolution, R~2000, moderate signal-to-noise ratio (SNR), SNR~15, astronomical spectra...
Discrete Source Survey of 6 GHz OH emission from PNe & pPNe and first 6 GHz images of K 3-35
Solar and Stellar Astrophysics (astro-ph.SR)
2010/12/23
The aim of this study is to investigate the physical properties of molecular envelopes of planetary nebulae in their earliest stages of evolution. Using the 100m telescope at Effelsberg, we have under...
High resolution oh maser survey in star forming regions。
Oh maser emission toward the young planetary nebula K3-35
maser emission young planetary nebula K3-35
2009/6/25
Oh maser emission toward the young planetary nebula K3-35。
VLA observations of H2O and OH (1612 MHz) maser emission toward OH 231.8+4.2
VLA observations OH H2O maser emission
2009/6/10
VLA observations of H2O and OH (1612 MHz) maser emission toward OH 231.8+4.2。
Far Infrared Mapping of Three Galactic Star Forming Regions: W3 (OH), S209 & S187
Interstellar dust W3(OH)–S209 S187
2009/5/20
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 200m using the TIFR 100 cm
...