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| 1 | CO observations of massive star forming regions at different evolutionary phases显示文摘The 12CO (J=1-0), 13CO (J=1-0) and C18O (J=1-0) emissions in 9 massive star forming regions, which are believed to be at different stages of massive star formation, were mapped with the 13.7 m millimeter wave telescope at Qinghai Station of Purple Mountain Observatory. Of the observed 9 sources, 13CO cores were detected in seven of them, and C18O cores in five of them. And only two sources associated with C18O cores and H2O masers showed the extended structures and strong outflows. This is the first detection of outflow associated with IRAS 22566+5828 in the observing field of S152/S153. The physical parameters of cores and outflows for these sources, derived from Local Thermal Equilibrium (LTE) analysis, are presented. These observing results suggest that the C18O cores will only appear when the gas density is high enough and the probability to have an outflow is very high when the clumps show the C18O and H2O maser simulta- neously. | CHEN Xi1,2, XU Ye1,3, SHEN Zhiqiang1,3 & LI Jingjing1,2 1. Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai 200030, China 2. Graduate School of the Chinese Academy of Sciences, Beijing 100034, China 3. Joint Institute for Galaxy and Cosmology, Shanghai Astronomical Observatory and the University of Science and Technology of China, Shanghai 200030, China | 2006 | Science China(Physics,Mechanics & Astronomy)2006，49，5： | 6 |
| 2 | The radio structure of BL Lac object S5 2007+777显示文摘BL Lac object S5 2007+777 has been classified as a HYMOR(Hybrid Morphology radio source) for its hybrid FR I and FR II radio morphology.It is one of four BL Lac objects with a kpc scale extended X-ray jet.In this paper,we searched the unpublished European VLBI Network(EVN) archived high resolution data for this source,and present the high resolution radio structure.The EVN images all show a core-jet structure in 1.6,5 and 8 GHz.In combination with the VLA data in the literature,we found position angle differences(△PA) of about 10°-20° between pc and kpc scale jet structures.The brightness temperature estimated from multi-band EVN images are around 1011.2-1011.8 K,from which the Doppler factor ranges from 3.2 to 12.0.We found significant flux variations of the radio core in 1.6 and 5 GHz,from which we derived the variability in brightness temperature Tvar to be 1013.6 K and 1014.0 K,corresponding to the Doppler factors of 9.3 and 12.4,respectively. | WU ZhongZu1,3,GU MinFeng2 & CHEN YongJun2 1 College of Science,Guizhou University,Guiyang 550025,China 2 Key Laboratory for Research in Galaxies and Cosmology,Shanghai Astronomical Observatory,Chinese Academy of Sciences,Shanghai 200030,China 3 NAOC-GZU Sponsored Center for Astronomy,Guizhou University,Guiyang 550025,China | 2010 | Science China(Physics,Mechanics & Astronomy)2010，53，S1： | 3 |
| 3 | Robot-assisted laparoscopic pancreatic surgery: single-surgeon experience显示文摘 | Pier Cristoforo Giulianotti Fabio Sbrana Francesco Maria Bianco Enrique Fernando Elli Galaxy Shah Pietro Addeo Giuseppe Caravaglios Andrea Coratti | 2010 | Surgical Endoscopy2010，，7： | 3 |
| 4 | Customized treatment algorithmfor giant cell tumor of bone: report of a eries显示文摘 | William G Ward Galaxy Li | 1997 | Clinical Or-thopaedics and Related Research Number1997，，： | 1 |
| 5 | On the effect of injection of gas in the numerical simulation of accretion flows显示文摘We investigate the effects of various ways of injection of gas at the outer boundary in the numerical simulations of non-viscous accretion flows.We study three models.In Model A,we inject material around the equatorial plane.In Models B and C,fullrange θ injection is used(we employ spherical coordinates).In all three models,the injected material has the same density distribution with polar angle θ.From the equatorial region to the polar regions,angular momentum of the injected material of Model B decreases faster than that in Model C.For all of the models,after a transient episode of infall at the beginning of the simulations,the gas piles up in the equatorial regions outside the black hole and forms a thick torus bounded by a centrifugal barrier.We find that the accretion rates of Models B and C are more than ten times higher than that in Model A.In Model A,there is weak accretion only in the torus and outflows are found on the surface of the torus.In Model B,we find strong inflows on the surface of its torus,and the accretion in the torus is weak.In Model C,strong inflows also occur on the surface of its torus,but the accretion regions are narrower and there are strong outflows in its torus.In all of our models,the time-averaged density,pressure and angular momentum in the equatorial region can be described by a radial power law,with P ∝r-3/2,P ∝r-2 and l∝r0. | BU DeFu,YUAN Feng,WU MaoChun & YANG XiaoHong Key Laboratory for Research in Galaxies and Cosmology,Shanghai Astronomical Observatory,Chinese Academy of Sciences,Shanghai 200030,China | 2010 | Science China(Physics,Mechanics & Astronomy)2010，53，S1： | 1 |
| 6 | Synchrotron peak luminosity,black hole mass and Eddington ratio for SDSS flat-spectrum radio quasars显示文摘For a sample of 185 flat-spectrum radio quasars(FSRQs) constructed from the SDSS DR3 quasar catalog,we found a significant correlation between the synchrotron peak luminosity and both the black hole mass and Eddington ratio.This implies that the physics of its jet formation is not only tightly related with the black hole mass,but also with the accretion rate.We verify that the synchrotron peak luminosity can be a better indicator of jet emission than 5 GHz luminosity,through comparing the relationships between each of these two parameters and both black hole mass and Eddington ratio.The fundamental plane of black hole activity for our FSRQs is established as Lr ∝ L0x.80 ± 0.06 Mbh -0.04 ± 0.09 with a weak dependence on black hole mass,however,the scatter is significant. | GU MinFeng1 & CHEN ZhaoYu1,2 1 Key Laboratory for Research in Galaxies and Cosmology,Shanghai Astronomical Observatory,Chinese Academy of Sciences,Shanghai 200030,China 2 Graduate University of the Chinese Academy of Sciences,Beijing 100049,China | 2010 | Science China(Physics,Mechanics & Astronomy)2010，53，S1： | 1 |
| 7 | Multi-epoch X-ray observations of the narrow-line Seyfert 1 galaxy SDSS J160508.87+323921.4 with XMM-Newton显示文摘We present results of multi-epoch XMM-Newton observations separated by several years of the narrow-line Seyfert 1(NLS1) galaxy,SDSS J160508.87+323921.4.The NLS1 showed X-ray flux variations on timescales of years as well as low amplitude variations on timescales as short as hours,while the X-ray spectral shape remained essentially unchanged.The spectrum shows a significant soft X-ray excess.The model of reflection from an ionized disc,that is dominant in the whole XMM-Newton bandpass,provides the best description of the observed spectra for all the observations,though alternatives such as Compton scattering(T-0.25 keV) cannot be ruled out in a statistical sense.For the disc reflection model,the observed variations may originate either from the change in the reflection fraction,or from the variability of the intrinsic X-ray luminosity. | AI YanLi1,2,3,YUAN WeiMin1,2,ZHOU HongYan4,5 & WANG JianGuo1,2,3 1 National Astronomical Observatories/Yunnan Observatory,Chinese Academy of Sciences,Kunming 650011,China 2 Key Laboratory for the Structure and Evolution of Celestial Objects,Chinese Academy of Sciences,Kunming 650011,China 3 Graduate University of the Chinese Academy of Sciences,Beijing 100049,China 4 Center for Astrophysics,University of Science and Technology of China,Hefei 230026,China 5 Joint Institute of Galaxies and Cosmology,SHAO and USTC,Shanghai 200030,China | 2010 | Science China(Physics,Mechanics & Astronomy)2010，53，S1： | 1 |
| 8 | Robot-assisted laparoscopic pancreatic surgery: single-surgeon experience显示文摘 | Pier Cristoforo Giulianotti Fabio Sbrana Francesco Maria Bianco Enrique Fernando Elli Galaxy Shah Pietro Addeo Giuseppe Caravaglios Andrea Coratti | 2010 | Surgical Endoscopy2010，，7： | 1 |
| 9 | 寻找夜空中的异类--如何利用机器学习方法辨识稀有射电天体显示文摘简介人类往往能很轻易地就分辨一个事物究竞是无趣还是有趣。当我们看到一个东西,即便我们从未见过它,不知道它是用来做什么的,我们的视觉系统也能瞬间在视野里将它分辨出来,并判断出它与周遭事物相比是不是个有意思的物体。但同样的事情,如果让一台机器来做,可就要了它的“命”了。事实上,要让机器学会分辨物体,对它们进行分类,是一件相当困难的事情。 | 大卫·帕金森 盖里·塞格尔 骆彦(译) 唐弘铭(译) Radio Galaxy Zoo:EMU团队 | 2023 | 天文爱好者2023，，2： | 0 |
| 10 | 改变还是颠覆? ThinkPad×100e全面解析显示文摘红/白/黑三种机身色彩、全新造型的键盘、最低3499元的官方报价,X100e的出现让绝大多数ThinkPad老用户都惊诧不已:这还是我们熟悉的ThinkPad吗? | Galaxy Lee 牛唱(Photo) | 2010 | 微型计算机2010，，6： | 0 |
| 11 | 深度曝光Win7上帝模式显示文摘近日,在网络上风传Windows7原来有一项十分隐秘的功能——GodMode(上帝模式)。该消息一传出,就引来广大网友热论。那么,这个GodMode到底有什么秘功能?难道能让我们更方便地调整Windows设置?还是可以让我们接触到一些隐藏的神秘功能? | galaxy | 2010 | 计算机应用文摘2010，，13： | 0 |
| 12 | The Structure of Narrow-Line Region in LINERs显示文摘低电离的原子排放区域(班机) 在本地星系的大部分是在场的,当他们到更发光的活跃星群的原子核(AGN ) 的连接留下时逃犯。我们分析小瘤空格望远镜( HST )在Hα+获得的狭窄的乐队图象[ NII ]或[ OIII ]为在在一次尝试的附近的星系的巴乐马山光分光镜的调查的样品的 23 架班机和低光明 Seyfert 星系的乐队排队解决狭窄的排放的结构这些对象的区域( NLR )。在所有情况中, NLR 很好被解决,他们的形态学不同于目标反对。群,线性结构,螺线手臂或一枚戒指在目标的大部分被检测,当 Seyfert 星系和班机之间没有重要差别时。我们发现 NLR 尺寸和狭窄的线光明强烈为班机和低光明 Seyfert 星系被相关,并且Hα+的尺寸[ NII ]排放线区域作为 R NLR L 与 NLR 尺寸光明关系的延期一致的Hα0.44±0.06,为发光 Seyfert 星系和类星体定义,到在光明并且到更低的活动层次更低的二个数量级。我们的结果建议在班机的 NLR 类似于 Seyfert 星系的那些,并且他们以中央活跃星群的原子核为动力。 | Hai-Feng Dai Ting-Gui Wang Center for Astrophysics,University of Science and Technology of China,Hefei 230026,China Joint Instotute of Galaxies and Cosmology,Shanghai Observatory and USTC,China | 2008 | Chinese Journal of Astronomy and Astrophysics2008，8，3： | 0 |
| 13 | 快速检测笔记本电脑的续航时间显示文摘春节快到了,很多朋友都准备购买笔记本电脑,购买时大家最担心的就是手中的笔记本电脑电池是行货新品吗, | Galaxy | 2006 | 微型计算机2006，，1： | 0 |
| 14 | Some developments of hot accretion flow theory in the past ten years显示文摘The hot accretion flow model was re-discovered in 1994 by Narayan and collaborators.Intensive theoretical works have been conducted and significant progresses have been achieved.In this paper,we review several developments in the past ten years.This mainly includes the finding of outflow and convection and its dynamical effect on inflow;the direct electron heating by viscous dissipation;the effect of large scale toroidal magnetic fields in the inner region of the accretion flow;and the effect of global Compton scattering.Their observational applications are also introduced very briefly. | YUAN Feng Key Laboratory for Research in Galaxies and Cosmology,Shanghai Astronomical Observatory,Chinese Academy of Sciences,Shanghai 200030,China | 2010 | Science China(Physics,Mechanics & Astronomy)2010，53，S1： | 0 |
| 15 | Numerical simulation of hot accretion flows with thermal conduction显示文摘We report on the effects of isotropic thermal conduction in non-radiative collisionless accretion flows in two dimensions.In comparison to accretion flows without conduction,we find that the disk generally becomes cooler and thinner.Specifically,the magnitude of this effect depends on the kinetic viscosity coefficient.If it is proportional to density,the density profile of the accretion flow is flat,therefore the effect is not very obvious.But,if it is proportional to r1/2,as is usual for the 'α' disk description,the density profile is steeper.Therefore,the effect will be much more obvious,with the temperature profile of the accretion flow becoming much flatter.This will have important observational consequences. | WU MaoChun,YUAN Feng & BU DeFu Key Laboratory for Research in Galaxies and Cosmology,Shanghai Astronomical Observatory,Chinese Academy of Sciences,Shanghai 200030,China | 2010 | Science China(Physics,Mechanics & Astronomy)2010，53，S1： | 0 |
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