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Thermal analysis of the baffle structure of the Solar Space Telescope

Science china(Physics,Mechanics & Astronomy) 2010年第9期53卷 1755-1764页

作者： li Rong1,2.3 & WANG Sen1,3 1 national {2. Observatories,chinese academy of sciences,Beijing 100012.china 2.Graduate University of chinese academy of sciences,Beijing 100049,china 3 key Laboratory of Solar Activity,national {2. Observatories of chinese academy of sciences,Beijing 100012.china national astronomical Observatories Chinese Academy of Sciences Beijing China Graduate University of chinese academy of sciences Beijing China key Laboratory of Solar Activity National Astronomical Observatories of Chinese Academy of Sciences Beijing China

The SST(Space Solar Telescope) is an astronomical telescope with a primary mirror of 1 m in *** observes the sun with a small view field to ensure that its high spatial resolution imaging has 0.1″-0.15″ and high SNR(signal to noise ratio).Surrounding the small view field is still the sun,which is an intense source of both heat and stray *** baffles(the main baffle,the aperture,and the outer baffle),which are used to eliminate the stray light,will change the thermal flux in the SST and will weaken the effect of the thermal control *** this study,the compatibility analysis of the thermal effect of baffle structures in SST is *** GCF(Geometry Composing Function) and BRDF(Bidirectional Reflectance Distribution Function),which are two inherent related parameters in the compatibility analysis,are *** objective and method of the compatibility analysis are *** the thermal analysis software,the temperature fields are calculated for different lengths of the main baffle,different radii of apertures,different lengths of the outer baffle with a 3' tilt angle and 16' tilt angle,and different tilt angles of the outer baffle with a 2.0 mm length.A series of configurations and sizes of the baffles are studied with the goals of both thermal control and elimination of stray *** design of the baffle structure of SST is achieved:the main baffle of length 4100 mm,the internal shield of radius 494 mm,the outer baffle of length 2.0 mm,and the outer baffle of tilt angle 3' are successfully *** paper presents the relationship between the thermal control design and stray light elimination plan in the *** aims of the optimal design of the baffle structure of SST are *** thoughts and methods of the optimal analysis are also useful for similar optical telescopes designed for solar observation.

关键词： baffle the main baffle the outer baffle GCF BRDF

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The Filament Eruption of 1999 March 2. and Its Associated Coronal Dimmings and CME

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chinese Journal of Astronomy and Astrophysics 2006年第3期6卷 345-353页

作者： Yun-Chun Jiang Le-Ping li li-Heng Yang national astronomical Observatories/{2. observatory Chinese Academy of Sciences Kunming 650011

We report a filament eruption near the center of the solar disk on 1999 March 2., in multi-wavelength observations by the Yohkoh Soft X-Ray Telescope （SXT）, the Extremeultraviolet Images Telescope （EIT） and the Michelson Doppler Imager （MDI） on the Solar and Heliospheric observatory （SOHO）. The eruption involved in the disappearance of an Ha filament can be clearly identified in EIT 195A difference images. Two flare-like EUV ribbons and two obvious coronal dimming regions were formed. The two dimming regions had a similar appearance in lines formed in temperature range 6×10^4 K to several 10^6 K. They were located in regions of opposite magnetic polarities near the two ends of the eruptive filament. No significant X-ray or Hα flare was recorded associated with the eruption and no obvious photospheric magnetic activity was detected around the eruptive region, and particularly below the coronal dimming regions. The above surface activities were closely associated with a partial halo-type coronal mass ejection （CME） observed by the Large Angle and Spectrometric Coronagraphs （LASCO） on the SOHO. In terms of the magnetic flux rope model of CMEs, we explained these multiple observations as an integral process of largescale rearrangement of coronal magnetic field initiated by the filament eruption, in which the dimming regions marked the evacuated feet of the flux rope.

关键词： Sun: activity - Sun: filaments - Sun: coronal mass ejections(CMEs) - Sun:magnetic fields

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A network flow algorithm to position tiles for LAMOST

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Research in Astronomy and Astrophysics 2009年第11期9卷 1277-1284页

作者： Guang-Wei li and Gang Zhao national {2. Observatories, chinese academy of sciences, Beijing 100012. china national astronomical Observatories Chinese Academy of Sciences Beijing 100012 China

We introduce the network flow algorithm used by the Sloan Digital Sky Survey （SDSS） into the sky survey of the Large sky Area Multi-Object fiber Spectroscopic Telescope （LAMOST） to position tiles. Because fibers in LAMOST＇s focal plane are distributed uniformly, we cannot use SDSS＇ method directly. To solve this problem, firstly we divide the sky into many small blocks, and we also assume that all the targets that are in the same block have the same position, which is the center of the block. Secondly, we give a value to limit the number of the targets that the LAMOST focal plane can collect in one square degree so that it cannot collect too many targets in one small block. Thirdly, because the network flow algorithm used in this paper is a bipartite network, we do not use the general solution algorithm that was used by SDSS. Instead, we give our new faster solution method for this special network. Compared with the Convergent Mean Shift Algorithm, the network flow algorithm can decrease observation times with improved mean imaging quality. This algorithm also has a very fast running speed. It can distribute millions of targets in a few minutes using a common personal computer.

关键词： methods data analysis -- methods statistical

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Mineralization episode of porphyry copper deposits in the Jinshajiang-Red River mineralization belt: Re-Os dating

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Science china Earth sciences 2005年第2期48卷 192-198页

作者： WANG Denghong, QU Wenjun, li Zhiwei, YIN Hanlong4 & CHEN Yuchuan Institute of Mineral Resources, {2. academy of Geological sciences, Beijing 100037, china national Center of Rock and Mineral Analysis, {2. academy of Geological sciences, Beijing 100037, china Resource Assessment Center of yunnan, {12., china Institute of Geology and Geophysics, chinese academy of sciences, Beijing 100101, china {2. academy of Geological sciences, Beijing 100037, china Institute of Mineral Resources Chinese Academy of Geological Sciences Beijing China national Center of Rock and Mineral Analysis Chinese Academy of Geological Sciences Beijing China Resource Assessment Center of yunnan Kunming China Institute of Geology and Geophysics Chinese Academy of Sciences Beijing China chinese academy of Geological {2. Beijing China

Re-Os isotopic dating for the molybdenites from the porphyry copper deposits of the Jinshajiang-Red River mineralization belt in yunnan Province yields isochron ages of 33.9±1.1 Ma for the Machangqing deposit and 34.4±0.5 Ma for the Tongchang deposit. This result shows that both the Machangqing and the Tongchang porphyry Cu-Mo deposits from two different ore-fields formed simultaneously. This new data and the published Re-Os model ages of molybdenite (35.4 Ma, 35.9 Ma, 36.2.Ma) of the Yulong porphyry copper deposit in Tibet, which is located in the same Jinshajiang-Red River mineralization belt as the Machangqing deposit and the Tongchang deposit, suggest that these three Cenozoic porphyry copper deposits in the Jinshajiang-Red River mineralization belt were contemporary for their mineralization episode. That is to say, even their present locality is far away and nearly iso-distantly distributed, these three porphyry Cu(Mo) deposits belong to the same mineralization episode at the end of Eocene.

关键词： Re-Os isotopic dating, porphyry Cu deposits, Cenozoic, mineralization episode.

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Variability in Blazars

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天文研究与技术 2003年第S1期 107-116页

作者： Xie Guang zhong (national astronomical Observatories/{2. observatory,, CAS, {2. kunming 650011, P. R. china

In this report, a review of historical observations and studies to the variability in blazars is given. The variability timescale, in particular, the optical variability timescale, is emphasized owing to its importance. Three samples of three different kinds of variations are presented, and the corresponding models to interpret them are given. The long periodic variability is paid a lot of attention because which could be explained by the eclipses of the binary supermassive black holes (SMBHs). In addition, the observed evidences, such as the periodic outbursts in OJ 2.7, supporting the binary SMBHs model are also presented. A brief conclusion and prospect is presented at the end of this report.

关键词： Nature AS in Variability in Blazars ARA Mark

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Spectroscopic study of globular clusters in the halo of M31 with the Xinglong 2.16 m telescope

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Research in Astronomy and Astrophysics 2011年第11期11卷 1298-1310页

作者： Zhou Fan1,2.Ya-Fang Huang1,2.Jin-Zeng li1,2.Xu Zhou1,2.jun Ma1,2.Hong Wu1,2.Tian-Meng Zhang1,2.and Yong-Heng Zhao1,{2. national astronomical Observatories,chinese academy of sciences,Beijing 100012.china 2.key Laboratory of Optical Astronomy,national astronomical Observatories,chinese academy of sciences,Beijing 100012.china national astronomical Observatories Chinese Academy of Sciences Beijing 100012 China key Laboratory of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing 100012 China

We present spectroscopic observations for 11 confirmed globular clusters(GCs) of M31 with the OMR spectrograph on the 2.16 m telescope at the Xinglong site of national {2. Observatories,chinese academy of *** of our sample clusters are located in the halo of M31 and the most remote one is out to a projected radius of 78.75 kpc from the galactic *** all our sample clusters,we measured the lick absorption-line indices and radial *** is noted that most GCs in our sample are distinct from the HI rotation curve of galaxy M31,especially for B514,MCGC5,H12.and B517,suggesting that most of our sample clusters do not have a kinematic association with the star-forming young disk of the *** separately fitted the absorption line indices from the updated stellar population model of Thomas et *** two different tracks of Cassisi and Padova,by applying the χ2.minimization *** fitting results show that all our sample clusters are older than 10 Gyr,and metal-poor(2.38 ≤ [Fe/H] ≤ 0.91 dex).After merging the spectroscopic metallicity of our work with the previously published ones,we extended the cluster sample out to a projected radius of 117 kpc from the galaxy's *** found the metallicity gradient exists for all the confirmed clusters with a slope of 0.02. ± 0.001 dex kpc ***,the slope turns out to be 0.018 ± 0.001 dex kpc 1 for all the halo clusters,which is much *** we only consider the outer halo clusters with rp > 2. kpc,the slope becomes 0.010 ± 0.002.dex kpc 1 and if one cluster G001 is excluded from the outer halo sample,the slope is 0.004 ± 0.002.dex kpc ***,we conclude that the metallicity gradient for M31's outer halo clusters is not significant,which agrees well with previous findings.

关键词： galaxies individual(M31) — galaxies star clusters — globular clusters general — star clusters general

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Corrections to Solar Thermal Structure when a Turbulent Magnetic Field is Included

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chinese Journal of Astronomy and Astrophysics 2004年第5期4卷 490-498页

作者： Yiliao Shao-LanBi nationalastronomicalObservatories YunnanObservatoryKunming650011

Correction of non-ideal effect due to a magnetic fluctuating tensor is derived from the ideal MHD equations. The inclusion of a magnetic turbulent field leads to modifications of the hydrostatic equilibrium equation and thermodynamical variables such as the temperature T, the adiabatic exponent γ, the adiabatic temperature gradient ?ad and the temperature gradient ?. In particular, the modifications in the adiabatic and radiative temperature gradients will result in a change in the Schwarzchild criterion, hence in the location of the base of the convective zone. Incorporating the modifications, we construct a modified thermodynamical equilibrium structure of the Sun.

关键词： solar convection MHD: thermodynamics variables sun: hydrostatic equilibriumequation

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Features of the Solar Active Cycles

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天文研究与技术 1999年第S1期 447-451页

作者： li ke{2. (yunnan observatory, The chinese academy of sciences, kunming 650011, china)

Characteristics of the sunspot cycle described by the international sunspot numbers are investigated based on the results obtainned by Hathaway, Wilson, and Reichmann (1994). A long period of about 90 years is found to possibly exist for the sunspot number time series. Cycles that take less time to rise from minimum to maximum of cycle amp{2.tude tend to have large amp{2.tude, and those that have small maximum amp{2.tude tend to run a long time to get ended. It is also found in this paper that the more recent cycles are larger in amp{2.tude and shorter both in cycle length and the rising time of solar cycle than the ear{2.er ones.

关键词： sun: active cycles sun: activity sun: sunspots

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Multi-epoch X-ray observations of the narrow-line Seyfert 1 galaxy SDSS J160508.87+32.92..4 with XMM-Newton

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Science china(Physics,Mechanics & Astronomy) 2010年第S1期53卷 207-211页

作者： AI Yanli1,2.3,YUAN WeiMin1,2.ZHOU HongYan4,5 & WANG JianGuo1,2.3 1 national {2. 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 2.002.,china 5 Joint Institute of Galaxies and Cosmology,SHAO and USTC,Shanghai 2.0030,china national astronomical Observatories/{2. observatory Chinese Academy of Sciences Kunming China key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming China Graduate University of the chinese academy of sciences Beijing China Center for Astrophysics University of Science and Technology of China Hefei China Joint Institute of Galaxies and Cosmology SHAO and USTC Shanghai China

We present results of multi-epoch XMM-Newton observations separated by several years of the narrow-line Seyfert 1(NLS1) galaxy,SDSS J160508.87+*** 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 *** spectrum shows a significant soft X-ray *** 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-0.2. {2.V) cannot be ruled out in a statistical *** 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.

关键词： galaxies:active Seyfert X-rays individual

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Some Characteristic Parameters of the Basic Components of the Solar Radio Emission

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天文研究与技术 1999年第S1期 457-460页

作者： Ji Shuchen (Beijing astronomical observatory, The {2., Beijing 100080, china) (yunnan observatory, The {2., kunming 650011, china) (national astronomical Observatories, The {2.) $$

Four basic components of the solar radio emission: the quiet sun, the slowly varying component (SVC), the radio burst and the ultra-fast varying component (UFVC) are studied. As their six characteristic parameters: radiation source, brightness temperature, radiation lifetime, polarized radiation, radiation mechanism, and character of superposition are affirmed.

关键词： Radio Some Characteristic Parameters of the Basic Components Basic of the Solar Radio Emission

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