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Avoided crossings between non-radial modes in low mass RGB stars

Research in Astronomy and Astrophysics 2012年第12期12卷 1655-1665页

作者： jun-jun guo1,2.3.yan li1,2.and xiang-jun lai1,{3.,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 Chinese academy of sciences,Beijing 100049,china national astronomical observatories/{3. observatory Chinese Academy of Sciences Kunming 650011 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming 650011 China Graduate University of Chinese academy of sciences Beijing 100049 China

Non-radial p modes and g modes appear simultaneously in red giant stars. Their frequencies have different variation rates,causing their frequencies to become close during stellar evolution so that avoided crossings *** separation between regions where acoustic waves and gravity waves propagate for l=1,2.and 3.is different,which results in the coupling efficiency also being *** present the results of numerical computations of the models we *** find that the two kinds of modes for l=2.and 3.need to be closer in frequency in order for a complete exchange to occur,compared to the case for modes with l=*** scaled oscillation frequencies also present better regularity with evolution than modes with l=1. In order to study the effect of the avoided crossings in detail,we set the mode which has the smallest mode inertia to be the p *** plot the two kinds of modes for l =1,2.and 3.in frequency and periodéchelle diagrams and find modes of l=2.and 3.fit the two relations better;they are more equally spaced in frequency and period than modes with l=*** careful observation of the two kinds oféchelle diagrams for l=2.and 3.we still find that some p modes shift a little from being equally spaced in frequency and some g modes,which are close to those p modes in period,shift a little from being equally spaced in ***,we study the relation between the deviation from period being equally spaced and the mode inertia of g modes for different *** g modes of l=1 with a period closer to the p mode have less inertia and the deviation is bigger in the periodéchelle *** deviation is also obvious. However g modes of l=2.and 3.shift a little or have almost no deviation from being equally spaced in period,even though some of them may have strong coupling and close mode inertia like in the p ***,we suggest a possible method for measuring period spacing of g modes precisely using mixed g modes with l=2.and 3.that have fewer observed mixed g m

关键词： stars:oscillations-stars:red giants

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Observation of spectral lines in the exceptional GRB 2.1009A

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Science china(Physics,Mechanics & Astronomy) 2024年第8期67卷 187-206页

作者： yan-Qiu Zhang Shao-lin Xiong Ji-Rong Mao Shuang-Nan Zhang Wang-Chen Xue Chao Zheng Jia-Cong liu Zhen Zhang Xi-Lu Wang Ming-Yu Ge Shu-Xu Yi li-Ming Song Zheng-Hua An Ce Cai Xin-Qiao li Wen-Xi Peng Wen-jun Tan Chen-Wei Wang xiang-yang Wen Yue Wang Shuo Xiao Fan Zhang Peng Zhang Shi-Jie Zheng Key Laboratory of Particle Astrophysics Institute of High Energy PhysicsChinese Academy of SciencesBeijing 100049China University of Chinese academy of sciences Beijing 100049China yunnan observatories Chinese Academy of SciencesKunming 650011China Center for astronomical Mega-Science Chinese Academy of SciencesBeijing 100012China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of SciencesKunming 650216China College of Physics and Hebei Key Laboratory of Photophysics Research and Application Hebei Normal UniversityShijiazhuang 050024China Guizhou Provincial Key Laboratory of Radio Astronomy and Data Processing Guizhou Normal UniversityGuiyang 550001China College of Electronic and Information Engineering Tongji UniversityShanghai 201804China

As the brightest gamma-ray burst ever observed,GRB 2.1009A provided a precious opportunity to explore spectral line *** this article,we performed a comprehensive spectroscopy analysis of GRB 2.1009A jointly with GECAM-C and Fermi/GBM data to search for emission and absorption *** the first time we investigated the line feature throughout this GRB including the most bright part where many instruments suffered problems,and identified prominent emission lines in multiple time *** central energy of the Gaussian emission line evolves from about 3. to 6 MeV,with a nearly constant ratio(about 10%)between the line width and central ***,we find that both the central energy and the energy flux of the emission line evolve with time as a power law decay with power law index of–1 and–2,*** suggest that the observed emission lines most likely origin from the blue-shifted electron positron pair annihilation 511 ke V *** find that a standard high latitude emission scenario cannot fully interpret the observation,thus we propose that the emission line comes from some dense clumps with electron positron pairs traveling together with the *** this scenario,we can use the emission line to directly,for the first time,measure the bulk Lorentz factor of the jet(Γ)and reveal its time evolution(i.e.,Γ~t^(-1))during the prompt ***,we find that the flux of the annihilation line in the co-moving frame keeps *** discoveries of the spectral line features shed new and important lights on the physics of GRB and relativistic jet.

关键词： GRB GRB 2.1009A emission line

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Chemical mixing by turbulent convection in the overshooting region below the convective envelope of RGB stars

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Research in Astronomy and Astrophysics 2011年第11期11卷 1351-1370页

作者： xiang-jun lai {3. li national astronomical observatories / {3. observatory Chinese Academy of SciencesKunming 650011 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy ofSciences Kunming 650011 China Graduate University of Chinese academy of sciences Beijing 100049 China

Based on the turbulent convection model （TCM）, we investigate chemical mixing in the bottom overshooting region of the convective envelope of intermediatemass stars, focusing on its influence on the formation and extension of blue loops in the Hertzsprung-Russell （HR） diagram. A diffusive mixing model is adopted during the Red Giant Branch （RGB） phase. The properties of the blue loop are changed by modification of the element profiles above the H-burning shell, which results from the incomplete mixing in the bottom overshooting region when the stellar model evolves up along the RGB. Such modification of the element profiles will lead to an increase of opacity in the region just above the H-burning shell and a decrease of opacity in the outer homogeneous convection zone, which will result in a quick decrease of the H-shell nuclear luminosity LH when the stellar model evolves from the RGB tip to its bottom and, finally, a much weaker and smaller convection zone will be obtained in the stellar envelope. This helps to form a longer blue loop. The extension of the blue loop is very sensitive to the parameters （Cx and αTCM） of the diffusive mixing model and of the TCM. The results mainly show that： 1） comparing the results of the classical model with the mixing-length theory, the lengths of the obtained blue loops with different combinations of the values of Cx and αTCM are all increased and the length of the blue loop increases with the values of parameters Cx and αTCM; 2） the diffusive mixing model can significantly extend the time of stellar models lingering on the blue side of the HR diagram, even though the length of the blue loop for the 7M⊙ star has a less prominent difference between the classical and diffusive mixing model; 3. both the observations referring to the location of the Cepheid instability strip and the number ratio NB/NR of blue to red evolved stars in the Galactic open clusters can confine the two parameters in a range of 0.5 ≤ αLTCM ≤ 0.9 and 10-5 ≤

关键词： stars convection-star interiors-star HR diagram-blue loops-Cepheids-Galactic open clusters

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Characteristics of convection and overshooting in RGB and AGB stars

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Research in Astronomy and Astrophysics 2011年第10期11卷 1143-1157页

作者： xiang-jun lai {3. li national astronomical observatories / {3. observatory Chinese Academy of Sciences Kunming 650011 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy ofSciences Kunming 650011 China Graduate University of Chinese academy of sciences Beijing 100049 China.

Based on the turbulent convection model （TCM） of li ＆ yang, we have studied the characteristics of turbulent convection in the envelopes of 2.and 5M⊙ stars at the red giant branch and asymptotic giant branch phases. The TCM has been successfully applied over the entire convective envelopes, including the convective unstable zone and the overshooting regions. We find that the convective motions become progressively stronger when the stellar models are located farther up along the Hayashi line. In the convective unstable zone, we find that the turbulent correlations are proportional to functions of a common factor （V - V^d）T, which explains similar distributions in those correlations. For the TCM we find that if the obtained stellar temperature structure is close to that of the mixing length theory （MLT）, the convective motion will have a much larger velocity and thus be more violent. However, if the turbulent velocity is adjusted to be close to that of the MLT, the superadiabatic convection zone would be much more extended inward, which would lead to a lower effective temperature of the stellar model. For the overshooting distance, we find that the e-folding lengths of the turbulent kinetic energy k in both the top and bottom overshooting regions decrease as the stellar model is progressively located farther up along the Hayashi line, but both the extents of the decrease are not obvious. The overshooting distances of the turbulent correlation /u＇rT＂ are almost the same for the different stellar models with the same set of TCM parameters. For the decay modes of the kinetic energy k, we find that they are very similar for different stellar models based on the same set of TCM parameters, and there is a nearly linear relationship between lg k and In P for different stellar models. When Cs or α increases while the other parameters are fixed, the obtained linearly decaying distance will become longer.

关键词： stars RGB and AGB -- convection of stars -- turbulent convection model convective overshooting

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The first data release(DR1) of the LAMOST regular survey

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Research in Astronomy and Astrophysics 2015年第8期15卷 1095-1124页

作者： A-li Luo Yong-Heng Zhao Gang Zhao li-Cai Deng Xiao-Wei liu Yi-Peng Jing Gang Wang Hao-Tong Zhang Jian-Rong Shi {3.-Qun Cui Yao-Quan Chu guo-Ping li Zhong-Rui Bai Yue Wu yan Cai Shu-Yun Cao Zi-Huang Cao Jeffrey L.Carlin Hai-Yuan Chen Jian-jun Chen Kun-Xin Chen li Chen Xue-Lei Chen Xiao-yan Chen Ying Chen Norbert Christlieb Jia-Ru Chu Chen-Zhou Cui Yi-Qiao Dong Bing Du Dong-Wei Fan Lei Feng Jian-Ning Fu Peng Gao Xue-Fei Gong Bo-Zhong Gu yan-Xin guo Zhan-Wen Han Bo-liang He Jin-liang Hou Yong-Hui Hou Wen Hou Hong-Zhuan Hu Ning-Sheng Hu Zhong-Wen Hu Zhi-Ying Huo Lei Jia Fang-Hua Jiang {3. Jiang Zhi-Bo Jiang Ge Jin Xiao Kong Xu Kong Ya-Juan Lei Ai-Hua li Chang-Hua li Guang-Wei li Hai-Ning li Jian li Qi li Shuang li Sha-Sha li Xin-Nan li yan li Yin-Bi li Ye-Ping li Yuan liang Chien-Cheng lin Chao liu Gen-Rong liu Guan-Qun liu Zhi-Gang liu Wen-Zhi Lu Yu Luo Yin-Dun Mao Heidi Newberg Ji-jun Ni Zhao-{3. Qi Yong-jun Qi Shi-Yin Shen Huo-Ming Shi Jing Song Yi-Han Song Ding-Qiang Su Hong-jun Su Zheng-Hong Tang Qing-Sheng Tao Yuan Tian Dan Wang Da-Qi Wang Feng-Fei Wang guo-Min Wang Hai Wang Hong-Chi Wang Jian Wang Jia-Ning Wang Jian-ling Wang Jian-Ping Wang jun-Xian Wang Lei Wang Meng-Xin Wang Shou-Guan Wang Shu-Qing Wang Xia Wang Ya-Nan Wang You Wang Yue-Fei Wang You-Fen Wang Peng Wei Ming-Zhi Wei Hong Wu Ke-Fei Wu Xue-Bing Wu Yu-Zhong Wu Xiao-Zheng Xing ling-Zhe Xu Xin-Qi Xu yan Xu Tai-Sheng yan De-Hua yang Hai-Feng yang Hui-Qin yang Ming yang Zheng-Qiu Yao Yong Yu Hui Yuan Hai-Bo Yuan Hai-Long Yuan Wei-Min Yuan Chao Zhai En-Peng Zhang Hua-Wei Zhang Jian-Nan Zhang li-Pin Zhang Wei Zhang Yong Zhang yan-Xia Zhang Zheng-Chao Zhang Ming Zhao Fang Zhou Xu Zhou Jie Zhu Yong-Tian Zhu Si-Cheng Zou Fang Zuo national astronomical observatories Chinese Academy of Sciences Department of Astronomy Peking University Shanghai astronomical observatory Chinese Academy of Sciences Nanjing Institute of astronomical Optics & Technology National Astronomical ObservatoriesChinese Academy of Sciences University of Science and Technology of china Department of Physics Applied Physics and AstronomyRensselaer Polytechnic InstituteTroyNY 12180USA Department of Physics and Astronomy Earlham CollegeRichmondIN 47374USA Universitt Heidelberg Zentrum für AstronomieLandessternwarteKnigstuhl 1269117 HeidelbergGermany Department of Astronomy Beijing Normal University yunnan observatories Chinese Academy of Sciences Purple Mountain observatory Chinese Academy of Sciences

The Large sky Area Multi-Object Fiber Spectroscopic Telescope（LAMOST） general survey is a spectroscopic survey that will eventually cover approximately half of the celestial sphere and collect 10 million spectra of stars, galaxies and QSOs. Objects in both the pilot survey and the first year regular survey are included in the LAMOST DR1. The pilot survey started in October 2.11 and ended in june 2.12, and the data have been released to the public as the LAMOST Pilot Data Release in August 2.12. The regular survey started in September 2.12, and completed its first year of operation in june 2.13. The LAMOST DR1 includes a total of 1202 plates containing 2 955 3.6 spectra, of which 1 790 879 spectra have observed signalto-noise ratio（SNR） ≥ 10. All data with SNR ≥ 2 are formally released as LAMOST DR1 under the LAMOST data policy. This data release contains a total of 2 204 696 spectra, of which 1 944 3.9 are stellar spectra, 12 082 are galaxy spectra and 5017 are quasars. The DR1 not only includes spectra, but also three stellar catalogs with measured parameters： late A,FGK-type stars with high quality spectra（1 061 918 entries）, A-type stars（100 073.entries）, and M-type stars（121 522 entries）. This paper introduces the survey design, the observational and instrumental limitations, data reduction and analysis, and some caveats. A description of the FITS structure of spectral files and parameter catalogs is also provided.

关键词： techniques: spectroscopic survey—data release—catalog

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Long-term analysis of clear nights using satellite data considering astronomical sites in western china

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Research in Astronomy and Astrophysics 2020年第6期20卷 96-108页

作者： Zi-Huang Cao li-Yong liu Yong-Heng Zhao Lu Feng Hugh RAJones Huang Shen Jin-Xin Hao yan-Jie Xue Yong-Qiang Yao Jing Xu Ali Esamdin Zhao-xiang Qi Jian-Rong Shi Jian li Yuan Tian Zheng Wang Tai-Sheng yan Xia Wang Jian-Ping Xiong Si-Cheng Yu jun-Bo Zhang Zhi-Xia Shen Yun-Ying Jiang Jia Yin Guang-Xin Pu Peng Wei Chun-Hai Bai guo-Jie Feng Lu Ma Teng-Fei Song Jian-Feng Wang Jian-Feng Tian Xian-Qun Zeng Zhi-Gang Hou Shi-Long liao Zhi-Song Cao Dong-Wei Fan Yun-Fei Xu Chang-Hua li Yi-Han Tao national astronomical observatories Chinese Academy of SciencesBeijing 100101China University of Chinese academy of sciences Beijing 100049China Shanghai astronomical observatory Chinese Academy of SciencesShanghai 200030China Centre for Astrophysics University of HertfordshireHatfieldUK School of Journalism.Communication University of china Beijing 100024China Xinjiang astronomical observatory Chinese Academy of SciencesUrumqi 830011China yunnan observatories Chinese Academy of SciencesKunming 650216China

A large ground-based optical/infrared telescope is being planned for a world-class astronomical site in *** cloud-free night percentage is the primary meteorological consideration for evaluating candidate *** data from GMS and NOAA satellites and the MODIS instrument were utilized in this research,covering the period from 1996 to *** data analysis benefits from overlapping results from different independent teams as well as a uniform analysis of selected sites using GMS+NOAA *** significant ground-based monitoring is needed to validate these findings,we identify three different geographical regions with a high percentage of cloud-free conditions(~83.on average),which is slightly lower than at Mauna Kea and Cerro Armazones(~85%on average)and were chosen for the large international projects TMT and ELT *** study finds evidence that cloud distributions and the seasonal changes affected by the prevailing westerly winds and summer monsoons reduce the cloud cover in areas influenced by the *** is consistent with the expectations from climate change models and is suggestive that most of the identified sites will have reduced cloud cover in the future.

关键词： methods statistical-site testing-atmospheric effects-MODIS

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Data processing and data products from 2.17 to 2.19 campaign of astronomical site testing at A{3.,Daocheng and Muztagh-ata

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Research in Astronomy and Astrophysics 2020年第6期20卷 109-130页

作者： Zi-Huang Cao Jin-Xin Hao Lu Feng Hugh RAJones Jian li Jing Xu li-Yong liu Teng-Fei Song Jian-Feng Wang Hua-lin Chen yan-Jie Xue Huang Shen Yong-Heng Zhao Zhao-xiang Qi Jian-Rong Shi Yuan Tian Zheng Wang Xia Wang Jin-liang Hou Jin-Ming Bai Ji yang Xu Zhou Yong-Qiang Yao Jia Yin Ali Esamdin Guang-Xin Pu Peng Wei Chun-Hai Bai guo-Jie Feng Lu Ma Xuan Zhang Yu liu Chong Pei Zhi-Xia Shen Yun-Ying Jiang Jian-Feng Tian Xian-Qun Zeng Zhi-Gang Hou Xu yang jun-Bo Zhang Shi-Long liao Dong-Wei Fan Yun-Fei Xu Jian-Ping Xiong Tai-Sheng yan Xi Zhang Chang-Hua li Yi-Han Tao Si-Cheng Yu Zhi-Song Cao Hong-Shuai Wang national astronomical observatories Chinese Academy of SciencesBeijing 100101China University of Chinese academy of sciences Beijing 100049China Shanghai astronomical observatory Chinese Academy of SciencesShanghai 200030China Centre for Astrophysics University of HertfordshireHatfieldUK School of Journalism Communication University of ChinaBeijing 100024China Nanjing Institute of astronomical Optics&Technology Chinese Academy of SciencesNanjing 210042China Xinjiang astronomical observatory Chinese Academy of SciencesUrumqi 830011China yunnan observatories Chinese Academy of SciencesKunming 650216China Purple Mountain observatory Chinese Academy of SciencesNanjing 210033China Beijing Kaiyang Space Technology Co. LtdBeijing 100085China

Based on previous site testing and satellite cloud data,Ali,Daocheng and Muztagh-ata have been selected as candidate sites for the Large Optical/Infrared Telescope(LOT) in *** present the data collection,processing,management and quality analysis for our site testing based on using similar *** analyze meteorological data,seeing,background light,cloud and precipitable water vapor data from 2.17 March 10 to 2.19 March *** also investigated the relative usefulness of our all-sky camera data in comparison to that from the meteorological TERRA satellite data based on a night-by-night comparison of the correlation and consistency between *** find a 6% discrepancy arising from a wide range of factors.

关键词： LOT Site-selection-data processing

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利用GNSS差分的天线阵大气相位扰动实时修正方法

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光子学报 2020年第9期49卷 109-118页

作者：薛喜平李春来张洪波孔德庆董亮苏彦朱新颖戴舜李俊铎李臣武宇翔汪赞中国科学院国家天文台北京100101 中国科学院月球与深空探测重点实验室北京100101 中国科学院大学北京100049 中国科学院云南天文台昆明650000

提出了一种基于全球导航卫星系统差分的天线阵大气相位扰动实时修正方法,以高稳定度的原子钟作为外频标,利用导航卫星载波相位的单差与历元上的双差,并通过星历扣除由于卫星运动引起的相位变化,在周跳检测和修正后,通过长周期的拟合消... 详细信息

提出了一种基于全球导航卫星系统差分的天线阵大气相位扰动实时修正方法,以高稳定度的原子钟作为外频标,利用导航卫星载波相位的单差与历元上的双差,并通过星历扣除由于卫星运动引起的相位变化,在周跳检测和修正后,通过长周期的拟合消除卫星轨道和站坐标误差的影响,最后通过双频或多频信号实现两地电离层和对流层扰动的实时测量.在国家天文台北京密云站和云南昆明站分别部署了一套全球导航卫星接收设备,进行异地大气相位扰动实时修正方法的实验验证.利用双频载波相位测量数据对第三频率进行修正,结果表明,在不同天气条件下修正后的大气相位扰动均方根达到1.9mm,表明该方法可用于射电天文和深空探测中天线阵的大气相位扰动修正.

关键词：大气测量天线组阵全球导航卫星系统载波相位差分大气相位扰动

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Atlas of dynamic spectra of fast radio burst FRB 202.1124A

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Chinese Physics B 2023年第2期32卷 1-4页

作者：王铂钧胥恒姜金辰徐江伟牛佳瑞陈平李柯伽张冰朱炜玮东苏勃张春风傅海周德江张永坤王培冯毅李晔李冬子鲁文宾杨元培 RNCaballero 蔡策陈卯蒸戴子高艾力·伊沙木丁甘恒谦韩金林郝龙飞黄玉祥姜鹏李承奎李菂李辉李新乔李志玄刘志勇罗睿门云鹏牛晨辉彭文溪钱磊宋黎明孙京海王发印汪敏王娜王维扬吴雪峰肖硕熊少林徐永华徐仁新杨俊杨轩姚蕊易祁彬岳友岭于东俊余文飞袁建平张彬彬张松波张双南赵一郑伟康朱岩邹金航 Kavli Institute for Astronomy and Astrophysics Peking UniversityBeijing 100871China national astronomical observatories Chinese Academy of SciencesBeijing 100101China Department of Astronomy Peking UniversityBeijing 100871China University of Chinese academy of sciences Chinese Academy of SciencesBeijing 100049China Department of Particle Physics and Astrophysics Weizmann Institute of ScienceRehovot 76100Israel Nevada Center for Astrophysics University of NevadaLas VegasNV 89154USA Department of Physics and Astronomy University of NevadaLas VegasNV 89154USA Department of Physics&Astronomy University of IowaIowa CityIA 52242USA Zhejiang Laboratory HangzhouZhejiang 311121China Purple Mountain observatory Chinese Academy of SciencesNanjing 210008China TAPIR Walter Burke Institute for Theoretical PhysicsMail Code 350-17CaltechPasadenaCA 91125USA Department of Astronomy University of California at BerkeleyBerkeleyCA 94720USA South-Western Institute For Astronomy Research Yunnan UniversityYunnan 650504China Key Laboratory of Particle Astrophysics Institute of High Energy PhysicsChinese Academy of SciencesBeijing 100049China Xinjiang astronomical observatory Chinese Academy of SciencesUrumqi 830011China University of Science and Technology of china Anhui 230026China yunnan observatories Chinese Academy of SciencesKunming 650216China Guizhou Normal University Guiyang 550001China CSIRO Space and Astronomy EppingNSW 1710Australia Max-Planck institut fur Radioastronomie Auf Dem HugelBonn53121Germany School of Astronomy and Space Science Nanjing UniversityNanjing 210093China State Key Laboratory of Nuclear Physics and Technology School of PhysicsPeking UniversityBeijing 100871China Shanghai astronomical observatory Chinese Academy of SciencesShanghai 200030China Key Laboratory of Modern Astronomy and Astrophysics(Nanjing University) Ministry of EducationNanjing 210093China College of Physics Hebei Normal UniversityShijiazhuang 050024China

Fast radio bursts(FRBs) are highly dispersed millisecond-duration radio bursts,[1,2]of which the physical origin is still not fully understood. FRB 202.1124A is one of the most actively repeating FRBs. In this paper, we present the collection of 1863.burst dynamic spectra of FRB 202.1124A measured with the Five-hundred-meter Aperture Spherical radio Telescope(FAST). The current collection, taken from the observation during the FRB active phase from April to {3.e 2021, is the largest burst sample detected for any FRB so far. The standard PSRFITs format is adopted, including dynamic spectra of the burst, and the time information of the dynamic spectra, in addition, mask files help readers to identify the pulse positions are also provided. The dataset is available in Science Data Bank, with the link https://***/10.57760/sciencedb.j00113.00076.

关键词： fast radio burst FAST

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