YNAO OpenIR研究单元&专题: 其他
http://ir.ynao.ac.cn:80/handle/114a53/49
2024-03-29T07:42:36Z
2024-03-29T07:42:36Z
The ALMA Survey of Star Formation and Evolution in Massive Protoclusters with Blue Profiles (ASSEMBLE): Core Growth, Cluster Contraction, and Primordial Mass Segregation
Xu, Fengwei
Wang, Ke
Liu, Tie
Tang, Mengyao
II, Neal J. Evans
Palau, Aina
Morii, Kaho
何金华
Sanhueza, Patricio
Liu, Hong-Li
Stutz, Amelia
Zhang, Qizhou
Chen, Xi
Li, Pak Shing
Gómez, Gilberto C.
Vázquez-Semadeni, Enrique
Li, Shanghuo
Mai, Xiaofeng
Lu, Xing
Liu, Meizhu
Chen, Li
Li, Chuanshou
Shi, Hongqiong
Ren, Zhiyuan
Li, Di
Garay, Guido
Bronfman, Leonardo
Dewangan, Lokesh
Juvela, Mika
Lee, Chang Won
Zhang, S.
Yue, Nannan
Wang, Chao
Ge, Yifei
Jiao, Wenyu
Luo, Qiuyi
Zhou, J.-W.
Tatematsu, Ken'ichi
Chibueze, James O.
Su, Keyun
Sun, Shenglan
Ristorcelli, I.
Toth, L. Viktor
http://ir.ynao.ac.cn:80/handle/114a53/26479
2024-03-29T05:33:16Z
2024-03-29T05:33:16Z
题名: The ALMA Survey of Star Formation and Evolution in Massive Protoclusters with Blue Profiles (ASSEMBLE): Core Growth, Cluster Contraction, and Primordial Mass Segregation
作者: Xu, Fengwei; Wang, Ke; Liu, Tie; Tang, Mengyao; II, Neal J. Evans; Palau, Aina; Morii, Kaho; 何金华; Sanhueza, Patricio; Liu, Hong-Li; Stutz, Amelia; Zhang, Qizhou; Chen, Xi; Li, Pak Shing; Gómez, Gilberto C.; Vázquez-Semadeni, Enrique; Li, Shanghuo; Mai, Xiaofeng; Lu, Xing; Liu, Meizhu; Chen, Li; Li, Chuanshou; Shi, Hongqiong; Ren, Zhiyuan; Li, Di; Garay, Guido; Bronfman, Leonardo; Dewangan, Lokesh; Juvela, Mika; Lee, Chang Won; Zhang, S.; Yue, Nannan; Wang, Chao; Ge, Yifei; Jiao, Wenyu; Luo, Qiuyi; Zhou, J.-W.; Tatematsu, Ken'ichi; Chibueze, James O.; Su, Keyun; Sun, Shenglan; Ristorcelli, I.; Toth, L. Viktor
摘要: The Atacama Large Millimeter/submillimeter Array (ALMA) Survey of Star Formation and Evolution in Massive Protoclusters with Blue Profiles (ASSEMBLE) aims to investigate the process of mass assembly and its connection to high-mass star formation theories in protoclusters in a dynamic view. We observed 11 massive (M clump greater than or similar to 103 M circle dot), luminous (L bol greater than or similar to 104 L circle dot), and blue-profile (infall signature) clumps by ALMA with resolution of similar to 2200-5500 au (median value of 3500 au) at 350 GHz (870 mu m). We identified 248 dense cores, including 106 cores showing protostellar signatures and 142 prestellar core candidates. Compared to early stage infrared dark clouds (IRDCs) by ASHES, the core mass and surface density within the ASSEMBLE clumps exhibited a significant increment, suggesting concurrent core accretion during the evolution of the clumps. The maximum mass of prestellar cores was found to be 2 times larger than that in IRDCs, indicating that evolved protoclusters have the potential to harbor massive prestellar cores. The mass relation between clumps and their most massive core (MMCs) is observed in ASSEMBLE but not in IRDCs, which is suggested to be regulated by multiscale mass accretion. The mass correlation between the core clusters and their MMCs has a steeper slope compared to that observed in stellar clusters, which can be due to fragmentation of the MMC and stellar multiplicity. We observe a decrease in core separation and an increase in central concentration as protoclusters evolve. We confirm primordial mass segregation in the ASSEMBLE protoclusters, possibly resulting from gravitational concentration and/or gas accretion.
2024-03-29T05:33:16Z
The ALMA-QUARKS Survey. I. Survey Description and Data Reduction
Liu, Xunchuan
Liu, Tie
Zhu, Lei
Garay, Guido
Liu, Hong-Li
Goldsmith, Paul
Evans, Neal
Kim, Kee-Tae
Liu, Sheng-Yuan
Xu, Fengwei
Lu, Xing
Tej, Anandmayee
Mai, Xiaofeng
Bronfman, Leonardo
Li, Shanghuo
Mardones, Diego
Stutz, Amelia
Tatematsu, Ken'ichi
Wang, Ke
Zhang, Qizhou
Qin, Sheng-Li
Zhou, Jianwen
Luo, Qiuyi
Zhang, Siju
Cheng, Yu
何金华
Gu, Qilao
Li, Ziyang
Zhang, Zhenying
Zhang, Suinan
Saha, Anindya
Dewangan, Lokesh
Sanhueza, Patricio
Shen, Zhiqiang
http://ir.ynao.ac.cn:80/handle/114a53/26436
2024-03-29T05:31:05Z
2024-03-29T05:31:05Z
题名: The ALMA-QUARKS Survey. I. Survey Description and Data Reduction
作者: Liu, Xunchuan; Liu, Tie; Zhu, Lei; Garay, Guido; Liu, Hong-Li; Goldsmith, Paul; Evans, Neal; Kim, Kee-Tae; Liu, Sheng-Yuan; Xu, Fengwei; Lu, Xing; Tej, Anandmayee; Mai, Xiaofeng; Bronfman, Leonardo; Li, Shanghuo; Mardones, Diego; Stutz, Amelia; Tatematsu, Ken'ichi; Wang, Ke; Zhang, Qizhou; Qin, Sheng-Li; Zhou, Jianwen; Luo, Qiuyi; Zhang, Siju; Cheng, Yu; 何金华; Gu, Qilao; Li, Ziyang; Zhang, Zhenying; Zhang, Suinan; Saha, Anindya; Dewangan, Lokesh; Sanhueza, Patricio; Shen, Zhiqiang
摘要: This paper presents an overview of the QUARKS survey, which stands for 'Querying Underlying mechanisms of massive star formation with ALMA-Resolved gas Kinematics and Structures'. The QUARKS survey is observing 139 massive gas clumps covered by 156 pointings at ALMA Band 6 (lambda similar to 1.3 mm). In conjunction with data obtained from the ALMA-ATOMS survey at Band 3 (lambda similar to 3 mm), QUARKS aims to carry out an unbiased statistical investigation of massive star formation process within protoclusters down to a scale of 1000 au. This overview paper describes the observations and data reduction of the QUARKS survey, and gives a first look at an exemplar source, the mini-starburst Sgr B2(M). The wide-bandwidth (7.5 GHz) and high-resolution (similar to 0.'' 3) observations of the QUARKS survey allow to resolve much more compact cores than could be done by the ATOMS survey, and to detect fainter filamentary structures that were not revealed earlier. The spectral windows cover transitions of species including CO, SO, N2D+, SiO, H30 alpha, H2CO, CH3CN and many other complex organic molecules, tracing gas components with different temperatures and spatial extents. QUARKS aims to deepen our understanding of several scientific topics of massive star formation, such as mass transport within protoclusters by (hub-)filamentary structures, the existence of massive starless cores, the physical and chemical properties of dense cores within protoclusters, and the feedback from already formed high-mass young protostars.
2024-03-29T05:31:05Z
OH as a probe of the warm-water cycle in planet-forming disks
Zannese, Marion
Tabone, Benoît
Habart, Emilie
Goicoechea, Javier R.
Zanchet, Alexandre
Dishoeck, Ewine F. van
Hemert, Marc C. van
Black, John H.
Tielens, Alexander G. G. M.
Veselinova, A.
Jambrina, P. G.
Menendez, M.
Verdasco, E.
Aoiz, F. J.
Gonzalez-Sanchez, L.
Trahin, Boris
Dartois, Emmanuel
Berné, Olivier
Peeters, Els
何金华
Sidhu, Ameek
Chown, Ryan
Schroetter, Ilane
Putte, Dries Van De
Canin, Amélie
Alarcón, Felipe
Abergel, Alain
Bergin, Edwin A.
Bernard-Salas, Jeronimo
Boersma, Christiaan
Bron, Emeric
Cami, Jan
Dicken, Daniel
Elyajouri, Meriem
Fuente, Asunción
Gordon, Karl D.
Issa, Lina
Joblin, Christine
Kannavou, Olga
Khan, Baria
Languignon, David
Gal, Romane Le
Maragkoudakis, Alexandros
Meshaka, Raphael
Okada, Yoko
Onaka, Takashi
Pasquini, Sofia
Pound, Marc W.
Robberto, Massimo
Röllig, Markus
Schefter, Bethany
Schirmer, Thiébaut
Vicente, Sílvia
Wolfire, Mark G.
http://ir.ynao.ac.cn:80/handle/114a53/26429
2024-03-29T05:30:08Z
2024-03-29T05:30:08Z
题名: OH as a probe of the warm-water cycle in planet-forming disks
作者: Zannese, Marion; Tabone, Benoît; Habart, Emilie; Goicoechea, Javier R.; Zanchet, Alexandre; Dishoeck, Ewine F. van; Hemert, Marc C. van; Black, John H.; Tielens, Alexander G. G. M.; Veselinova, A.; Jambrina, P. G.; Menendez, M.; Verdasco, E.; Aoiz, F. J.; Gonzalez-Sanchez, L.; Trahin, Boris; Dartois, Emmanuel; Berné, Olivier; Peeters, Els; 何金华; Sidhu, Ameek; Chown, Ryan; Schroetter, Ilane; Putte, Dries Van De; Canin, Amélie; Alarcón, Felipe; Abergel, Alain; Bergin, Edwin A.; Bernard-Salas, Jeronimo; Boersma, Christiaan; Bron, Emeric; Cami, Jan; Dicken, Daniel; Elyajouri, Meriem; Fuente, Asunción; Gordon, Karl D.; Issa, Lina; Joblin, Christine; Kannavou, Olga; Khan, Baria; Languignon, David; Gal, Romane Le; Maragkoudakis, Alexandros; Meshaka, Raphael; Okada, Yoko; Onaka, Takashi; Pasquini, Sofia; Pound, Marc W.; Robberto, Massimo; Röllig, Markus; Schefter, Bethany; Schirmer, Thiébaut; Vicente, Sílvia; Wolfire, Mark G.
摘要: Water is a key ingredient for the emergence of life as we know it. Yet, its destruction and reformation in space remain unprobed in warm gas (T > 300 K). Here we detect with the James Webb Space Telescope the emission of the hydroxyl radical (OH) from d203-506, a planet-forming disk exposed to external far-ultraviolet (FUV) radiation. These observations were made as part of the Early Release Science programme PDRs4All, which is focused on the Orion bar. The observed OH spectrum is compared with the results of quantum dynamical calculations to reveal two essential molecular processes. The highly excited rotational lines of OH in the mid-infrared are telltale signs of H2O destruction by FUV radiation. The OH rovibrational lines in the near-infrared are attributed to chemical excitation by the key reaction O + H-2 -> OH + H, which seeds the formation of water in the gas phase. These results show that under warm and irradiated conditions, water is destroyed and efficiently reformed through gas-phase reactions. We infer that, in this source, the equivalent of Earth oceans' worth of water is destroyed per month and replenished. This warm-water cycle could reprocess some water inherited from cold interstellar clouds and explain the lower deuterium fraction of water in Earth's oceans compared with that found around protostars.
2024-03-29T05:30:08Z
一种基于宽带动态选频的多通道太阳射电流量监测系统
董亮
朱琳玲
潘业欣
敦金平
闫凯
王云冈
郭少杰
高冠男
http://ir.ynao.ac.cn:80/handle/114a53/26191
2023-09-18T02:15:56Z
2023-09-18T02:09:47Z
题名: 一种基于宽带动态选频的多通道太阳射电流量监测系统
作者: 董亮; 朱琳玲; 潘业欣; 敦金平; 闫凯; 王云冈; 郭少杰; 高冠男
摘要: 本申请涉及一种基于宽带动态选频的多通道太阳射电流量监测系统,其中,该系统包括接收模块,用于接收第一频段内的第一信号,并传输至下位机;第一信号包括太阳射电信号和无线电干扰信号;下位机,用于将第一信号转换为第一数字信号,并对第一数字信号进行频域分析,得到第一频谱数据,将第一频谱数据上传至上位机;上位机,用于获取多个监测频段,并在多个监测频段内监测太阳射电流量;其中,监测频段根据第一频谱数据在第一频段内确定;监测频段内的第二信号中不存在无线电干扰信号;本申请提供的太阳射电流量监测系统可以有效地规避无线电干扰信号的影响,实现太阳射电流量的稳定监测。
2023-09-18T02:09:47Z
Infrared photometric study of dust obscured galaxies
Chen PS(陈培生)
Liu JY(刘杰英)
http://ir.ynao.ac.cn:80/handle/114a53/26150
2023-08-14T03:40:12Z
2023-08-14T03:23:47Z
题名: Infrared photometric study of dust obscured galaxies
作者: Chen PS(陈培生); Liu JY(刘杰英)
摘要: <p>We have collected almost all published dust obscured galaxies (DOGs) with the certain coordinate in the literature (817 DOGs in total) to investigate their infrared properties by using 2MASS (and other observations in the JHK bands), WISE, IRAS and Herschel data in this paper. Our study shows that objects with different types have different presentations for the relations between the redshift and infrared colors. It is also found that in the near infrared two-color diagram, DOGs are distributed across the blackbody line and the power law line indicative of the thermal emission from the stellar component and the star formation for some objects, and the AGN dominated for other objects in the near infrared. However, in the two-color diagrams with longer wavelengths the majority of DOGs are distributed around the power law line indicative of the central AGN dominated in the midinfrared, far infrared, and submillimeter regions. We also compared the infrared color propertes between DOGs and ULIRGs. It is found that, statistically, ULIRGs have redder colors than that for DOGs in the near and midinfrared region while compared with DOGs, ULIRGs are more near the blackbody line indicative of the star formation dominated in far infrared.</p>
2023-08-14T03:23:47Z
基于丽江10cm日冕仪的镜面尘埃杂散光研究
沙飞扬
刘煜
张雪飞
宋腾飞
张洪起
王永峰
孙明哲
http://ir.ynao.ac.cn:80/handle/114a53/26091
2023-07-10T02:25:27Z
2023-07-03T09:38:20Z
题名: 基于丽江10cm日冕仪的镜面尘埃杂散光研究
作者: 沙飞扬; 刘煜; 张雪飞; 宋腾飞; 张洪起; 王永峰; 孙明哲
摘要: <p>The solar corona is the outermost layer of the solar atmosphere, consisting of thin, highly ionized and hot plasma. In visible light, the solar corona is much dimmer than the photosphere, only one millionth as bright, so it is not visible in daylight. The only exception is during a total solar eclipse, when the moon blocks the light from the photosphere completely and reveals the corona. The coronagraph is a special telescope that can observe the solar corona even in the absence of a total solar eclipse. It creates an artificial eclipse by using an occulter to block the bright photosphere. Depending on the location of the occulter, there are two main types of coronagraphs: externally occulted and internally occulted. The externally occulted coronagraph blocks the direct sunlight with an occulter in front of the objective lens, but it also causes some vignetting in the field of view, which affects the quality of the observations. The internally occulted coronagraph has the occulter behind the objective lens, however, this means that some parts of the telescope, such as the objective lens and the tube, are exposed to direct sunlight and produce a lot of stray light, which needs to be strictly suppressed. The stray light of the internally occulted coronagraph can be divided into two parts: fixed and variable. The former does not change with time and environmental cleanliness, while the latter increases with decreasing environmental cleanliness. For the ground-based internally occulted coronagraph with regular observations, the scattering from dust on the objective surface is the variable stray light, as the dust continues to accumulate on the surface. Although the accumulation can be slowed down by frequent cleaning of the objective surface and the level of this stray light can be suppressed, the objective surface cannot be guaranteed to remain clean throughout the observation due to weather, atmospheric particle pollution and other factors. More importantly, this approach is somewhat subjective, as the observer cannot directly assess the current level of mirror cleanliness, resulting in an untimely cleaning and multiple disassembly of the objective lens, creating secondary contamination on the objective surface to some extent. So, the stray light levels are changing over time, leading to different amounts of scattered background in the coronal data, which brings great inconvenience in the analysis of the faint coronal structure and the coronal intensity calibration. We performed an experiment to explore how the amount of dust on the objective surface affects the intensity of the scattering background in the coronal image plane. We used the Lijiang 10 cm Lyot Coronagraph (Yunnan Observatories Green-line Imaging System, YOGIS), an internally occulted coronagraph that operates at a wavelength of 530. 3 nm and has a main focal length of 1490 millimeters. YOGIS is a joint project between the Yunnan Observatories and the National Astronomical Observatory of Japan, and it is the only ground-based coronagraph in China that can perform regular observations, which has a total length of nearly 3 meters and a weight of 100 kilograms, and uses a CMOS camera with 2 048× 2 048. The experiment was conducted at Lijiang Observatory (E100° 01 ′4 ″, N26° 41 ′42 ″), which is located at an altitude of 3 200 meters and has low atmospheric scattering, making it ideal for ground-based solar corona observation. Two experimenters and one observation assistant participated in the experiment on November 17, 2022, when the sky was clear and cloudless. The main goal of the experiment is to obtain dust information and measure its impact on the coronal image, called scattering background. To obtain dust data, we need the conjugate imaging of the objective lens. We achieve this by pointing the coronagraph at the sun and placing the camera at lens' focal plane. The resulting image has three parts. Firstly, light scattered by surface microroughness, which remains constant regardless of the cleanness level. Secondly, light scattered by dust particles on the objective surface, which varies depending on how clean it is. Finally, the light scattered by the earth's atmospheric is scattered by surface microroughness and dust particles, which is negligible compared to the second part. We use Otsu's method to process the image into binary pixels that show each particles' area, which tell us about its area and intensity. Assuming that the dust is distributed evenly on objective surface, we use total intensity (I) as a measure for dust information. To get the scattering background, we take two images of corona: one before and the other after cleaning the objective surface, and then align and subtract them. To account for the change in solar brightness, we normalize the two images by dividing them by their respective solar radiation intensities before subtraction. Based on the above two aspects, we conducted the experiments with the following steps. Firstly, we imaged lens and corona with significant dust on objective surface. Then we cleaned it and imaged again. This gave us scattering background and its related dust scattering points' intensity (I). Then, we converted this image into polar coordinates and took median intensities for each radius. This showed us that the scattering background decreased linearly with distance. We also saw that the slope and intercept of this linear equation depended linearly on dust intensity (I). Hence, we derived the function of the scattering background with respect to the distance and the total intensity of the scattering points( I). We can use these relationships to create different scattering background based on different intensities (I), and then subtract them from the corresponding coronal images to get the corrected ones. Our model is validated by comparing the intensity decay curves of the corrected coronal images with those of the clean images, which are similar. Our method not only effectively improves the quality of coronal data, but also makes faint coronal structure more prominent and clearer, which helps us to obtain more accurate results when analyzing the intensity decay trend of the inner corona and coronal structure changes. What's more, it will help us to further understand the effects of other stray light sources inside the coronagraph, helping the further technological development of large-aperture coronagraphs.</p>
摘要: <p>利用云南天文台丽江10 cm日冕仪绿线成像系统研究了物镜表面尘埃量级与其造成的散射杂散光强度的关系,获得了散射光随日心距离的分布规律,并对日冕图像进行了修正。得到了不含尘埃散射杂散光背景的日冕图像,提高了数据质量。本文研究有助于研究日冕强度、结构变化趋势,也有助于理解日冕仪内部其他杂散光源,助力我国未来大口径日冕仪的研发。 </p>
2023-07-03T09:38:20Z
Evidence of high-mass star formation through multiscale mass accretion in hub-filament-system clouds
Liu, Hong-Li
Tej, Anandmayee
Liu, Tie
Sanhueza, Patricio
Qin, Sheng-Li
He JH(何金华)
Goldsmith, Paul F.
Garay, Guido
Pan, Sirong
Morii, Kaho
Li, Shanghuo
Stutz, Amelia
Tatematsu, Ken'ichi
Xu, Feng-Wei
Bronfman, Leonardo
Saha, Anindya
Issac, Namitha
Baug, Tapas
Toth, L. Viktor
Dewangan, Lokesh
Wang, Ke
Zhou, Jianwen
Lee, Chang Won
Yang, Dongting
Luo, Anxu
Shen, Xianjin
Zhang, Yong
Wu, Yue-Fang
Ren, Zhiyuan
Liu, Xun-Chuan
Soam, Archana
Zhang, Siju
Luo, Qiu-Yi
http://ir.ynao.ac.cn:80/handle/114a53/26036
2023-07-17T02:44:15Z
2023-06-05T06:17:28Z
题名: Evidence of high-mass star formation through multiscale mass accretion in hub-filament-system clouds
作者: Liu, Hong-Li; Tej, Anandmayee; Liu, Tie; Sanhueza, Patricio; Qin, Sheng-Li; He JH(何金华); Goldsmith, Paul F.; Garay, Guido; Pan, Sirong; Morii, Kaho; Li, Shanghuo; Stutz, Amelia; Tatematsu, Ken'ichi; Xu, Feng-Wei; Bronfman, Leonardo; Saha, Anindya; Issac, Namitha; Baug, Tapas; Toth, L. Viktor; Dewangan, Lokesh; Wang, Ke; Zhou, Jianwen; Lee, Chang Won; Yang, Dongting; Luo, Anxu; Shen, Xianjin; Zhang, Yong; Wu, Yue-Fang; Ren, Zhiyuan; Liu, Xun-Chuan; Soam, Archana; Zhang, Siju; Luo, Qiu-Yi
摘要: <p>We present a statistical study of a sample of 17 hub-filament-system (HFS) clouds of high-mass star formation using high-angular resolution (∼1-2 arcsec) ALMA 1.3 and 3 mm continuum data. The sample includes eight infrared (IR)-dark and nine IR-bright types, which correspond to an evolutionary sequence from the IR-dark to IR-bright stage. The central massive clumps and their associated most massive cores are observed to follow a trend of increasing mass (M) and mass surface density (∑) with evolution from the IR-dark to IR-bright stage. In addition, a mass-segregated cluster of young stellar objects (YSOs) are revealed in both IR-dark and IR-bright HFSs with massive YSOs located in the hub and the population of low-mass YSOs distributed over larger areas. Moreover, outflow feedback in all HFSs are found to escape preferentially through the inter-filamentary diffuse cavities, suggesting that outflows would render a limited effect on the disruption of the HFSs and ongoing high-mass star formation therein. From the above observations, we suggest that high-mass star formation in the HFSs can be described by a multiscale mass accretion/transfer scenario, from hub-composing filaments through clumps down to cores, which can naturally lead to a mass-segregated cluster of stars. © 2023 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society.</p>
2023-06-05T06:17:28Z
50 mm白光球载日冕仪:Ⅰ.基本结构与地面观测实验
林隽
宋腾飞
孙明哲
张涛
许方宇
王晶星
付玉
李燕
康凯锋
黄旻
刘洋
周江华
张晓军
夏利东
张红鑫
刘大洋
宋红强
田晖
皮晓宇
伏红林
张雪飞
赵明宇
刘煜
李语强
金振宇
宋海军
http://ir.ynao.ac.cn:80/handle/114a53/25893
2023-04-24T03:05:25Z
2023-04-24T03:02:47Z
题名: 50 mm白光球载日冕仪:Ⅰ.基本结构与地面观测实验
作者: 林隽; 宋腾飞; 孙明哲; 张涛; 许方宇; 王晶星; 付玉; 李燕; 康凯锋; 黄旻; 刘洋; 周江华; 张晓军; 夏利东; 张红鑫; 刘大洋; 宋红强; 田晖; 皮晓宇; 伏红林; 张雪飞; 赵明宇; 刘煜; 李语强; 金振宇; 宋海军
摘要: <p>A 50-mm balloon-borne white-light coronagraph was introduced in the study, which was a traditional Lyot coronagraph, with a working wavelength of 5500 Å and a passband of 50 Å for observing the inner corona from 1. 08 R⊙ to 1. 5 R⊙. Dhyana 95V2-YNTT sCMOS was used to collect the observational data. Three experiments were conducted on the ground. The first experiment was conducted at the Gaomeigu Station, Lijiang, Yunnan, and the other two were conducted at the Wumingshan mountain in Daocheng, Sichuan, approximately 4800 m above sea level. The data with scientific significance were obtained in the latter two experiments. Comparison of our data with those obtained by the K-cor of the 20-cm aperture of the High Altitude Observatory at the Mauna Loa Solar Observatory on the same days verified the consistency of the two datasets, indicating the successful development of the white-light coronagraph. The brightness of the background sky indicates that Wumingshan is an ideal high altitude site for solar observations.</p>
摘要: <p>本文介绍一台口径为50 mm、用于在浮空平台上进行观测的白光日冕仪.工作波段为5500?,透过带宽为50?,为传统的Lyot式日冕仪,可观测1.08–1.50个太阳半径范围的内日冕.用鑫图的Dhyana 95V2-YNTT sCMOS相机采集观测数据.对日冕仪进行了三次地面观测实验:第一次在云南丽江高美古观测站进行,另两次在海拔4800 m左右的四川稻城无名山观测站进行,后两次实验获得了较为理想的日冕白光观测数据.与美国高山天文台的20 cm口径K-cor日冕仪在同一天之内观测到的结果基本一致,说明白光日冕仪的研制获得成功.同时获得的天空背景亮度表明,稻城无名山是一处较为理想的高海拔太阳观测址点. </p>
2023-04-24T03:02:47Z
一种抵近太阳探测器供电系统和方法
黄善杰
张涛
许方宇
宋腾飞
http://ir.ynao.ac.cn:80/handle/114a53/25882
2023-04-03T09:17:52Z
2023-04-03T09:14:03Z
题名: 一种抵近太阳探测器供电系统和方法
作者: 黄善杰; 张涛; 许方宇; 宋腾飞
摘要: 本发明涉及一种抵近太阳探测器供电系统和方法,该系统包括:设于第一太阳能电池板的第一太阳辐射功率计;设于第二太阳能电池板的第二太阳辐射功率计;设于热防护罩上的热电转换装置;设置于热防护罩背部的温度传感器;第一太阳辐射功率计、第二太阳辐射功率计、温度传感器与控制中心连接;第一太阳能电池板、第二太阳能电池板、热电转换装置与储电装置连接。本发明可以让抵近太阳探测器在不同强弱太阳辐照下稳定供电,且保证太阳能电池板不被强太阳辐射烧坏。
2023-04-03T09:14:03Z
上海临港新城天文气象条件统计研究
杜芝茂
姚嵩
林清
宋腾飞
王晶星
陆琦
彭博
http://ir.ynao.ac.cn:80/handle/114a53/25865
2023-03-20T05:51:13Z
2023-03-20T05:14:23Z
题名: 上海临港新城天文气象条件统计研究
作者: 杜芝茂; 姚嵩; 林清; 宋腾飞; 王晶星; 陆琦; 彭博
摘要: <p>Shanghai Astronomy Museum is located in Lingang New City, Pudong New Area, Shanghai, was completed in July 2021. The aim is to understand the astronomical and meteorological conditions in the area, and give advice to improve the observation of the astronomical telescope. The humidity, dew point, wind speed, wind direction and temperature were recorded in Lingang Area and were systematically statistically analyzed. It is found that the temperature in this area is suitable, with an average temperature of 16. 7 ℃; The humidity is relatively high, the annual average humidity is 76. 9%, the wind speed is stable, and the annual average wind speed is 1. 9 m/s. The meteorological laws related to astronomical observation in Lingang New City are studied, and it is feasible to build an observatory in Lingang area to carry out astronomical observation.</p>
摘要: <p>上海天文馆落户于上海市浦东新区临港新城,2021年7月已经建成使用。为了解该地区的天文气象条件,以便对天文望远镜的观测优化提出参考意见。该文对临港新城的湿度、露点、风速、风向、气温这几个气象条件进行了系统的统计分析,发现该地区温度适宜,平均温度为16.7℃;湿度偏大,年平均湿度为76.9%;风速稳定,年平均风速为1.9 m/s。研究了临港新城与天文观测相关的气象规律,认为在临港地区建设天文台开展天文观测是可行的。 </p>
2023-03-20T05:14:23Z