Vector Magnetograph Observations by the Solar Flare Telescope at Boao

1　ＩｎｔｒｏｄｕｃｔｉｏｎＡｆｉｌｔｅｒ ｂａｓｅｄｖｅｃｔｏｒｍａｇｎｅｔｏｇｒａｐｈｉｓａｔｔａｃｈｅｄｔｏｔｈｅＳｏｌａｒＦｌａｒｅＴｅｌｅｓｃｏｐｅ (Ｍｏｏｎｅｔａｌ.1 996 ,Ｐａｒｋｅｔａｌ.1 997)ａｔｔｈｅＢｏｈｙｕｎｓａｎＯｐｔｉｃａｌＡｓｔｒｏｎｏｍｙＯｂｓｅｒｖａｔｏｒｙ (ＢＯＡＯ) ,ＷｈｉｃｈｕｓｅｄａｖｅｒｙｎａｒｒｏｗｂａｎｄＬｙｏｔｆｉｌｔｅｒａｎｄＫＤ Ｐｃｒｙｓｔａｌｓｆｏｒｐｏｌａｒｉｍｅｔｒｉｃｏｂｓｅｒｖａｔｉｏｎｓ .ＴｈｅＳｔｏｋｅｓｐａ ｒａｍｅｔｅｒｓａｒｅｍ…     

Infrared Observations from the New Solar Telescope at Big Bear

The 1.6 m clear aperture solar telescope in Big Bear is operational and with its adaptive optics (AO) system it provides diffraction limited solar imaging and polarimetry in the near-infrared (NIR). While the AO system is being upgraded to provide diffraction limited imaging at bluer wavelengths, the instrumentation and observations are concentrated in the NIR. The New Solar Telescope (NST) operates in campaigns, making it the ideal ground-based telescope to provide complementary/supplementary data to SDO and Hinode. The NST makes photometric observations in Hα (656.3 nm) and TiO (705.6 nm) among other lines. As well, the NST collects vector magnetograms in the 1565 nm lines and is beginning such observations in 1083.0 nm. Here we discuss the relevant NST instruments, including AO, and present some results that are germane to NASA solar missions.     

Algorithm Design and Test of the Solar Guide Telescope

The Solar Guide Telescope (SGT), an important solar attitude sensor of the SST (Space Solar Telescope, a space solar observing instrument being developed in China), can accurately produce pointing error signals of the SST for attitude control at high speed. We analyze in detail the error algorithm of the heliocentric coordinates and the edge judging of solar images. The measuring accuracy of ±0.5 arcsec of the SGT is verified by experiments on the tracking of the Sun and by testing a sun simulator. Some factors causing the pointing errors are examined.     

Estimation of Solar Observations with the Five-hundred-meter Aperture Spherical Radio Telescope(FAST)

We present the estimation of solar observation with the Five-hundred-meter Aperture Spherical radio Telescope(FAST). For both the quiet Sun and the Sun with radio bursts, when pointing directly to the Sun, the total power received by FAST would be out of the safe operational range of the signal chain, even resulting in damage to the receiver. As a conclusion, the Sun should be kept at least ～2° away from the main beam during observations at～1.25 GHz. The separation for lower frequency should be ...     

Solar System Observations with MIRI, The Mid InfraRed Instrument on the James Webb Space Telescope

MIRI is the Mid InfraRed Instrument for the James Webb Space Telescope (JWST) and will provide imaging, coronography and integral field spectroscopy in the range between 4.9 and 28.6  $\upmu \hbox{m}.$ We summarise solar system observations which may be possible with this instrument, drawing on examples of observations made with previous space missions such as IRAS, ISO and Spitzer.     

First Observations from the Multi-Application Solar Telescope (MAST) Narrow-Band Imager

The Multi-Application Solar Telescope is a 50 cm off-axis Gregorian telescope recently installed at the Udaipur Solar Observatory, India. In order to obtain near-simultaneous observations at photospheric and chromospheric heights, an imager optimized for two or more wavelengths is being integrated with the telescope. Two voltage-tuneable lithium-niobate Fabry–Perot etalons along with a set of interference blocking filters have been used for developing the imager. Both of the etalons are used in tandem for photospheric observations in Fe i 6173 Å and chromospheric observation in H\(\alpha\) 6563 Å spectral lines, whereas only one of the etalons is used for the chromospheric Ca II line at 8542 Å. The imager is also being used for spectropolarimetric observations. We discuss the characterization of the etalons at the above wavelengths, detail the integration of the imager with the telescope, and present a few sets of observations taken with the imager set-up.     

Imaging Spectropolarimeter for the Multi-Application Solar Telescope at Udaipur Solar Observatory: Characterization of Polarimeter and Preliminary Observations

The Multi-Application Solar Telescope (MAST) is a 50 cm off-axis Gregorian telescope that has recently become operational at the Udaipur Solar Observatory (USO). An imaging spectropolarimeter is being developed as one of the back-end instruments of MAST to gain a better understanding of the evolution and dynamics of solar magnetic and velocity fields. This system consists of a narrow-band filter and a polarimeter. The polarimeter includes a linear polarizer and two sets of liquid crystal variable retarders (LCVRs). The instrument is intended for simultaneous observations in the spectral lines 6173 Å and 8542 Å, which are formed in the photosphere and chromosphere, respectively. In this article, we present results from the characterization of the LCVRs for the spectral lines of interest and the response matrix of the polarimeter. We also present preliminary observations of an active region obtained using the spectropolarimeter. For verification purposes, we compare the Stokes observations of the active region obtained from the Helioseismic Magnetic Imager (HMI) onboard the Solar Dynamics Observatory (SDO) with that of MAST observations in the spectral line 6173 Å. We find good agreement between the two observations, considering the fact that MAST observations are limited by seeing.     

太阳和月球射电辐射对40m天线数据接收影响分析

利用标准射电源和标准噪声源,对宁静太阳和月球射电辐射的噪声温度进行了测量,估计它们对40m天线接收绕月卫星信号的影响,结论是:(1)40m天线指向偏离太阳超过2°时,能够满足正常数据接收要求;(2)40m天线指向月球时,系统接收的噪声温度增加值为87.1K, 此时系统的总噪声温度能够满足正常数据接收要求.     

Advanced Technology Solar Telescope

High-resolution studies of the Sun’s magnetic fields are needed for a better understanding of the fundamental processes responsible for solar variability. The generation of magnetic fields through dynamo processes, the amplification of fields through the interaction with plasma flows, and the destruction of fields are poorly understood. There is incomplete insight into physical mechanisms responsible for chromospheric and coronal structure and heating, causes of variations in the radiative output of the Sun, and mechanisms that trigger flares and coronal mass ejections. Progress in answering these critical questions requires study of the interaction of the magnetic field and convection with a resolution sufficient to observe scale fundamental to these processes. The planned 4 m aperture ATST will be a unique scientific tool, with excellent angular resolution, a large wavelength range, and low scattered light. With its integrated adaptive optics, the ATST will achieve a spatial resolution nearly 10 times better than any existing solar telescope. The ATST design and development phase began in 2001 and it is now ready to begin construction in 2009.     

EAST-Educational Adaptive-optics Solar Telescope

For the public having a better understanding of solar activities, the Educational Adaptive-optics Solar Telescope(EAST) was built in July 2021 and is located at the Shanghai Astronomy Museum. The EAST consists of a 65 cm aperture solar telescope with a 177-element adaptive optics system and two-channel high resolution imaging system at the Hα and TiO bands, in addition to three full disk solar telescopes at CaK, Hα and TiO bands equipped on the tube of the main telescope. In this paper, the conf...     

2130MHz太阳射电望远镜中频放大器的调试

本文介绍云南天文台２１３０ＭＨｚ太阳射电望远镜中频放大器的结构原理，技术指标及测试结果。     

云南天文台太阳望远镜光学系统的光学传递函数检验

摘要：给出了太阳光谱望远镜光学系统成像质量的测定方法．以及给出了我们用星光作为目标来测定望远镜光学系统传递函数时必须考虑的条件和理论基础。实测结果给出望远镜空间分辨率的上限为0．6“，95％光能集中度在1．2“以内。     

15厘米太阳射电望远镜增益运算放大器的制作与调试

本文介绍了１５厘米太阳射电望远镜增益运算放大器的结构原理，调试检测及测试结果。     

Near-Infrared Solar Electric Field Telescope

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Simulation Research on the Solar Hard X-Ray Imaging Telescope

The hard X-ray imaging telescope of the modulation collimator type is widely used in current solar observations. The spatial modulation telescope is the telescope which keeps its central axis not rotate, suitable for the satellite of 3-axis attitude stabilization. For the possible Chinese solar mission in the near future, we make a design of hard X-ray imaging telescope, and simulate the photon counting using the common simulation software GEANT4. Then we implement the image reconstruction with MATLAB, and compare the reconstructed image of the photons simulated by GEANT4 with that of the photons calculated by the geometric algorithm. The results show that the simulated one by GEANT4 is more closer to the reality than that obtained by the geometric algorithm. An executable design is also proposed at last.     

The 26 December 2001 Solar Event Responsible for GLE63. I. Observations of a Major Long-Duration Flare with the Siberian Solar Radio Telescope

Ground level enhancements (GLEs) of cosmic-ray intensity occur, on average, once a year. Because they are rare, studying the solar sources of GLEs is especially important to approach understanding their origin. The SOL2001-12-26 eruptive-flare event responsible for GLE63 seems to be challenging in some aspects. Deficient observations limited our understanding of it. Analysis of additional observations found for this event provided new results that shed light on the flare configuration and evolution. This article addresses the observations of this flare with the Siberian Solar Radio Telescope (SSRT). Taking advantage of its instrumental characteristics, we analyze the detailed SSRT observations of a major long-duration flare at 5.7 GHz without cleaning the images. The analysis confirms that the source of GLE63 was associated with an event in active region 9742 that comprised two flares. The first flare (04:30?–?05:03 UT) reached a GOES importance of about M1.6. Two microwave sources were observed, whose brightness temperatures at 5.7 GHz exceeded 10 MK. The main flare, up to an importance of M7.1, started at 05:04 UT and occurred in strong magnetic fields. The observed microwave sources reached a brightness temperature of about 250 MK. They were not static. After appearing on the weaker-field periphery of the active region, the microwave sources moved toward each other nearly along the magnetic neutral line, approaching the stronger-field core of the active region, and then moved away from the neutral line like expanding ribbons. These motions rule out an association of the non-thermal microwave sources with a single flaring loop.     

太阳光谱望远镜的Stokes光谱测量

中国科学院云南天文台"太阳Stokes光谱观测与理论研究”团组自进入国家天文观测中心以来,经过一年多的努力,对50cm太阳光谱望远镜原偏振测量部分进行了彻底改造,由原来的D.C.调制改为A.C.调制,且增加了偏振测量校正系统.其机械,电控设计和加工于2000年2月完成,3月完成了光学调试,4月上旬完成了偏振解调和图像处理的软件编制.自2000年4月下旬以来,对23周峰年出现的部分活动区进行了较为成功的斯托克斯光谱测量,其偏振测量精度可达2×10-3,已接近国际水平,为该团组开展的课题研究打下了良好的基础.以此望远镜与怀柔观测基地太阳磁场望远镜相配合,将使我国太阳矢量磁场和速度场的研究更上一个台阶.给出了偏振测量的具体方法和部分测量结果.尽管取得了以上的成绩,但在近期内将对该偏振测量方式作进一步改进,用双光束分析代替单光束分析,使偏振测量精度提高到5×10-4,从而使之不仅能在活动区而且也能在宁静区得到矢量磁场的信息,不仅如此,还可对太阳第二光谱进行测量,提高我们依托该望远镜进行研究的广度和深度.     

Temperature of Solar Prominences Obtained with the Fast Imaging Solar Spectrograph on the 1.6 m New Solar Telescope at the Big Bear Solar Observatory

We observed solar prominences with the Fast Imaging Solar Spectrograph (FISS) at the Big Bear Solar Observatory on 30 June 2010 and 15 August 2011. To determine the temperature of the prominence material, we applied a nonlinear least-squares fitting of the radiative transfer model. From the Doppler broadening of the Hα and Ca ii lines, we determined the temperature and nonthermal velocity separately. The ranges of temperature and nonthermal velocity were 4000?–?20?000 K and 4?–?11 km?s^?1. We also found that the temperature varied much from point to point within one prominence.     

1m望远镜夜间观测概况

本文主要介绍1m望远镜夜间观测情况，并对夜间观测时段(有效观测时间)进行统计、分析，并给出其结果。     

13.7米射电望远镜的太阳观测与研究

本文分析研究了22GHz频率上高分辨率(～4′)的太阳射电观测资料.发现源区域由两部分组成,即对应于黑子群中前导黑子的角径较小、温度较高的核,和对应于色球钙谱斑、环绕核的角径较大、温度较低的晕.此外,还分析了源区域的SVC的某些特征.