Solar adaptive optics systems for the New Vacuum Solar Telescope at the Fuxian Lake Solar Observatory

Adaptive optics(AO)is essential for high-quality ground-based observations with large telescopes because it counters the impact of wavefront aberrations caused by atmospheric turbulence.The new vacuum solar telescope(NVST)is one of the most important high-resolution solar observation instruments in the world.Three sets of solar adaptive optics systems have been developed and installed on this telescope:conventional adaptive optics,ground layer adaptive optics,and multi-conjugate adaptive optics.These have been in operation from 2018 to 2023.This paper details the development and application of solar adaptive optics on the NVST and discusses the newest instrumentation.

Comparison of Precipitation Observations from a Prototype Space-based Cloud Radar and Ground-based Radars

A prototype space-based cloud radar has been a precipitation system over Tianjin, China in July developed and was installed on an airplane to observe 2010. Ground-based S-band and Ka-band radars were used to examine the observational capability of the prototype. A cross-comparison algorithm between different wavelengths, spatial resolutions and platform radars is presented. The reflectivity biases, correlation coefficients and standard deviations between the radars are analyzed. The equivalent reflectivity bias between the S- and Ka-band radars were simulated with a given raindrop size distribution. The results indicated that reflectivity bias between the S- and Ka-band radars due to scattering properties was less than 5 dB, and for weak precipitation the bias was negligible. The prototype space-based cloud radar was able to measure a reasonable vertical profile of reflectivity, but the reflectivity below an altitude of 1.5 km above ground level was obscured by ground clutter. The measured refiectivity by the prototype space-based cloud radar was approximately 10.9 dB stronger than that by the S-band Doppler radar （SA radar）, and 13.7 dB stronger than that by the ground-based cloud radar. The reflectivity measured by the SA radar was 0.4 dB stronger than that by the ground-based cloud radar. This study could provide a method for the quantitative examination of the observation ability for space-based radars.

Review on strategies of space-based optical space situational awareness

Space-based optical(SBO)space surveillance has attracted widespread interest in the last two decades due to its considerable value in space situation awareness(SSA).SBO observation strategy,which is related to the performance of space surveillance,is the top-level design in SSA missions reviewed.The recognized real programs about SBO SAA proposed by the institutions in the U.S.,Canada,Europe,etc.,are summarized firstly,from which an insight of the development trend of SBO SAA can be obtained.According to the aim of the SBO SSA,the missions can be divided into general surveillance and space object tracking.Thus,there are two major categories for SBO SSA strategies.Existing general surveillance strategies for observing low earth orbit(LEO)objects and beyond-LEO objects are summarized and compared in terms of coverage rate,revisit time,visibility period,and image processing.Then,the SBO space object tracking strategies,which has experienced from tracking an object with a single satellite to tracking an object with multiple satellites cooperatively,are also summarized.Finally,this paper looks into the development trend in the future and points out several problems that challenges the SBO SSA.

Thickness evolution of graphite-based cathodes in the dual ion batteries via in operando optical observation

Graphite has been currently considered as a promising cathode material in dual ion batteries(DIBs)due to its unique features of sp2 hybridized carbon and stacked two-dimensional layered structures.However,unexpected volume/thickness changes in the graphite cathodes,induced by the intercalation/deintercalation of anions with large molecular size have been known to be a critical problem in designing DIB cells.To understand the volume/thickness changes in the DIB electrodes,in operando optical observing apparatus has been employed to observe the cross-section view of a graphite-based cathode upon cycles in the present work.The observation suggests that the cathode initially presented a huge irreversible thickness change(60%),and such thickness variation was prone to reduce and remain <20% in the following cycles.The results from both in operando observation and electrochemical characterizations collectively indicate that the greater thickness variation at initial cycle should be attributed to both anion intercalation into graphite-based cathodes and irreversible decomposition of chemical components in the DIB system.The method here highlights a universal route for fundamentally understanding the electrodes of huge volume variation.

Observing single cells in whole organs with optical imaging

Cells are the basic unit of human organs that are not fully understood.The revolutionary advancements of optical imaging alowed us to observe single cells in whole organs,revealing the complicated composition of cells with spatial information.Therefore,in this review,we revisit the principles of optical contrast related to those biomolecules and the optical techniques that transform optical contrast into detectable optical signals.Then,we describe optical imaging to achieve threedimensional spatial discrimination for biological tisutes.Due to the milky appearance of tissues,the spatial information burred deep in the whole organ.Fortunately,strategies developed in the last decade could circumvent this issue and lead us into a new era of investigation of the cells with their original spatial information.

An impact assessment of sea ice on ocean optics observations in the marginal ice zone of the Arctic

Diffuse attenuation coefficient （DAC） of sea water is an important parameter in ocean thermodynamics and biology, reflecting the absorption capability of sea water in different layers. In the Arctic Ocean, however, sea ice affects the radiance/irradiance measurements of upper ocean, which results in obvious errors in the DAC calculation. To better understand the impacts of sea ice on the ocean optics observations, a series ofin situ experiments were carried out in the summer of 2009 in the southern Beaufort Sea. Observational results show that the profiles of spectral diffuse attenuation coefficients of seawater near ice cover within upper surface of 50 m were not contaminated by the sea ice with a solar zenith angle of 55＆#176;, relative azimuth angle of 110＆#176;≤φ≤115＆#176; and horizontal distance between the sensors and ice edge of greater than 25 m. Based on geometric optics theory, the impact of ice cover could be avoided by adjusting the relative solar azimuth angle in a particular distance between the instrument and ice. Under an overcast sky, ice cover being 25 m away from sensors did not affect the profiles of spectral DACs within the upper 50 m either. Moreover, reli-able spectral DACs of seawater could be obtained with sensors completely covered by sea ice.

Solar Multi-Spectral Radiometric Observations of Atmospheric Optical Thickness over Passarlapudi Gas Well Blow-Out Site in India

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Comments on "Direct Radiative Forcing of Anthropogenic Aerosols over Oceans from Satellite Observation"

Previous observational studies have estimated anthropogenic aerosol direct radiative forcing over oceans without due consideration of cloudy-sky aerosols. However, when interaction between clouds and aerosols located below or above the cloud level is taken into account, the aerosol direct radiative forcing is larger by as much as 5 W m-2 in most mid-latitude regions in the Northern Hemisphere.

Magnetic Field Strengths and Structures from Radio Observations of Solar Active Regions

Radio observations of some active regions (ARs) obtained with the Nobeyama radioheliograph at λ=1.76 cm are used for estimating the magnetic field strength in the upper chromosphere, based on thermal bremsstrahlung. The results are compared with the magnetic field strength in the photosphere from observations with the Solar Magnetic Field Telescope (SMFT) at Huairou Solar Observing Station of Beijing Astronomical Observatory. The difference in the magnetic field strength between the two layers seems reasonable. The solar radio maps of active regions obtained with the Nobeyama radioheliograph, both in total intensity (I-map) and in circular polarizations (V-map), are compared with the optical magnetograms obtained with the SMFT. The comparison between the radio map in circular polarization and the longitudinal photospheric magnetogram of a plage region suggests that the radio map in circular polarization is a kind of magnetogram of the upper chromosphere. The comparison of the radio map in total intensity with the photo-spheric vector magnetogram of an AR shows that the radio map in total intensity gives indications of magnetic loops in the corona, thus we have a method of defining the coronal magnetic structure from the radio I-maps at λ=1.76 cm. Analysing the I-maps, we identified three components: (a) a compact bright source; (b) a narrow elongated structure connecting two main magnetic islands of opposite polarities (observed in both the optical and radio magnetograms); (c) a wide, diffuse, weak component that corresponds to a wide structure in the solar active region which shows in most cases an S or a reversed S contour, which is probably due to the differential rotation of the Sun. The last two components suggest coronal loops on different spatial scales above the neutral line of the longitudinal photospheric magnetic field.

基于有限时间观测器的光储系统母线电压互补滑模控制

针对光储直流微网混合储能系统易受能源间歇性输入、负载随机性扰动以及功率流向切换等干扰,会造成母线电压波动、系统功率失稳等问题,提出一种基于有限时间观测器的互补滑模控制(FTESO+CSMC)策略.首先,根据混合储能元件的高低频特性,对系统差额功率进行电流等效分配.然后,设计有限时间扩张状态观测器,对系统受到的总扰动进行观测,并将扰动观测值作为前馈项输入互补滑模控制器中,对系统扰动进行补偿,保证系统状态在有限时间内达到收敛,提高了系统的快速性和抗扰性,并根据Lyapunov理论证明了控制系统的稳定性.最后,基于MATLAB仿真平台,对多种模拟工况进行仿真,仿真结果表明,相较于传统控制策略,本文所提控制具有更快的响应速度以及更好的抗扰性能.

南极光学天文望远镜控制软件关键技术

南极天文望远镜控制软件是望远镜软件系统的重要组成部分,是控制计算机在望远镜用户层和设备层之间运行的关键技术。对于用户层,控制软件需具备全自动观测的交互接口、卫星通信条件下的远程访问和故障诊断等功能;对于设备层,控制软件不但要完成对天体目标的精确指向和精密跟踪、计算并补偿系统误差和控制关键部件以达到目标像质,而且需实现对电源分配系统、除霜及加热系统的控制、设备及环境信息的采集和监测等。相比于普通台址,在南极大陆运行的光学天文望远镜有其独特的特点,控制软件需进行特殊设计。本文重点从操作系统选择、远程建立望远镜指向误差修正模型方法、全自动观测软件接口、卫星通信及远程运维、望远镜实时状态监测和故障诊断等方面探讨了南极天文光学望远镜控制软件的关键技术和设计原则,并展望未来技术的发展,为南极天文望远镜的研制和控制系统研发提供技术储备。

基于CE-318观测的甘肃省气溶胶光学特性分析

对于大气气溶胶地基观测资料的定量分析是了解气溶胶光学特性和大气污染特征的基本途径,可为探讨污染治理方向提供一定的依据。近年来,利用地基观测资料分析甘肃省不同区域气溶胶光学特性的研究较少。为了解甘肃省不同下垫面的大气气溶胶光学特性,本文基于2018年4月至2020年9月CE-318型太阳光度计观测资料,通过ASTPwin软件反演获得了甘肃省四个站点的气溶胶光学厚度AOD,计算了Angstrom波长指数α,分析了甘肃省不同区域不同季节AOD和α的分布和变化特征以及气溶胶光学厚度和波长指数的关系。结果表明:(1)观测时段内,所有站点各波段AOD的变化趋于一致,且AOD值随波长增大而减小。兰州和皋兰山AOD值冬季最高,春、秋季次之,夏季最低,兰州冬、春季AOD值分别比年均值超出14.98%和4.68%,皋兰山冬季AOD值比年均值超出3.88%。敦煌和民勤AOD值均为春季最高,比各自的年均值高出24.49%和26.30%。敦煌AOD季节分布为:春季>夏季>冬季>秋季,而民勤则表现为从春到冬季逐渐减小的趋势。(2)兰州和皋兰山春夏季主控粒子为粗模态,秋冬季则为细颗粒物主导。敦煌和民勤大气气溶胶常年由粗模态粒子主控。2019年冬季,兰州市区AOD值比其城郊的皋兰山高出68.0%;敦煌和民勤2019年春季沙尘气溶胶污染较为严重,敦煌AOD值比民勤超出42.42%。(3)四个站点AOD和α的频率分布均呈单峰曲线,不同季节AOD高频次分布范围存在差异性,但都处于1.0以下。α的高频次范围分布较为复杂,兰州春季、皋兰山春夏季、敦煌四季、民勤春夏秋季,α分布区间均小于1.0,而兰州夏秋冬季、皋兰山秋冬季、民勤冬季α主要分布于1.1以上。(4)不同季节AOD和α的关系存在差异,表现为不同季节,大气出现严重或者局部污染时,气溶胶的主控粒子粒径大小不同。春季大气出现局部或者严重污染、夏季大气局部污染时,四个站点气溶胶主要是大粒径粒子,其中沙尘气溶胶的贡献较大。夏季大气处于严重污染时,皋兰山气溶胶主要是细模态粒子,兰州、敦煌、民勤气溶胶依然由粗模态主控,但是兰州小粒径粒子导致的污染比重高于其余两站,其中85%以上属于城市工业-气溶胶污染。秋季大气处于严重污染状况时,兰州和皋兰山均由细模态粒子主导,其中城市工业-气溶胶占比明显增加,而敦煌和民勤依然由粗模态粒子主导,其中沙尘气溶胶占比偏重。冬季大气严重污染时,兰州依然由细模态粒子主导,而其他三站由粗模态粒子占据主导地位,冬季大气局部污染时,敦煌和民勤粗模态粒子与细模态粒子同时出现,皋兰山以细模态粒子为主。分析可知,总体上甘肃偏北地区气溶胶污染以沙尘气溶胶为主,而偏南地区气溶胶污染表现为粗模态与细模态粒子交替出现,这为下一步结合卫星遥感资料研究甘肃不同区域的气溶胶特性及大气污染特征提供了一些参考。

基于NSGA-Ⅱ的车载光学测量设备任务调度方案优化

针对车载光学测量设备任务调度方案优化问题,提出了一种基于非支配排序的遗传算法(non-dominated sorting genetic algorithmⅡ,NSGA-Ⅱ)的多目标遗传算法。首先,建立了包含约束、优化指标在内的观测任务调度问题的数学模型。其中,针对多优化指标进行巧妙处理,将某些不作为最优指标的优化指标作为指标约束进行处理。其次,基于NSGA-Ⅱ中的快速非优超排序方法计算多目标适应度函数与选择算子,多目标优化求解得到的Pareto最优解集即为任务调度方案集。最后,通过仿真算例对所提算法进行了求解验证。仿真结果表明,该算法能够有效解决任务调度方案优化问题,为车载光学测量设备的工程实践提供了一定的参考。

地球静止轨道航天器绕飞持续观测任务轨迹规划与控制

针对地球静止轨道(geosynchronous orbit,GEO)航天器的高清观测任务,成像卫星在连续小推力作用下接近GEO航天器,对GEO航天器自然绕飞并以有利的光照条件对其持续观测。针对Clohessy-Wiltshire(CW)方程的偏差问题,通过修正非球形摄动和重力加速度二次长期项偏差对CW方程进行改进,补偿非线性偏差的长期项和主要的摄动项。在轨迹规划问题上,计算绕飞轨迹的初始相位角区间,以保证成像卫星在整个绕飞任务中都能够以良好的观测角观测GEO航天器。基于CW方程和改进的CW方程对成像卫星接近和绕飞GEO航天器全过程进行仿真,基于CW方程的仿真没有达到预期目标;基于改进的CW方程的仿真达到预期目标,全过程所需施加的总速度增量仅为4.67 m/s,工程上具有很强的可行性。

构建海底信息网技术分析

本文介绍了国内外各种海底网络的最新研究和应用情况。在现有典型网络的基本结构和技术特点基础上,提出适时构建海底信息网以实现海底光缆网、海底警戒网和海底观测网的“三网合一”,并针对最新相关软硬件技术进行了系统分析。

Portable adaptive optics for exoplanet imaging

The portable adaptive optics(PAO)device is a low-cost and compact system,designed for 4-meter class telescopes that have no adaptive optics(AO)system,because of the physical space limitation at the Nasmyth or Cassegrain focus and the historically high cost of conventional AO.The initial scientific observations of the PAO are focused on the direct imaging of exoplanets and sub-stellar companions.This paper discusses the concept of PAO and the associated high-contrast imaging performance in our recent observational runs.PAO deliver a Strehl ratio better than 60%in H band under median seeing conditions of 1".Combined with our dedicated image rotation and subtraction(IRS)technique and the optimized IRS(O-IRS)algorithm,the averaged contrast ratio for a 5≤V_(mag)≤9 primary star is 1.3×10^(-5)and3.3×10^(-6)at angular distance of 0.36"with exposure time of 7 minutes and 2 hours,respectively.PAO has successfully revealed the known exoplanet ofκAnd b in our recent observation with the 3.5-meter ARC telescope at Apache Point Observatory.We have performed the associated astrometry and photometry analysis of the recoveredκAnd b planet,which gives a projected separation of 0.98"±0.05",a position angle of 51.1°±0.5°and a mass of 10.15_(-1.255)^(+2.19) MJup.These results demonstrate that PAO can be used for direct imaging of exoplanets with medium-sized telescopes.

Measurements of atmospheric turbulence parameters at Vainu Bappu Observatory using short-exposure CCD images

We report atmospheric turbulence parameters, namely atmospheric seeing, tilt-anisoplanatic angle(θ_0) and coherence time(Τ_0), measured under various sky conditions, at Vainu Bappu Observatory in Kavalur. Bursts of short exposure images of selected stars were recorded with a high-speed, frame-transfer CCD mounted on the Cassegrain focus of a newly commissioned 1.3 m telescope. The estimated median seeing is ≈ 1.85 " at wavelength of ～ 600 nm, the image motion correlation between different pairs of stars is ～44% for θ0≈ 36" and mean Τ_0 is ≈ 2.4 ms. This work was motivated by the design considerations and expected performance of an adaptive optics system that is currently being planned for the telescope.

Autonomous optical navigation of Mars probe aided by one-way Doppler measurements in capture stage

The optical navigation errors of Mars probe in the capture stage depend closely on which targets are selected to be observed in the Mars system.As for this problem,an integrated navigation scheme is proposed wherein the optical observation is aided by one-way Doppler measurements.The errors are then analyzed respectively for the optical observation and one-way Doppler measurements.The real-time calculating scheme which exploits the extended Kalman filter(EKF)framework is designed for the integrated navigation.The simulation tests demonstrate that the errors of optical navigation,which select the Mars moon as the observation target,are relatively smaller than those in the Mars-orientation optical navigation case.On one hand,the integrated navigation errors do not depend on the selecting pattern of optical observation targets.On the other hand,the integrated navigation errors are significantly reduced as compared with those in the optical-alone autonomous navigation mode.

Infrared optical coatings in SITP

Infrared optical coatings in SITP (Shanghai Institute of Technical Physics) mainly cover the spectrum range from 0.7 μm to 15 μm, and visible and near-UV range are also been included. The coatings are mainly used for metal-reflectance mirrors, Anti-reflection(AR) lens and windows, filters, and dichroic beam splitters. Coatings passed some dependability tests. These optical coated devices usually consist in a remote observing instrument. Most coating materials are commercial products. And one kind of special material PbTe is made by ourselves. Some main results of our research department are reported.

Optical and atomic force microscopic study on step bunching in BaB_2O_4 crystal growth

The formation of macrostep during high-temperature phase of barium meta-borate （^-BaB204） single crystal growth has been investigated by both optical in-situ observation system and atomic force microscopy （AFM）. The in- si$u observation results demonstrate that the critical linear size of growing facet exceeding the size that the macrostep generates is significantly anisotropic. The critical linear sizes are around 280 ~m and 620 ~m for {1010} and （T010} planes, respectively. AFM study illustrates that macrostep train with a height of 150 nm^200 nm is one typical morphological feature of the as-grown crystal surface. The riser of each macrostep consists of several straight and parallel sub-steps, indicating the occurrence of step bunching. Additionally, triangular sub-steps with heights of several nanometers on the treads of the macrosteps are found to be another typical feature of surface morphology, which implies a microscopically competitive bunching of sub-steps between various crystallographic orientations.