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Crossmatching of high-proper motion L, T, and Y brown dwarfs with large photometric surveys 高真运动L、T和Y棕矮星与大型光度测量的交叉匹配
IF 0.7 4区 物理与天体物理 Q4 ASTRONOMY & ASTROPHYSICS Pub Date : 2023-01-01 DOI: 10.1515/astro-2022-0214
A. Avdeeva, Sergey V. Karpov, O. Malkov
Abstract L, T, and Y brown dwarf (BD) exploration is a topical issue. First, the transition boundary between planets and BDs is not fully understood yet. Second, there is a phenomenon called the L/T-transition. The observed properties of cooler BDs differ significantly from the less cool ones, namely, colors of BDs shift much bluer and, simultaneously, dwarfs become brighter with a decrease in temperature. Models of this phenomenon are now being actively developed, for which reason BDs observed in a wide range of spectra are needed. Our goal is to refine the position of BDs in the parameter space of colors and magnitudes in order to effectively search for them in photometric surveys (without involving spectroscopic observations). For that reason, we crossmatched about 500 known L, T, and Y BDs with large photometric surveys. We paid special attention to the problem of identifying objects near the Sun because the crossmatching by default is made by searching for the closest object in a particular survey, which can be inappropriate concerning the high proper motions of our dwarfs. We have determined the color indices that can be used to search for these objects in large photometric surveys, and we have pointed out the color indices that are inappropriate for this purpose. We also made preliminary estimates of the radius matching to search for objects in the modern photometric surveys, given their proximity to the Sun and, consequently, their high proper motion.
摘要L、T和Y棕矮星(BD)探测是一个热门问题。首先,行星和BD之间的过渡边界尚不完全清楚。其次,有一种现象叫做L/T跃迁。观察到的较冷BD的性质与较不冷BD的明显不同,即BD的颜色变蓝,同时,随着温度的降低,矮星变得更亮。目前正在积极开发这种现象的模型,因此需要在广泛的光谱中观察到BD。我们的目标是细化BD在颜色和星等参数空间中的位置,以便在光度测量中有效地搜索它们(不涉及光谱观测)。因此,我们用大型光度测量交叉匹配了大约500个已知的L、T和Y BD。我们特别注意识别太阳附近物体的问题,因为默认情况下,交叉匹配是通过在特定的调查中搜索最近的物体来进行的,这对于我们的矮星的高固有运动来说可能是不合适的。我们已经确定了可用于在大型光度测量中搜索这些物体的颜色指数,并指出了不适合此目的的颜色指数。我们还对现代光度测量中搜索物体的半径匹配进行了初步估计,考虑到它们离太阳很近,因此它们的固有运动也很高。
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引用次数: 0
Ka/C dual frequency ranging system for ocean altimetry satellite and analysis of ionospheric error 海洋测高卫星Ka/C双频测距系统及电离层误差分析
IF 0.7 4区 物理与天体物理 Q4 ASTRONOMY & ASTROPHYSICS Pub Date : 2023-01-01 DOI: 10.1515/astro-2022-0220
N. Li, Zhenhe Zhai, Jian Ma, Bin Guan, Wenhui Cui, Duan Li
Abstract In view of the future development trend of ocean altimetry satellites, the design idea of Ka/C dual frequency combination system is proposed, that is, the mode of using an altimeter antenna to contain Ka and C frequencies (35.7 and 5.3 GHz, respectively) for combined ranging. First, the random error model of altimeter measuring the distance from the altimeter phase center to the sea surface is given, and the analysis shows that the ionospheric correction error is one of the important factors. Second, the calculation of typical ionospheric parameters shows that the influence of ionospheric higher order terms on altimeter ranging is below the mm level, and its influence can be ignored. The rigorous expression for the first-order and second-order term correction of ionosphere error are given, respectively, by using dual frequency and three frequencies. The computational experiment of Jason-2 and SARAL satellite show that the maximum magnitude of ionospheric error correction in Ku band can reach 11 cm, while the maximum magnitude of ionospheric error correction in Ka band can reach 2 cm. For high-precision applications, ionospheric corrections must be made for single Ka frequency. After Ka/C dual frequency combination is adopted, error correction can be directly conducted without global ionospheric map (GIM) model, and its accuracy will be further improved than GIM model. Under 1 Hz sampling conditions, the ionospheric correction accuracy of Ka/C combination can be better than 2.5 mm, basically eliminating the influence of the ionosphere, and the total ranging accuracy can reach 3.5 cm considering the propagation error.
摘要针对未来海洋测高卫星的发展趋势,提出了Ka/C双频组合系统的设计思路,即采用一个测高天线包含Ka和C频率(分别为35.7 GHz和5.3 GHz)进行组合测距的模式。首先,给出了测高度计相位中心到海面距离的随机误差模型,分析表明电离层校正误差是影响随机误差的重要因素之一。其次,对典型电离层参数的计算表明,电离层高阶项对高度计量程的影响小于mm级,可以忽略。分别给出了电离层误差一阶项和二阶项双频和三频校正的严格表达式。Jason-2和SARAL卫星的计算实验表明,Ku波段电离层误差校正的最大幅度可达11 cm, Ka波段电离层误差校正的最大幅度可达2 cm。对于高精度应用,必须对单个Ka频率进行电离层校正。采用Ka/C双频组合后,无需全球电离层图(GIM)模型即可直接进行误差校正,其精度将比GIM模型进一步提高。在1 Hz采样条件下,Ka/C组合的电离层校正精度可优于2.5 mm,基本消除了电离层的影响,考虑传播误差,总测距精度可达3.5 cm。
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引用次数: 0
Clay minerals and other hydrous alteration products in the Kaba meteorite: Review of the literature and new XRD investigations 卡巴陨石中的粘土矿物和其他含水蚀变产物:文献综述和新的XRD研究
IF 0.7 4区 物理与天体物理 Q4 ASTRONOMY & ASTROPHYSICS Pub Date : 2023-01-01 DOI: 10.1515/astro-2022-0213
István Viczián, F. Kristály
Abstract The present study is a review of publications regarding special aspects of the mineralogy of the Kaba meteorite, clay minerals, hydrous phases, and organic matter. In Section 1, the history of fall and finding of the meteorite and the first classical mineralogical description in the Year 1961 are mentioned. The most frequent alteration product of primary silicates and the glassy matrix is Fe-bearing saponite. By modelling of hydrothermal alteration of Allende-type meteorites, artificial saponite could be produced. The thermodynamic study proved the possibility of hydrous neoformation of silicates and magnetite at low temperatures, mostly below 100°C. The formation of Fe-rich external rims in forsterite grains by hydrothermal action was demonstrated by electron probe microanalysis and scanning electron microscopy-cathodo-luminescence methods. Foliation in CV3 carbonaceous chondrites indicates that the Kaba meteorite is derived from the external, shallow zone of the parent body. A combination of X-ray power diffraction (XRD) and Mössbauer spectroscopy made the exact modal analysis of CV3 chondrites possible, including Kaba. The study of alteration by in situ determination of stable oxygen isotope contents may provide constraints regarding the oxygen isotopic composition of the aqueous fluid on the CV parent asteroid. The degree of thermal metamorphism of the organic matter was determined by using Raman spectroscopy. The presence of aromatic and aliphatic, saturated and unsaturated hydrocarbons, and various amino acids was demonstrated. The non-biogenic origin is more probable; however, there are textural and mineralogical observations that may indicate also the biogenic origin of organic matter. In addition to the review of the literature above, as an appendix, shortly new XRD investigations of the authors are reported that indicated smectite-like phases in a thin section made of the meteorite.
摘要本研究综述了关于卡巴陨石矿物学、粘土矿物、含水相和有机物的特殊方面的出版物。在第1节中,提到了陨石坠落和发现的历史以及1961年的第一次经典矿物学描述。原生硅酸盐和玻璃质基质最常见的蚀变产物是含铁皂石。通过模拟阿连德型陨石的热液蚀变,可以生产人造皂石。热力学研究证明了硅酸盐和磁铁矿在低温下(大多低于100°C)含水新生的可能性。用电子探针显微分析和扫描电子显微镜阴极发光方法证明了镁橄榄石晶粒在水热作用下形成富铁外缘。CV3碳质球粒陨石中的叶片表明卡巴陨石来源于母体的外部浅区。X射线功率衍射(XRD)和穆斯堡尔谱的结合使包括卡巴在内的CV3球粒陨石的精确模态分析成为可能。通过原位测定稳定氧同位素含量来研究蚀变可能会对CV母小行星上的水性流体的氧同位素组成提供限制。利用拉曼光谱测定了有机物的热变质程度。证明了芳香烃和脂肪族、饱和烃和不饱和烃以及各种氨基酸的存在。非生物成因的可能性更大;然而,一些结构和矿物学观察结果也可能表明有机物的生物成因。除了对上述文献的回顾外,作为附录,作者的新XRD研究报告显示,陨石薄片中存在类似蒙脱石的相。
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引用次数: 0
An outlier detection method with CNN for BeiDou MEO moderate-energy electron data 基于CNN的北斗MEO中能电子数据离群值检测方法
IF 0.7 4区 物理与天体物理 Q4 ASTRONOMY & ASTROPHYSICS Pub Date : 2023-01-01 DOI: 10.1515/astro-2022-0196
Tian Chao, Cui Ruifei, Zhang Riwei, Xu Peikang, Chen Libo, Shang Jie, Quan Lin, Wan Yujun, Hu Sihui, Yue Fulu, Su Xing
Abstract BeiDou Medium Earth Orbit moderate-energy electron detection data play an important role in space environment effect analysis including satellite anomaly diagnosis, satellite risk estimation, etc. However, the data contain outliers which cause obstacle for the subsequent usage significantly. To solve this problem, we propose an outlier detection method based on convolutional neural networks (CNNs) which can learn a rule from labeled historical data and detect outliers from the detection data. With this method, we can identify outliers and do some follow-up operations to improve the data quality. In comparison with general methods, this CNN method provides a more reliable and rapid way to build dataset for the follow-up work.
摘要北斗中地球轨道中能电子探测数据在卫星异常诊断、卫星风险估计等空间环境效应分析中发挥着重要作用。然而,数据中含有异常值,这对后续的使用造成了很大的障碍。为了解决这一问题,我们提出了一种基于卷积神经网络(cnn)的异常点检测方法,该方法可以从标记的历史数据中学习规则,并从检测数据中检测异常点。通过这种方法,我们可以识别异常点,并进行一些后续操作,以提高数据质量。与一般方法相比,该CNN方法为后续工作提供了更可靠、更快速的数据集构建方式。
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引用次数: 0
An ion beam system for calibration of space low-energy ion detectors 一种用于空间低能离子探测器标定的离子束系统
IF 0.7 4区 物理与天体物理 Q4 ASTRONOMY & ASTROPHYSICS Pub Date : 2023-01-01 DOI: 10.1515/astro-2022-0225
Shi Guifen, Lian Yiren, Miao Bin, Liu Kai, Hao Xinjun, Pan Zonghao, G. Meng
Abstract Low-energy ion detection in space is one of the most important interests of space exploration. An accurate calibration of this type of instrument is necessary to ensure the effectiveness and scientificness of the obtained data. And the ion source is the most critical equipment in a calibration facility. In this study, an ion beam system based on Kaufman ion source is designed, which can meet the ground calibration of space low-energy ion detection instrument in the low-energy range of 100–1,000 eV. The experimental research shows that when the beam intensity of the ion source is about 100 mA, the Faraday Cup collects about 1 mA of current, and the generated ion beam fluctuates less than 5% within 60 min, which can meet the ground calibration requirements of space low-energy ion detection instruments.
摘要空间低能离子探测是空间探测的重要研究方向之一。为了确保所获得数据的有效性和科学性,有必要对这类仪器进行准确的校准。离子源是校准设施中最关键的设备。本研究设计了一种基于考夫曼离子源的离子束系统,该系统可以满足空间低能离子探测仪器在100–1000低能范围内的地面校准 实验研究表明,当离子源的束流强度约为100 mA,法拉第杯收集大约1 电流mA,产生的离子束在60内波动小于5% min,可以满足空间低能离子探测仪器的地面校准要求。
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引用次数: 0
Deep learning applications for stellar parameter determination: II-application to the observed spectra of AFGK stars 深度学习在恒星参数确定中的应用:ii -在AFGK恒星观测光谱中的应用
IF 0.7 4区 物理与天体物理 Q4 ASTRONOMY & ASTROPHYSICS Pub Date : 2022-10-31 DOI: 10.1515/astro-2022-0209
M. Gebran, F. Paletou, I. Bentley, Rose Brienza, Kathleen Connick
Abstract In this follow-up article, we investigate the use of convolutional neural network for deriving stellar parameters from observed spectra. Using hyperparameters determined previously, we have constructed a Neural Network architecture suitable for the derivation of T eff {T}_{{rm{eff}}} , log g log g , [ M / H ] left[Mhspace{0.1em}text{/}hspace{0.1em}H] , and v e sin i {v}_{e}sin i . The network was constrained by applying it to databases of AFGK synthetic spectra at different resolutions. Then, parameters of A stars from Polarbase, SOPHIE, and ELODIE databases are derived, as well as those of FGK stars from the spectroscopic survey of stars in the solar neighbourhood. The network model’s average accuracy on the stellar parameters is found to be as low as 80 K for T eff {T}_{{rm{eff}}} , 0.06 dex for log g log g , 0.08 dex for [ M / H ] left[Mhspace{0.1em}text{/}hspace{0.1em}H] , and 3 km/s for v e sin i {v}_{e}sin i for AFGK stars.
摘要在这篇后续文章中,我们研究了使用卷积神经网络从观测光谱中推导恒星参数。使用之前确定的超参数,我们构建了一个适用于推导T eff的神经网络架构{T}_{rm{eff}},log glog g,[M/H]left[Mhspace{0.1em}text{/}space{0.1em}H]和v e sin i{v}_{e} 我。通过将网络应用于不同分辨率的AFGK合成光谱数据库,对网络进行了约束。然后,从Polarbase、SOPHIE和ELODIE数据库中导出了A星的参数,以及从太阳系恒星光谱调查中导出的FGK星的参数。对于T eff,网络模型对恒星参数的平均精度低至80K{T}_{rm{eff}},log glog g为0.06 dex,[M/H]left[Mhspace{0.1em}text{/}hspace为0.08 dex{0.1em}H],对于v e sin i为3 km/s{v}_{e} sin i代表AFGK明星。
{"title":"Deep learning applications for stellar parameter determination: II-application to the observed spectra of AFGK stars","authors":"M. Gebran, F. Paletou, I. Bentley, Rose Brienza, Kathleen Connick","doi":"10.1515/astro-2022-0209","DOIUrl":"https://doi.org/10.1515/astro-2022-0209","url":null,"abstract":"Abstract In this follow-up article, we investigate the use of convolutional neural network for deriving stellar parameters from observed spectra. Using hyperparameters determined previously, we have constructed a Neural Network architecture suitable for the derivation of T eff {T}_{{rm{eff}}} , log g log g , [ M / H ] left[Mhspace{0.1em}text{/}hspace{0.1em}H] , and v e sin i {v}_{e}sin i . The network was constrained by applying it to databases of AFGK synthetic spectra at different resolutions. Then, parameters of A stars from Polarbase, SOPHIE, and ELODIE databases are derived, as well as those of FGK stars from the spectroscopic survey of stars in the solar neighbourhood. The network model’s average accuracy on the stellar parameters is found to be as low as 80 K for T eff {T}_{{rm{eff}}} , 0.06 dex for log g log g , 0.08 dex for [ M / H ] left[Mhspace{0.1em}text{/}hspace{0.1em}H] , and 3 km/s for v e sin i {v}_{e}sin i for AFGK stars.","PeriodicalId":19514,"journal":{"name":"Open Astronomy","volume":"32 1","pages":""},"PeriodicalIF":0.7,"publicationDate":"2022-10-31","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"48159783","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 1
The specifics of pulsar radio emission 脉冲星射电发射的细节
IF 0.7 4区 物理与天体物理 Q4 ASTRONOMY & ASTROPHYSICS Pub Date : 2022-05-23 DOI: 10.1515/astro-2022-0025
Boris Ya. Losovsky
A characteristic property of pulsars is pulsed periodic radio emission, which has a high stability of periods. Despite the high stability of the emission periods of pulsars, monitoring the time of arrival of pulses (timing) shows the presence of different types of irregularities: variations of residual deviations, changes in the shape of the pulse, switching on and off of radio emission, and rotation discontinuities. Numerous observations of the radio emission of pulsars indicate that they are caused mainly by processes occurring in the pulsar’s magnetosphere. The special interest causes the observations of a pulsar in the Crab Nebula, performed, in particular, at Jodrell Bank and Pushchino Radio Astronomy Observatory of Lebedev Physical Institute. The connection between the scattering of radio pulses and the measure of the pulsar dispersion, which was established earlier in Pushchino together with Jodrell Bank, has been confirmed. The observed variations in the scattering of radio pulses and their partial correlation with the dispersion measure are explained by the eclipse of the pulsar by plasma clouds with electron density fluctuations significantly exceeding the corresponding fluctuations in the interstellar medium. The question of a possible connection between glitches, dispersion measure variations, radio pulses scattering, and gamma-ray flares is discussed.
脉冲星的一个特征是脉冲周期性射电发射,它具有很高的周期稳定性。尽管脉冲星的发射周期具有很高的稳定性,但监测脉冲到达的时间(定时)显示了不同类型的不规则性的存在:残余偏差的变化,脉冲形状的变化,无线电发射的开关和旋转不连续。对脉冲星射电辐射的大量观测表明,它们主要是由脉冲星磁层中发生的过程引起的。这种特殊的兴趣引起了对蟹状星云中一颗脉冲星的观测,特别是在列别捷夫物理研究所的Jodrell Bank和Pushchino射电天文台进行的。早先在普什奇诺与乔德雷尔班克一起建立的无线电脉冲散射与脉冲星色散测量之间的联系已经得到证实。观测到的射电脉冲散射的变化及其与色散测量的部分相关性可以用等离子体云对脉冲星的日食来解释,等离子体云的电子密度波动明显超过星际介质中相应的波动。讨论了小故障、色散测量变化、射电脉冲散射和伽马射线耀斑之间可能存在的联系。
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引用次数: 0
Influence of the magnetic field on the formation of protostellar disks 磁场对原恒星盘形成的影响
IF 0.7 4区 物理与天体物理 Q4 ASTRONOMY & ASTROPHYSICS Pub Date : 2022-04-25 DOI: 10.1515/astro-2022-0022
Natalya S. Kargaltseva, Sergey A. Khaibrakhmanov, Alexander E. Dudorov, Sergey N. Zamozdra, Andrey G. Zhilkin
We numerically model the collapse of magnetic rotating protostellar clouds with mass of 10 M {M}_{odot } . The simulations are carried out with the help of 2D MHD code Enlil. The structure of the cloud at the isothermal stage of the collapse is investigated for the cases of weak, moderate, and strong initial magnetic field. Simulations reveal the universal hierarchical structure of collapsing protostellar clouds, consisting of the flattened envelope with the qausi-magnetostatc disk inside and the first core in its center. The size of the primary disk increases with the initial magnetic energy of the cloud. The magnetic braking efficiently transports the angular momentum from the primary disk into the envelope in the case, when the initial magnetic energy of the cloud is more than 20% of its gravitational energy. The intensity of the outflows launched from the region near the boundary of the first core increases with initial magnetic energy. The “dead” zone with small ionization fraction, x < 1 0 11 xlt 1{0}^{-11} , forms inside the first hydrostatic core and at the base of the outflow. Ohmic dissipation and ambipolar diffusion determine conditions for further formation of the protostellar disk in this region.
我们对质量为10 M⊙{M}_{odot}的磁性旋转原恒星云的坍缩进行了数值模拟。在二维MHD代码Enlil的帮助下进行了仿真。在弱、中、强初始磁场条件下,研究了坍缩等温阶段云的结构。模拟揭示了崩塌的原恒星云的普遍层次结构,包括扁平的包膜,内部是准静磁盘,中心是第一个核心。主磁盘的大小随着云的初始磁能的增加而增加。在这种情况下,当云的初始磁能超过其重力能的20%时,磁制动有效地将角动量从主盘传输到包膜中。从第一个磁芯边界附近区域发射的流出物强度随着初始磁能的增加而增加。电离率小的“死”区,x <1 0−11 xlt 1{0}^{-11},在第一个流体静力核心内部和流出的底部形成。欧姆耗散和双极扩散决定了该区域原恒星盘进一步形成的条件。
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引用次数: 0
Dynamics of magnetic flux tubes in accretion disks of Herbig Ae/Be stars 赫比格Ae/Be星吸积盘中磁通管的动力学
IF 0.7 4区 物理与天体物理 Q4 ASTRONOMY & ASTROPHYSICS Pub Date : 2022-03-28 DOI: 10.1515/astro-2022-0017
Sergey A. Khaibrakhmanov, Alexander E. Dudorov
The dynamics of magnetic flux tubes (MFTs) in the accretion disk of typical Herbig Ae/Be star (HAeBeS) with fossil large-scale magnetic field is modeled taking into account the buoyant and drag forces, radiative heat exchange with the surrounding gas, and the magnetic field of the disk. The structure of the disk is simulated using our magnetohydrodynamic model, taking into account the heating of the surface layers of the disk with the stellar radiation. The simulations show that MFTs periodically rise from the innermost region of the disk with speeds up to 10–12 km s 1 {{rm{s}}}^{-1} . MFTs experience decaying magnetic oscillations under the action of the external magnetic field near the disk’s surface. The oscillation period increases with distance from the star and initial plasma beta of the MFT, ranging from several hours at r = 0.012 au r=0.012hspace{0.33em}{rm{au}} up to several months at r = 1 au r=1hspace{0.33em}{rm{au}} . The oscillations are characterized by pulsations of the MFT’s characteristics including its temperature. We argue that the oscillations can produce observed IR-variability of HAeBeSs, which would be more intense than in the case of T Tauri stars, since the disks of HAeBeSs are hotter, denser, and have stronger magnetic field.
考虑吸积盘中的浮力和阻力、与周围气体的辐射热交换以及吸积盘中的磁场,建立了典型赫比格Ae/Be星(HAeBeS)吸积盘中磁通管(MFTs)的动力学模型。利用我们的磁流体动力学模型模拟了圆盘的结构,并考虑了恒星辐射对圆盘表层的加热。模拟结果表明,mft周期性地从圆盘最内层区域上升,速度可达10-12 km s−1 {{rm{s}}}^{-1}。在磁碟表面附近的外磁场作用下,MFTs经历衰减的磁振荡。振荡周期随着与恒星的距离和MFT初始等离子体β的增加而增加,从r=0.012 au时的几个小时r=0.012hspace{0.33em}{rm{au}}到r=1 au时的几个月r=1hspace{0.33em}{rm{au}}。振荡的特征是MFT的特征(包括其温度)的脉动。我们认为,振荡可以产生观测到的HAeBeSs红外变化率,这种变化率将比金牛座T星的情况更强烈,因为HAeBeSs的圆盘更热,密度更大,磁场更强。
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引用次数: 0
ANALOG-1 ISS – The first part of an analogue mission to guide ESA’s robotic moon exploration efforts ANALOG-1国际空间站——模拟任务的第一部分,指导欧空局的机器人月球探测工作
IF 0.7 4区 物理与天体物理 Q4 ASTRONOMY & ASTROPHYSICS Pub Date : 2022-01-01 DOI: 10.1515/astro-2022-0002
K. Wormnes, W. Carey, T. Krueger, Leonardo Cencetti, E. D. Exter, Stephen Ennis, Edmundo Ferreira, Antonio Fortunato, L. Gerdes, Lukas Hann, C. Lombardi, E. Luzzi, Sebastian Martin, M. Massironi, S. Payler, Aaron Pereira, A. Rossi, R. Pozzobon, F. Sauro, P. Schoonejans, Frank van der Hulst, J. Grenouilleau
Abstract The European Space Agency’s ANALOG-1 experiment is the culmination of 12 distinct METERON experiments carried out since 2011. These all address aspects of teleoperating a robotic asset from an orbital platform, i.e., technical implementation, user interfaces, autonomy and operations. The ANALOG-1 technology demonstration and operations concept experiment is based upon the surface mission scenario segment of the notional EL3 sample return mission. This segment focuses on the control of a lunar surface robotic asset from the Earth and from the Lunar Gateway. The experiment is taking place in two parts, with the first successfully completed from the ISS in November 2019. It assessed the effectiveness of a state-of-the-art robotic control interface to control a complex mobile robot from orbit, as well as evaluating the scientific interactions, during robotic-assisted geology exploration, between crew in orbit and scientists on the ground. Luca Parmitano operated the robot while he was on the ISS. For this experiment, a complex control station had been installed on the ISS. The experiment demonstrated the advantage of having an immersive control station and high level of robotic dexterity, with Luca finishing all his assigned and secondary geology targets ahead of time.
摘要欧洲航天局的模拟-1实验是自2011年以来进行的12次不同的METERON实验的高潮。这些都涉及从轨道平台远程操作机器人资产的各个方面,即技术实现、用户界面、自主性和操作。模拟-1技术演示和操作概念实验基于EL3样品返回任务的水面任务场景部分。本节重点介绍来自地球和月球门户的月球表面机器人资产的控制。该实验分为两部分,第一部分于2019年11月在国际空间站成功完成。它评估了最先进的机器人控制接口在轨道上控制复杂移动机器人的有效性,并评估了在机器人辅助地质勘探期间,轨道上的机组人员和地面科学家之间的科学互动。卢卡·帕米塔诺在国际空间站上操作机器人。在这个实验中,国际空间站上安装了一个复杂的控制站。该实验展示了具有沉浸式控制站和高水平机器人灵活性的优势,卢卡提前完成了所有指定的和次要的地质目标。
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引用次数: 9
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