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Electromagnetic Electron-Cyclotron Wave for Ring Distribution with Alternating Current (AC) Electric Field in Saturn Magnetosphere 土星磁层交流电场环形分布的电磁电子回旋波
IF 0.5 Q3 Earth and Planetary Sciences Pub Date : 2022-06-01 DOI: 10.5140/jass.2022.39.2.35
Annex Edappattu Haridas, S. Kanwar, R. S. Pandey
During their respective missions, the spacecraft Voyager and Cassini measured several Saturn magnetosphere parameters at different radial distances. As a result of information gathered throughout the journey, Voyager 1 discovered hot and cold electron distribution components, number density, and energy in the 6–18 Rs range. Observations made by Voyager of intensity fluctuations in the 20–30 keV range show electrons are situated in the resonance spectrum’s high energy tail. Plasma waves in the magnetosphere can be used to locate Saturn’s inner magnetosphere’s plasma clusters, which are controlled by Saturn’s spin. Electromagnetic electron cyclotron (EMEC) wave ring distribution function has been investigated. Kinetic and linear approaches have been used to study electromagnetic cyclotron (EMEC) wave propagation. EMEC waves’ stability can be assessed by analyzing the dispersion relation’s effect on the ring distribution function. The primary goal of this study is to determine the impact of the magnetosphere parameters which is observed by Cassini. The magnetosphere of Saturn has also been observed. When the plasma parameters are increased as the distribution index, the growth/damping rate increases until the magnetic field model affects the magnetic field at equator, as can be seen in the graphs. We discuss the outputs of our model in the context of measurements made in situ by the Cassini spacecraft.
在各自的任务中,旅行者号和卡西尼号在不同的径向距离上测量了几个土星磁层参数。由于在整个旅程中收集的信息,旅行者1号发现了6-18 Rs范围内的冷热电子分布成分、数量密度和能量。旅行者号对20-30 keV范围内的强度波动的观测表明,电子位于共振光谱的高能尾部。磁层中的等离子体波可以用来定位土星内部磁层的等离子体星团,这些星团是由土星的自旋控制的。研究了电磁电子回旋加速器(EMEC)的波环分布函数。动力学和线性方法已被用于研究电磁回旋加速器(EMEC)的波传播。通过分析频散关系对环分布函数的影响,可以评价EMEC波的稳定性。这项研究的主要目标是确定卡西尼号观测到的磁层参数的影响。土星的磁层也被观测到了。当等离子体参数随分布指数增加时,增长/阻尼率增加,直到磁场模型影响赤道处的磁场,如图所示。我们在卡西尼号宇宙飞船现场测量的背景下讨论我们模型的输出。
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引用次数: 0
A Study of Double Dark Photons Produced by Lepton Colliders using High Performance Computing 轻子对撞机产生双暗光子的高性能计算研究
IF 0.5 Q3 Earth and Planetary Sciences Pub Date : 2022-03-01 DOI: 10.5140/jass.2022.39.1.1
Kihong Park, Kyungho Kim, Kihyeon Cho
The universe is thought to be filled with not only Standard Model (SM) matters but also dark matters. Dark matter is thought to play a major role in its construction. However, the identity of dark matter is as yet unknown, with various search methods from astrophysical observartion to particle collider experiments. Because of the cross-section that is a thousand times smaller than SM particles, dark matter research requires a large amount of data processing. Therefore, optimization and parallelization in High Performance Computing is required. Dark matter in hypothetical hidden sector is though to be connected to dark photons which carries forces similar to photons in electromagnetism. In the recent analysis, it was studied using the decays of a dark photon at collider experiments. Based on this, we studies double dark photon decays at lepton colliders. The signal channels are e+e– → AʹAʹ and e+e– → AʹAʹγ where dark photon Aʹ decays dimuon. These signal channels are based on the theory that dark photons only decay into heavily charged leptons, which can explain the muon magnetic momentum anomaly. We scanned the cross-section according to the dark photon mass in experiments. MadGraph5 was used to generate events based on a simplified model. Additionally, to get the maximum expected number of events for the double dark photon channel, the detector efficiency for several center of mass (CM) energy were studied using Delphes and MadAnalysis5 for performance comparison. The results of this study will contribute to the search for double dark photon channels at lepton colliders.
人们认为,宇宙中不仅充满了标准模型(SM)物质,也充满了暗物质。暗物质被认为在其构造中起着重要作用。然而,通过从天体物理观测到粒子对撞机实验的各种搜索方法,暗物质的身份仍然未知。由于暗物质的横截面比SM粒子小一千倍,因此暗物质研究需要大量的数据处理。因此,需要高性能计算中的优化和并行化。假设的隐藏扇区中的暗物质被认为与暗光子有关,暗光子携带的力与电磁中的光子相似。在最近的分析中,使用对撞机实验中的暗光子衰变来研究它。在此基础上,我们研究了双暗光子在轻子对撞机上的衰变。信号通道为e+e -→A′A′和e+e -→A′A′γ,暗光子A′衰变为介子。这些信号通道基于暗光子只衰变成重电荷轻子的理论,这可以解释μ子磁动量异常。我们根据实验中暗光子的质量对截面进行了扫描。使用MadGraph5生成基于简化模型的事件。此外,为了获得双暗光子通道的最大期望事件数,利用Delphes和MadAnalysis5对几种质心能量的探测器效率进行了性能比较研究。本研究结果将有助于在轻子对撞机上寻找双暗光子通道。
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引用次数: 0
Empirical Modeling of the Global Distribution of Magnetosonic Waves with Ambient Plasma Environment using Van Allen Probes 用范艾伦探针模拟等离子体环境下磁声波的全球分布
IF 0.5 Q3 Earth and Planetary Sciences Pub Date : 2022-03-01 DOI: 10.5140/jass.2022.39.1.11
Kyung‐Chan Kim
It is suggested that magnetosonic waves (also known as equatorial noise) can scatter radiation belt electrons in the Earth’s magnetosphere. Therefore, it is important to understand the global distribution of these waves between the proton cyclotron frequency and the lower hybrid resonance frequency. In this study, we developed an empirical model for estimating the global distribution of magnetosonic wave amplitudes and wave normal angles. The model is based on the entire mission period (approximately 2012–2019) of observations of Van Allen Probes A and B as a function of the distance from the Earth (denoted by L*), magnetic local time (MLT), magnetic latitude (λ), and geomagnetic activity (denoted by the Kp index). In previous studies the wave distribution inside and outside the plasmasphere were separately investigated and modeled. Our model, on the other hand, identifies the wave distribution along with the ambient plasma environment—defined by the ratio of the plasma frequency (fpe) to the electron cyclotron frequency (fce)—without separately determining the wave distribution according to the plasmapause location. The model results show that, as Kp increases, the dayside wave amplitude in the equatorial region intensifies. It thereby propagates the intense region towards the wider MLT and inward to L* < 4. In contrast, the fpe/fce ratio decreases with increasing Kp for all regions. Nevertheless, the decreasing aspect differs between regions above and below L* = 4. This finding implies that the particle energy and pitch angle that magnetosonic waves can effectively scatter vary depending on the locations and geomagnetic activity. Our model agrees with the statistically observed wave distribution and ambient plasma environment with a coefficient of determination of > 0.9. The model is valid in all MLTs, 2 ≤ L* < 6, |λ| < 20°, and Kp ≤ 6.
有人认为,磁声波(也称为赤道噪声)可以散射地球磁层中的辐射带电子。因此,了解这些波在质子回旋频率和较低混合共振频率之间的整体分布是很重要的。在本研究中,我们建立了一个估算磁声波振幅和波法向角全球分布的经验模型。该模型基于范艾伦探测器A和B的整个任务期间(大约2012-2019年)的观测结果,作为与地球的距离(用L*表示)、磁当地时间(MLT)、磁纬度(λ)和地磁活动(用Kp指数表示)的函数。在以往的研究中,对等离子体层内外的波分布分别进行了研究和模拟。另一方面,我们的模型根据等离子体频率(fpe)与电子回旋频率(fce)的比值来确定波的分布,而不是根据等离子体顶位置单独确定波的分布。模式结果表明,随着Kp的增大,赤道地区日侧波振幅增大。因此,它将强区向更宽的MLT传播,并向内传播到L* < 4。相反,fpe/fce比值随Kp的增加而降低。然而,L* = 4以上和以下区域的下降幅度有所不同。这一发现表明,磁声波能有效散射的粒子能量和俯仰角随位置和地磁活动的不同而变化。我们的模型与统计观测到的波分布和周围等离子体环境一致,决定系数> 0.9。该模型适用于2≤L* < 6, |λ| < 20°,Kp≤6的所有mlt。
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引用次数: 0
Investigation of the Jets of the Blazar 3C 279 with Korean VLBI Network (KVN) 22–129 GHz Observations 利用韩国VLBI网络(KVN) 22-129 GHz观测对Blazar 3C 279喷流的研究
IF 0.5 Q3 Earth and Planetary Sciences Pub Date : 2021-12-01 DOI: 10.5140/jass.2021.38.4.193
Sungmin Yoo, Sang-Sung Lee, Sang-Hyun Kim, H. An
We present analysis results of Korean VLBI Network (KVN) four-band data for the highly variable blazar 3C 279. We measured the 22, 43, 86, and 129 GHz flux densities and spectral indices of the source using contemporaneous data taken over 5.6 years. We used the discrete correlation function to investigate correlations between the radio emission properties and those measured in the optical (2 × 1014 – 1.5 × 1015 Hz), X-ray (0.3–10 keV), and gamma-ray (0.1–300 GeV) bands. We found a significant correlation between the radio spectral index and gamma-ray flux without a time delay and interpreted the correlation using an extended jet scenario for blazar emission.
本文介绍了韩国VLBI网络(KVN)对高变量blazar 3C 279四波段数据的分析结果。我们使用5.6年的同期数据测量了22、43、86和129 GHz的通量密度和光谱指数。我们使用离散相关函数研究了射电发射特性与光学(2 × 1014 - 1.5 × 1015 Hz)、x射线(0.3-10 keV)和伽马射线(0.1-300 GeV)波段测量的发射特性之间的相关性。我们发现射电光谱指数和伽马射线通量之间存在显著的相关性,没有时间延迟,并使用扩展的喷流情景解释了这种相关性。
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引用次数: 0
Observations of the Aurora by Visible All-Sky Camera at Jang Bogo Station, Antarctica 南极张伯戈站可见光全天空照相机对极光的观测
IF 0.5 Q3 Earth and Planetary Sciences Pub Date : 2021-12-01 DOI: 10.5140/jass.2021.38.4.203
G. Jee, Young-bae Ham, Y. Choi, Eunsol Kim, Changsup Lee, H. Kwon, T. Trondsen, Ji Eun Kim, Jeong‐Han Kim
The auroral observation has been started at Jang Bogo Station (JBS), Antarctica by using a visible All-sky camera (v-ASC) in 2018 to routinely monitor the aurora in association with the simultaneous observations of the ionosphere, thermosphere and magnetosphere at the station. In this article, the auroral observations are introduced with the analysis procedure to recognize the aurora from the v-ASC image data and to compute the auroral occurrences and the initial results on their spatial and temporal distributions are presented. The auroral occurrences are mostly confined to the northern horizon in the evening sector and extend to the zenith from the northwest to cover almost the entire sky disk over JBS at around 08 MLT (magnetic local time; 03 LT) and then retract to the northeast in the morning sector. At near the magnetic local noon, the occurrences are horizontally distributed in the northern sky disk, which shows the auroral occurrences in the cusp region. The results of the auroral occurrences indicate that JBS is located most of the time in the polar cap near the poleward boundary of the auroral oval in the nightside and approaches closer to the oval in the morning sector. At around 08 MLT (03 LT), JBS is located within the auroral oval and then moves away from it, finally being located in the cusp region at the magnetic local noon, which indicates that the location of JBS turns out to be ideal to investigate the variabilities of the poleward boundary of the auroral oval from long-term observations of the auroral occurrences. The future plan for the ground auroral observations near JBS is presented.
2018年,在南极张伯皋站(JBS)开始了极光观测,利用可见光全天照相机(v-ASC)对极光进行常规监测,同时对电离层、热层和磁层进行观测。本文介绍了极光观测资料,介绍了从v-ASC图像数据中识别极光并计算极光发生次数的分析过程,并给出了极光发生次数的时空分布的初步结果。极光的出现主要局限于北半球地平线的傍晚部分,并从西北方向延伸到天顶,覆盖了JBS上空的几乎整个天盘,大约在08mlt(磁地方时;03lt),然后在上午扇区向东北撤回。在接近磁极局地中午时,极光在北部天盘呈水平分布,显示出极光发生在尖峰区。极光发生的结果表明,JBS大部分时间位于极帽中靠近极光卵圆的极向边界的夜晚,并在早晨接近卵圆。在08 MLT (03 LT)前后,JBS位于极光椭圆内,然后远离极光椭圆,最终位于磁局地午时的尖端区域,这表明JBS的位置是研究极光椭圆极向边界变化的理想位置。提出了今后在JBS附近进行地面极光观测的计划。
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引用次数: 4
Characteristics of Horizontal Winds in the Mesosphere and Lower Thermosphere Region over Korean Peninsula Observed from the Korea Astronomy and Space Science Institute Meteor Radar 韩国天文空间研究所流星雷达观测的朝鲜半岛上空中层和下层热层水平风的特征
IF 0.5 Q3 Earth and Planetary Sciences Pub Date : 2021-12-01 DOI: 10.5140/jass.2021.38.4.229
H. Kam, Y. Kwak, Tae-Yong Yang, Y. Kim, Jeongheon Kim, Jaewook Lee, Seonghwan Choi, J. Baek
We present for the first time the characteristics of upper atmospheric horizontal winds over the Korean Peninsula. Winds and their variability are derived using four-year measurements by the Korea Astronomy and Space Science Institute (KASI) meteor radar. A general characteristic of zonal and meridional winds is that they exhibit distinct diurnal and seasonal variations. Their changes indicate sometimes similar or sometimes different periodicities. Both winds are characterized by either semi-diurnal tides (12 hour period) and/or diurnal tides (24 hour period) from 80–100 km. In terms of annual change, the annual variation is the strongest component in both winds, but semi-annual and ter-annual variations are only detected in zonal winds.
本文首次提出了朝鲜半岛上空大气高层水平风的特征。风和它们的变化是由韩国天文和空间科学研究所(KASI)流星雷达四年测量得出的。纬向风和经向风的一般特征是它们表现出明显的日变化和季节变化。它们的变化显示出有时相似或有时不同的周期性。这两种风的特点是在80-100公里范围内出现半日潮(12小时周期)和/或日潮(24小时周期)。在年际变化方面,两种风的年际变化都是最强的,而只有纬向风的半年和多年变化才存在。
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引用次数: 2
Development of a New Pressure-Sinkage Model for Rover Wheel-Lunar Soil Interaction based on Dimensional Analysis and Bevameter Tests 基于量纲分析和测试的月球车车轮-月壤相互作用压力沉降模型的建立
IF 0.5 Q3 Earth and Planetary Sciences Pub Date : 2021-12-01 DOI: 10.5140/jass.2021.38.4.237
Yujin Lim, V. Le, Pierre Anthyme Bahati
A rover is a planetary surface exploration device designed to move across the ground on a planet or a planetary-like body. Exploration rovers are increasingly becoming a vital part of the search for scientific evidence and discoveries on a planetary satellite of the Sun, such as the Moon or Mars. Reliable behavior and predictable locomotion of a rover is important. Understanding soil behavior and its interaction with rover wheels—the terramechanics—is of great importance in rover exploration performance. Up to now, many researchers have adopted Bekker’s semiempirical model to predict rover wheelsoil interaction, which is based on the assumption that soil is deformable when a pressure is applied to it. Despite this basic assumption of the model, the pressure-sinkage relation is not fully understood, and it continues to present challenges for rover designers. This article presents a new pressure-sinkage model based on dimensional analysis (DA) and results of bevameter tests. DA was applied to the test results in order to propose a new pressure-sinkage model by reducing physical quantitative parameters. As part of the work, a new bevameter was designed and built so that it could be successfully used to obtain a proper pressure-sinkage relation of Korean Lunar Soil Simulant (KLS-1). The new pressure-sinkage model was constructed by using three different sizes of flat plate diameters of the bevameter. The newly proposed model was compared successfully with other models for validation purposes.
漫游者是一种行星表面探测装置,设计用于在行星或类行星物体的地面上移动。探测车正日益成为在月球或火星等太阳的行星卫星上寻找科学证据和发现的重要组成部分。探测器可靠的行为和可预测的运动是很重要的。了解土壤特性及其与探测车车轮的相互作用,即地形力学,对探测车的探测性能具有重要意义。到目前为止,许多研究者采用Bekker的半经验模型来预测探测车轮-土相互作用,该模型是基于假设土壤在施加压力时是可变形的。尽管有这个模型的基本假设,但压力-下沉关系仍未被完全理解,这继续给火星车的设计者带来挑战。本文提出了一种基于量纲分析(DA)和井径试验结果的新型压力沉降模型。将数据分析应用于试验结果,通过减少物理定量参数,提出新的压力沉降模型。作为工作的一部分,我们设计并制造了一个新的测量仪,以便能够成功地使用它来获得合适的韩国月球土壤模拟物(KLS-1)的压力沉降关系。采用三种不同尺寸的平板直径,建立了新的压力沉降模型。为了验证目的,将新提出的模型与其他模型成功地进行了比较。
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引用次数: 0
Design of Regional Coverage Low Earth Orbit (LEO) Constellation with Optimal Inclination 具有最佳倾角的区域覆盖低地球轨道星座设计
IF 0.5 Q3 Earth and Planetary Sciences Pub Date : 2021-12-01 DOI: 10.5140/jass.2021.38.4.217
Jin-Hui Shin, Sang-Young Park, Jihae Son, S. Song
In this study, we describe an analytical process for designing a low Earth orbit constellation for discontinuous regional coverage, to be used for a surveillance and reconnaissance space mission. The objective of this study was to configure a satellite constellation that targeted multiple areas near the Korean Peninsula. The constellation design forms part of a discontinuous regional coverage problem with a minimum revisit time. We first introduced an optimal inclination search algorithm to calculate the orbital inclination that maximizes the geometrical coverage of single or multiple ground targets. The common ground track (CGT) constellation pattern with a repeating period of one nodal day was then used to construct the rest of the orbital elements of the constellation. Combining these results, we present an analytical design process that users can directly apply to their own situation. For Seoul, for example, 39.0° was determined as the optimal orbital inclination, and the maximum and average revisit times were 58.1 min and 27.9 min for a 20-satellite constellation, and 42.5 min and 19.7 min for a 30-satellite CGT constellation, respectively. This study also compares the revisit times of the proposed method with those of a traditional Walker-Delta constellation under three inclination conditions: optimal inclination, restricted inclination by launch trajectories from the Korean Peninsula, and inclination for the sun-synchronous orbit. A comparison showed that the CGT constellation had the shortest revisit times with a non-optimal inclination condition. The results of this analysis can serve as a reference for determining the appropriate constellation pattern for a given inclination condition.
在这项研究中,我们描述了设计一个用于监视和侦察空间任务的非连续区域覆盖的近地轨道星座的分析过程。这项研究的目的是配置一个针对朝鲜半岛附近多个地区的卫星星座。星座设计形成了一个具有最小重访时间的不连续区域覆盖问题的一部分。首先介绍了一种最优轨道倾角搜索算法,用于计算使单个或多个地面目标几何覆盖最大化的轨道倾角。然后使用重复周期为一个交点日的共地轨道(CGT)星座模式来构建星座的其余轨道要素。结合这些结果,我们提出了一个分析设计过程,用户可以直接应用到他们自己的情况。以首尔为例,39.0°被确定为最佳轨道倾角,20颗卫星星座的最大和平均重访时间分别为58.1分钟和27.9分钟,30颗卫星CGT星座的最大和平均重访时间分别为42.5分钟和19.7分钟。在最佳倾角、朝鲜半岛发射轨迹限制倾角和太阳同步轨道倾角三种倾角条件下,将该方法与传统的Walker-Delta星座的重访次数进行了比较。比较表明,在非最优倾角条件下,CGT星座的重访时间最短。分析结果可为给定倾角条件下确定合适的星座模式提供参考。
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引用次数: 1
Practical Algorithms on Lunar Reference Frame Transformations for Korea Pathfinder Lunar Orbiter Flight Operation 韩国探路者月球轨道飞行器运行中月球参照系变换的实用算法
IF 0.5 Q3 Earth and Planetary Sciences Pub Date : 2021-09-01 DOI: 10.5140/jass.2021.38.3.185
Young-Joo Song, Donghun Lee, Young-Rok Kim, Jonghee Bae, Jae-ik Park, Seung-Su Hong, Dae-Kwan Kim, Sang-Ryool Lee
This technical paper deals the practical transformation algorithms between several lunar reference frames which will be used for Korea pathfinder lunar orbiter (KPLO) flight operation. Despite of various lunar reference frame definitions already exist, use of a common transformation algorithm while establishing lunar reference frame is very important for all members related to KPLO mission. This is because use of slight different parameters during frame transformation may result significant misleading while reprocessing data based on KPLO flight dynamics. Therefore, details of practical transformation algorithms for the KPLO mission specific lunar reference frames is presented with step by step implementation procedures. Examples of transformation results are also presented to support KPLO flight dynamics data user community which is expected to give practical guidelines while post processing the data as their needs. With this technical paper, common understandings of reference frames that will be used throughout not only the KPLO flight operation but also science data reprocessing can be established. It is expected to eliminate, or at least minimize, unnecessary confusion among all of the KPLO mission members including: Korea Aerospace Research Institute (KARI), National Aeronautics and Space Administration (NASA) as well as other organizations participating in KPLO payload development and operation, or further lunar science community world-wide who are interested in KPLO science data post processing.
本文讨论了用于韩国探路者月球轨道飞行器(KPLO)飞行操作的几种月球参考系之间的实际转换算法。尽管月球参照系的定义多种多样,但在建立月球参照系的过程中,使用一种通用的变换算法对与KPLO任务相关的所有成员来说都是非常重要的。这是因为在帧变换过程中使用微小的不同参数可能会导致在基于KPLO飞行动力学的数据再处理时产生显著的误导。因此,详细介绍了KPLO任务特定月球参照系的实用变换算法,并给出了逐步实现的步骤。还提供了转换结果的示例,以支持KPLO飞行动力学数据用户社区,期望在根据他们的需要对数据进行后期处理时提供实用的指导方针。通过这篇技术论文,可以建立对参考框架的共同理解,这些框架不仅将在KPLO飞行操作中使用,而且还将在科学数据再处理中使用。预计将消除或至少减少所有KPLO任务成员之间不必要的混乱,包括:韩国航空研究所(KARI),美国航空航天局(NASA)以及其他参与KPLO有效载荷开发和运营的组织,或对KPLO科学数据后处理感兴趣的全球月球科学界。
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引用次数: 1
Evaluation of a Laser Altimeter using the Pseudo-Random Noise Modulation Technique for Apophis Mission 用伪随机噪声调制技术对阿波菲斯任务激光高度计的评价
IF 0.5 Q3 Earth and Planetary Sciences Pub Date : 2021-09-01 DOI: 10.5140/jass.2021.38.3.165
H. Lim, Ki-Pyoung Sung, Mansoo Choi, J. Park, C. Choi, S. Bang, Young‐Jun Choi, H. Moon
Apophis is a near-Earth object with a diameter of approximately 340 m, which will come closer to the Earth than a geostationary orbit in 2029, offering a unique opportunity for characterizing the object during the upcoming encounter. Therefore, Korea Astronomy and Space Science Institute has a plan to propose a space mission to explore the Apophis asteroid using scientific instruments such as a laser altimeter. In this study, we evaluate the performance metrics of a laser altimeter using a pseudorandom noise modulation technique for the Apophis mission, in terms of detection probability and ranging accuracy. The closed-form expression of detection probability is provided using the cross correlation between the received pulse trains and pseudo-random binary sequence. And the new ranging accuracy model using Gaussian error propagation is also derived by considering the sampling rate. The operation range is significantly limited by thermal noise rather than background noise, owing to not only the low power laser but also the avalanche photodiode in the analog mode operation. However, it is demonstrated from the numerical simulation that the laser altimeter can achieve the ranging performance required for a proximity operation mode, which employs commercially available components onboard CubeSat-scale satellites for optical communications.
阿波菲斯是一个直径约340米的近地天体,它将在2029年比地球静止轨道更接近地球,这为即将到来的相遇提供了一个独特的机会。因此,韩国天文研究院计划,利用激光测高仪等科学仪器,对阿波菲斯小行星进行探测。在本研究中,我们在探测概率和测距精度方面评估了阿波菲斯任务中使用伪随机噪声调制技术的激光高度计的性能指标。利用接收到的脉冲序列与伪随机二值序列之间的相互关系,给出了检测概率的封闭表达式。在考虑采样率的基础上,推导了基于高斯误差传播的测距精度模型。由于低功率激光器和雪崩光电二极管在模拟模式下工作,其工作范围受到热噪声而不是背景噪声的明显限制。然而,数值模拟表明,激光高度计可以实现近距离操作模式所需的测距性能,该模式采用商用立方体卫星上的光学通信组件。
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引用次数: 1
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