Cosmic Research最新文献

英文中文

Prediction of Ionospheric TEC during the Annular and Total Solar Eclipses that Occurred over Indonesia by Using OKSM and FFNN 利用OKSM和FFNN预测印度尼西亚日全食和日环食期间电离层TEC

IF 0.6 4区物理与天体物理 Q4 ASTRONOMY & ASTROPHYSICS

Cosmic Research

Pub Date : 2023-11-24 DOI: 10.1134/s001095252360004x

S. Kiruthiga, S. Mythili, R. Mukesh, Sarat C. Dass

Abstract

People across the world have been fascinated by solar eclipses for thousands of years. Solar eclipses are not only fascinating to observe but also provide opportunities for scientific research. During a solar eclipse, the quantity of solar energy reaching the Earth’s surface is reduced as the Moon passes in front of the Sun. This reduction in solar energy can have an effect on the Total Electron Content of the Earth’s ionosphere. In this paper, prediction and analysis of TEC variations in the Ionosphere during the solar eclipses happened on 26.12.2019 between 04:51 to 7:34 hours (UTC) and 09.03.2016 between 12:18 to 1:02 hours (UTC) over the Indonesia region were done by using two models: Ordinary Kriging based Surrogate Model (OKSM) and Feed-Forward Neural Network (FFNN). During the eclipse period, the TEC values were predicted by the OKSM and FFNN models and it is validated using literature. For this study, the GPS data belonging to the BAKO station situated in Indonesia were collected from IONOLAB servers and the input parameters were collected from the OMNIWEB servers. Forty days prior TEC data and input parameters were used to predict the TEC values. The credibility of the predicted results is assessed using statistical factors such as RMSE, CC, MAE, MAPE, sMAPE and R-Square. The statistical results show OKSM has performed well when compared to the FFNN model over the annular and total solar eclipse period. The study suggests that combining multiple modelling methods, such as OKSM and FFNN can improve our understanding of ionospheric variability during solar eclipses and provide more accurate predictions of TEC variations. This has important implications for satellite communications and navigation systems that rely on accurate TEC measurements for positioning and timing.

摘要几千年来，世界各地的人们都对日食着迷。日食不仅令人着迷，而且为科学研究提供了机会。在日食期间，到达地球表面的太阳能数量随着月球在太阳前面经过而减少。太阳能的减少会对地球电离层的总电子含量产生影响。本文采用基于普通克里格代理模型(OKSM)和前馈神经网络(FFNN)两种模型，对印度尼西亚地区2019年12月26日04:51 ~ 7:34 (UTC)和2016年3月9日12:18 ~ 1:02 (UTC)日食期间电离层TEC的变化进行了预测和分析。利用OKSM和FFNN模型预测了日食期间的TEC值，并进行了文献验证。在本研究中，来自印度尼西亚BAKO站的GPS数据来自IONOLAB服务器，输入参数来自OMNIWEB服务器。使用40天前的TEC数据和输入参数来预测TEC值。使用RMSE、CC、MAE、MAPE、sMAPE和R-Square等统计因子评估预测结果的可信度。统计结果表明，与FFNN模型相比，OKSM模型在日环食和日全食期间表现良好。该研究表明，结合OKSM和FFNN等多种模拟方法可以提高我们对日食期间电离层变化的认识，并提供更准确的TEC变化预测。这对依靠精确的TEC测量进行定位和授时的卫星通信和导航系统具有重要影响。

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引用次数: 0

Entropy Functionals and Information Difference of Satellite-Monitoring Time Series 卫星监测时间序列的熵函数与信息差

IF 0.6 4区物理与天体物理 Q4 ASTRONOMY & ASTROPHYSICS

Cosmic Research

Pub Date : 2023-11-24 DOI: 10.1134/s0010952523700429

Yu. A. Antonov, V. I. Zakharov, N. A. Sukhareva

Abstract

The results of information analysis of the time series of satellite monitoring of the state of the interplanetary magnetic field provided by the database of the Goddard Space Flight Center. In the arsenal of analysis methods, the main attention is paid to the control of nonextensive properties when scaling time samples created on the basis of the 2001–2022 time series. The reconstruction of the modality of the probability-distribution function for the components of the interplanetary magnetic field in the considered ensemble of realizations is demonstrated. The results of the reconstruction of the kinetics of the Shannon–Boltzmann–Gibbs, Tsallis, and Rényi entropy measures are presented. In a nonextensive approximation, the influence of q-deformation of the phase space on the stochastic regimes of the system under study. In this work, for the first time, the kinetics of information discrepancy and the kinetics of entropy measures of the ensemble of realizations of the values of the interplanetary magnetic field are studied together. The need for approval is indicated by the q-deformation parameters of the phase space, the reference and controlled subsystems, including when using asymptotic approximations in forecasting methods using neural-network algorithms and deep-learning algorithms.

摘要对美国戈达德航天飞行中心数据库提供的行星际磁场状态卫星监测时间序列信息进行了分析。在分析方法库中，主要关注的是在缩放基于2001-2022时间序列创建的时间样本时对非扩展特性的控制。给出了在考虑的实现系综中行星际磁场分量的概率分布函数的模态重建。给出了Shannon-Boltzmann-Gibbs、Tsallis和rsamnyi熵测度的动力学重建结果。在非扩展近似下，研究了相空间的q-变形对系统随机状态的影响。本文首次研究了行星际磁场值实现系综的信息差异动力学和熵测度动力学。需要通过相空间、参考和控制子系统的q-变形参数来表示，包括在使用神经网络算法和深度学习算法的预测方法中使用渐近逼近时。

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引用次数: 0

Optimization of Solar-Sail Control When a Vehicle Moves along Cyclic Heliocentric Trajectories 优化飞行器沿循环日心轨迹移动时的太阳帆控制

IF 0.6 4区物理与天体物理 Q4 ASTRONOMY & ASTROPHYSICS

Cosmic Research

Pub Date : 2023-11-24 DOI: 10.1134/S0010952523700430

M. A. Rozhkov, O. Starinova

引用次数: 0

The Significance of Input Features for Domain Adaptation of Spacecraft Data 输入特征对航天器数据域自适应的意义

IF 0.6 4区物理与天体物理 Q4 ASTRONOMY & ASTROPHYSICS

Cosmic Research

Pub Date : 2023-11-24 DOI: 10.1134/s0010952523700466

E. Z. Karimov, I. N. Myagkova, V. R. Shirokiy, O. G. Barinov, S. A. Dolenko

Abstract

The problem of improving the neural network forecast of geomagnetic index Dst under conditions in which the input data for such a forecast are measured by two spacecraft, one of which is close to the end of its life cycle, and the data history of the other is not yet enough to construct a neural network forecast of the required quality. For an efficient transition from the data of one spacecraft to the data of another, it is necessary to use methods of domain adaptation. This paper tests and compares several data translation methods. Also, for each translated attribute, an optimal set of parameters for its translation were found, which further reduces the difference between domains. The paper shows that the use of domain adaptation methods with the selection of significant features can improve the forecast compared to the results of using untranslated data.

摘要针对地磁指数Dst的神经网络预报输入数据是由两艘航天器测量的，其中一艘航天器已接近寿命周期，而另一艘航天器的数据历史还不足以构建所需质量的神经网络预报的情况下，如何改进该神经网络预报的问题。为了实现从一个航天器数据到另一个航天器数据的有效转换，需要使用域自适应方法。本文对几种数据翻译方法进行了测试和比较。此外，对于每个翻译的属性，找到了一组最优的翻译参数，这进一步减少了域之间的差异。研究表明，与使用未翻译数据的预测结果相比，使用选择显著特征的领域自适应方法可以提高预测结果。

引用次数: 0

A Prototype of a Background Solar Wind Forecasting Service Based on MHD Modeling and WSA Boundary Conditions 基于MHD模型和WSA边界条件的背景太阳风预报服务原型

IF 0.6 4区物理与天体物理 Q4 ASTRONOMY & ASTROPHYSICS

Cosmic Research

Pub Date : 2023-11-24 DOI: 10.1134/s0010952523700508

S. Arutyunyan, A. Kodukov, M. Subbotin, D. Pavlov

Abstract

A prototype service for MHD modeling of the calm solar wind and forecasting the speed and density of solar wind particles in interplanetary space, similar to the NOAA and ESA services, has been created. The service consists of an MHD simulator, a module for processing simulation results, and a web interface. The simulator is based on the implementation of the TVDLF method in the PLUTO package. The boundary conditions of the model (density, radial velocity, magnetic field, temperature) at a distance of 0.1 AU from the origin are obtained regularly from the corresponding NOAA service, in which they are calculated according to the WSA model based on the magnetograms of the GONG network. Two modes of boundary conditions are available: constant and daily. The simulations were carried out on a uniform grid in the range of 0.1–1.7 AU by distance (512 elements), –60°...+60° by latitude (60 elements), 0°–360° by longitude (180 elements). The calculated particle velocity and density maps are compared with the NOAA SWPC and NASA CCMC calculations under the same boundary conditions. A retrospective comparison of the resulting forecasts with data from direct measurements (OMNI) was carried out.

建立了类似于NOAA和ESA服务的MHD模拟平静太阳风和预测行星际空间太阳风粒子速度和密度的原型服务。该服务由一个MHD模拟器、一个处理模拟结果的模块和一个web界面组成。模拟器基于PLUTO包中的TVDLF方法的实现。模型在离原点0.1 AU处的边界条件(密度、径向速度、磁场、温度)是由NOAA相应服务定期获得的，其中这些边界条件是根据基于GONG网磁图的WSA模型计算得到的。边界条件有两种模式:不变模式和日模式。模拟在距离为0.1-1.7 AU(512个单元)，-60°…纬度+60°(60个元素)，经度0°-360°(180个元素)。在相同边界条件下，将计算得到的粒子速度和密度图与NOAA SWPC和NASA CCMC计算结果进行了比较。对结果预报与直接测量(OMNI)数据进行了回顾性比较。

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引用次数: 0

A Catalog of Geoefficient Flare Events of the Current 25th Solar Cycle in a Modern Presentation 第25个太阳周期地球有效耀斑事件的现代记录

IF 0.6 4区物理与天体物理 Q4 ASTRONOMY & ASTROPHYSICS

Cosmic Research

Pub Date : 2023-11-24 DOI: 10.1134/s001095252370048x

L. P. Zabarinskaya, V. N. Ishkov, N. A. Sergeeva

Abstract

To study the phenomena occurring on the Sun and in interplanetary space and their influence on near-Earth space and on processes in the outer and inner shells of the Earth, the results of continuous long-term observations of solar activity become very valuable. A representative collection of such long-term homogeneous series of systematic observations obtained by the worldwide network of solar and astronomical observatories, as well as by spacecraft, has been collected at the World Data Center for Solar–Terrestrial Physics in Moscow. The article describes a cumulative interactive catalog of the main characteristics of significant solar-flare events of the current 25th cycle of solar activity.

摘要为了研究太阳和行星际空间发生的现象及其对近地空间和地球内外壳层过程的影响，对太阳活动的长期连续观测结果变得非常有价值。莫斯科的世界日地物理数据中心收集了由世界范围的太阳和天文观测站网络以及宇宙飞船获得的这种长期均匀系列系统观测资料的代表性资料。本文描述了目前太阳活动第25个周期的重要太阳耀斑事件的主要特征的累积交互目录。

引用次数: 0

Evolution of Rotational Motion of the Planet Earth under the Influence of Internal Dissipative Forces 内耗散力作用下行星地球旋转运动的演化

IF 0.6 4区物理与天体物理 Q4 ASTRONOMY & ASTROPHYSICS

Cosmic Research

Pub Date : 2023-11-24 DOI: 10.1134/s001095252370051x

N. I. Amelkin

Abstract

The influence of internal dissipation on the rotational motion of the Earth in the gravitational field of the Sun and Moon is studied within the model of M.A. Lavrentiev. The averaged equations of second approximation describing the evolution of the Earth’s rotation axis and the magnitude of its angular velocity are obtained. The dependence of the rate of evolution on the values of the model parameters is studied. Phase trajectories of the evolutionary process are constructed for different parameter values. It is shown that the observed drift of the Earth’s magnetic poles can be explained within the framework of a mechanical model by the angular acceleration of the Earth.

摘要在M.A. Lavrentiev模型中研究了内耗散对地球在日月引力场中旋转运动的影响。得到了描述地球自转轴演化及其角速度大小的二阶近似平均方程。研究了演化速率与模型参数值的关系。在不同的参数值下，构造了演化过程的相轨迹。结果表明，观测到的地球磁极漂移可以用地球的角加速度在力学模型的框架内解释。

引用次数: 0

Determination of the Effective Collision Frequency of Electrons in the E and D Regions of the High-Latitude Ionosphere from Analysis of Radio Occultation Measurements 从掩星测量分析确定高纬度电离层E区和D区电子有效碰撞频率

IF 0.6 4区物理与天体物理 Q4 ASTRONOMY & ASTROPHYSICS

Cosmic Research

Pub Date : 2023-11-24 DOI: 10.1134/s0010952523700491

V. N. Gubenko, V. E. Andreev, I. A. Kirillovich, T. V. Gubenko, A. A. Pavelyev, D. V. Gubenko

Abstract

Collisions between electrons and neutral molecules are of special interest for the physics of the Earth’s ionosphere, in particular, for determining the ionospheric conductivity and current systems in the lower ionosphere of the planet, as well as elucidating the role they play in attenuating radio waves propagating inside the D and E regions of the ionosphere. The effective collision frequency of electrons can be estimated from laboratory studies of electron mobility in atmospheric gases in combination with rocket measurements of temperature and particle density in the Earth’s upper atmosphere, or it can be determined independently from analysis of radio occultation data. We have developed a method for reconstructing the vertical profiles of the absorption coefficient of decimeter (wavelength ~19 cm) radio waves by solving the inverse problem of signal absorption in the D and E regions of the Earth’s ionosphere. Based on the analysis of radio occultation data from the FORMOSAT-3/COSMIC satellites, the altitude profiles of the absorption coefficient of decimeter (DM) radio waves in the planet’s ionosphere during the geomagnetic storm on June 22–23, 2015, were determined. It is known that the absorption coefficient at a given fixed frequency is directly proportional to both the electron density and the collision frequency of electrons with ions and neutrals. Using the data on the vertical profiles of the absorption coefficient of DM radio waves and the electron density reconstructed from the analysis of FORMOSAT-3/COSMIC radio occultations, we estimated the effective collision frequency of electrons in the D and E regions of the Earth’s high-latitude ionosphere. The practical significance of studying the frequency of electron collisions and the effects of radio wave absorption in the D and E regions of the planet’s ionosphere is associated with maintaining the uninterrupted operation of space radio communication and navigation systems.

摘要电子和中性分子之间的碰撞对于地球电离层的物理学具有特殊的意义，特别是对于确定电离层电导率和地球电离层下部的电流系统，以及阐明它们在电离层D和E区域内传播的无线电波衰减中所起的作用。电子的有效碰撞频率可以通过对大气气体中电子迁移率的实验室研究，结合对地球高层大气中温度和粒子密度的火箭测量来估计，或者可以通过对无线电掩星数据的分析独立确定。通过求解地球电离层D区和E区信号吸收逆问题，提出了一种重建分米(波长~19 cm)无线电波吸收系数垂直剖面的方法。基于对FORMOSAT-3/COSMIC卫星掩星数据的分析，确定了2015年6月22日至23日地磁暴期间地球电离层分米(DM)无线电波吸收系数的高度剖面图。已知在给定固定频率下的吸收系数与电子密度和电子与离子和中性离子的碰撞频率成正比。利用DM无线电波吸收系数垂直剖面数据和FORMOSAT-3/COSMIC掩星分析重建的电子密度数据，估算了地球高纬度电离层D区和E区电子的有效碰撞频率。研究行星电离层D区和E区电子碰撞频率和无线电波吸收效应的现实意义与保持空间无线电通信和导航系统的不间断运行有关。

{"title":"Determination of the Effective Collision Frequency of Electrons in the E and D Regions of the High-Latitude Ionosphere from Analysis of Radio Occultation Measurements","authors":"V. N. Gubenko, V. E. Andreev, I. A. Kirillovich, T. V. Gubenko, A. A. Pavelyev, D. V. Gubenko","doi":"10.1134/s0010952523700491","DOIUrl":"https://doi.org/10.1134/s0010952523700491","url":null,"abstract":"<h3 data-test=\"abstract-sub-heading\">Abstract</h3><p>Collisions between electrons and neutral molecules are of special interest for the physics of the Earth’s ionosphere, in particular, for determining the ionospheric conductivity and current systems in the lower ionosphere of the planet, as well as elucidating the role they play in attenuating radio waves propagating inside the <i>D</i> and <i>E</i> regions of the ionosphere. The effective collision frequency of electrons can be estimated from laboratory studies of electron mobility in atmospheric gases in combination with rocket measurements of temperature and particle density in the Earth’s upper atmosphere, or it can be determined independently from analysis of radio occultation data. We have developed a method for reconstructing the vertical profiles of the absorption coefficient of decimeter (wavelength ~19 cm) radio waves by solving the inverse problem of signal absorption in the <i>D</i> and <i>E</i> regions of the Earth’s ionosphere. Based on the analysis of radio occultation data from the <i>FORMOSAT-3</i>/<i>COSMIC</i> satellites, the altitude profiles of the absorption coefficient of decimeter (DM) radio waves in the planet’s ionosphere during the geomagnetic storm on June 22–23, 2015, were determined. It is known that the absorption coefficient at a given fixed frequency is directly proportional to both the electron density and the collision frequency of electrons with ions and neutrals. Using the data on the vertical profiles of the absorption coefficient of DM radio waves and the electron density reconstructed from the analysis of <i>FORMOSAT-3</i>/<i>COSMIC</i> radio occultations, we estimated the effective collision frequency of electrons in the <i>D</i> and <i>E</i> regions of the Earth’s high-latitude ionosphere. The practical significance of studying the frequency of electron collisions and the effects of radio wave absorption in the <i>D</i> and <i>E</i> regions of the planet’s ionosphere is associated with maintaining the uninterrupted operation of space radio communication and navigation systems.</p>","PeriodicalId":56319,"journal":{"name":"Cosmic Research","volume":"77 1","pages":""},"PeriodicalIF":0.6,"publicationDate":"2023-11-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"138543167","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: 0

The Influence of Field-Aligned Currents on Electron Density in the Ionosphere: Combined Observations of SWARM Satellites and ESR Radar 场向电流对电离层电子密度的影响:SWARM卫星和ESR雷达的联合观测

IF 0.6 4区物理与天体物理 Q4 ASTRONOMY & ASTROPHYSICS

Cosmic Research

Pub Date : 2023-11-24 DOI: 10.1134/s0010952523700454

R. Yu. Lukianova

Abstract

The results are presented of combined measurements by the SWARM spacecraft (SC) and European incoherent scatter radar on Svalbard for two events of simultaneous observations: in the nighttime ionosphere during substorm activation on January 9, 2014, and in the daytime ionosphere under quiet conditions on February 5, 2017. Onboard magnetometers of the SWARM SC provide measurements of field-aligned current density over the ionosphere. The radar, which is under the flyby trajectory at this time, measures the vertical distribution of the electron density (Ne). Experiments have shown that, under disturbed nighttime conditions, at the location of the field-aligned current flowing from the ionosphere, the plasma density increases throughout the entire slab of the ionosphere and the change in Ne is in agreement with theoretical estimates. In the daytime quiet ionosphere, Ne increases only in the F layer, but practically does not change in the E layer. The differences may be due to the fact that, in the first case, the carriers of the upward directed current are represented by the entire energy spectrum of auroral electrons of 1–10 keV, and in the second case only by the low-energy part.

摘要介绍了2014年1月9日亚暴激活期间夜间电离层和2017年2月5日安静条件下白天电离层两个同步观测事件的SWARM卫星和欧洲非相干散射雷达联合观测结果。SWARM SC的机载磁力计提供电离层上场对准电流密度的测量。此时位于飞越轨迹下方的雷达测量电子密度(Ne)的垂直分布。实验表明，在夜间受到干扰的条件下，在电离层流出的磁场对准电流的位置，整个电离层的等离子体密度增加，Ne的变化与理论估计一致。在白天安静电离层，Ne仅在F层增加，而在E层几乎没有变化。差异可能是由于在第一种情况下，向上定向电流的载流子由1-10 keV的极光电子的整个能谱表示，而在第二种情况下仅由低能量部分表示。

{"title":"The Influence of Field-Aligned Currents on Electron Density in the Ionosphere: Combined Observations of SWARM Satellites and ESR Radar","authors":"R. Yu. Lukianova","doi":"10.1134/s0010952523700454","DOIUrl":"https://doi.org/10.1134/s0010952523700454","url":null,"abstract":"<h3 data-test=\"abstract-sub-heading\">Abstract</h3><p>The results are presented of combined measurements by the <i>SWARM</i> spacecraft (SC) and European incoherent scatter radar on Svalbard for two events of simultaneous observations: in the nighttime ionosphere during substorm activation on January 9, 2014, and in the daytime ionosphere under quiet conditions on February 5, 2017. Onboard magnetometers of the <i>SWARM</i> SC provide measurements of field-aligned current density over the ionosphere. The radar, which is under the flyby trajectory at this time, measures the vertical distribution of the electron density (Ne). Experiments have shown that, under disturbed nighttime conditions, at the location of the field-aligned current flowing from the ionosphere, the plasma density increases throughout the entire slab of the ionosphere and the change in Ne is in agreement with theoretical estimates. In the daytime quiet ionosphere, Ne increases only in the <i>F</i> layer, but practically does not change in the <i>E</i> layer. The differences may be due to the fact that, in the first case, the carriers of the upward directed current are represented by the entire energy spectrum of auroral electrons of 1–10 keV, and in the second case only by the low-energy part.</p>","PeriodicalId":56319,"journal":{"name":"Cosmic Research","volume":"19 1","pages":""},"PeriodicalIF":0.6,"publicationDate":"2023-11-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"138531242","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: 0

Features of Narrowband Stimulated Electromagnetic Emission Depending on the Effective Radiated Power of the EISCAT/Heating Facility 取决于 EISCAT/加热设施有效辐射功率的窄带受激电磁辐射特征

IF 0.6 4区物理与天体物理 Q4 ASTRONOMY & ASTROPHYSICS

Cosmic Research

Pub Date : 2023-11-24 DOI: 10.1134/S0010952523700478

A. Kalishin, N. Blagoveshchenskaya, T. Borisova, I. M. Egorov, G. A. Zagorskiy, A. S. Kovalev

引用次数: 0

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