Relevant bibliographies by topics / Magnetosphere system

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  1. Journal articles
  2. Dissertations / Theses
  3. Books
  4. Book chapters
  5. Conference papers
  6. Reports

Academic literature on the topic 'Magnetosphere system'

Author: Grafiati
Published: 6 September 2023

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Journal articles on the topic "Magnetosphere system"

1

Bunce, E. J., and S. W. H. Cowley. "A note on the ring current in Saturn’s magnetosphere: Comparison of magnetic data obtained during the Pioneer-11 and Voyager-1 and -2 fly-bys." Annales Geophysicae 21, no. 3 (March 31, 2003): 661–69. http://dx.doi.org/10.5194/angeo-21-661-2003.

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Abstract. We examine the residual (measured minus internal) magnetic field vectors observed in Saturn’s magnetosphere during the Pioneer-11 fly-by in 1979, and compare them with those observed during the Voyager-1 and -2 fly-bys in 1980 and 1981. We show for the first time that a ring current system was present within the magnetosphere during the Pioneer-11 encounter, which was qualitatively similar to those present during the Voyager fly-bys. The analysis also shows, however, that the ring current was located closer to the planet during the Pioneer-11 encounter than during the comparable Voyager-1 fly-by, reflecting the more com-pressed nature of the magnetosphere at the time. The residual field vectors have been fit using an adaptation of the current system proposed for Jupiter by Connerney et al. (1981a). A model that provides a reasonably good fit to the Pioneer-11 Saturn data extends radially between 6.5 and 12.5 RS (compared with a noon-sector magnetopause distance of 17 RS), has a north-south extent of 4 RS, and carries a total current of 9.6 MA. A corresponding model that provides a qualitatively similar fit to the Voyager data, determined previously by Connerney et al. (1983), extends radially between 8 and 15.5 RS (compared with a noon-sector magnetopause distance for Voyager-1 of 23–24 RS), has a north-south extent of 6 RS, and carries a total current of 11.5 MA.Key words. Magnetospheric physics (current systems, magnetospheric configuration and dynamics, planetary magnetospheres)
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Chelpanov, Maksim, Sergey Anfinogentov, Danila Kostarev, Olga Mikhailova, Aleksandr Rubtsov, Viktor Fedenev, and Andrey Chelpanov. "Review and comparison of MHD wave characteristics at the Sun and in Earth’s magnetosphere." Solnechno-Zemnaya Fizika 8, no. 4 (December 24, 2022): 3–28. http://dx.doi.org/10.12737/szf-84202201.

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Magnetohydrodynamic (MHD) waves play a crucial role in the plasma processes of stellar atmospheres and planetary magnetospheres. Wave phenomena in both media are known to have similarities and unique traits typical of each system. MHD waves and related phenomena in magnetospheric and solar physics are studied largely independently of each other, despite the similarity in properties of these media and the common physical foundations of wave generation and propagation. A unified approach to studying MHD waves in the Sun and Earth's magnetosphere opens up prospects for further progress in these two fields. The review examines the current state of research into MHD waves in the Sun’s atmosphere and Earth's magnetosphere. It outlines the main features of the wave propagation media: their structure, scales, and typical parameters. We describe the main theoretical models applied to wave behavior studies; discuss their advantages and limitations; compare characteristics of MHD waves in the Sun’s atmosphere and Earth’s magnetosphere; and review observation methods and tools to obtain information on waves in various media.
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Alexeev, I. I., and E. S. Belenkaya. "Modeling of the Jovian Magnetosphere." Annales Geophysicae 23, no. 3 (March 30, 2005): 809–26. http://dx.doi.org/10.5194/angeo-23-809-2005.

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Abstract. This paper presents a global model of the Jovian magnetosphere which is valid not only in the equatorial plane and near the planet, as most of the existing models are, but also at high latitudes and in the outer regions of the magnetosphere. The model includes the Jovian dipole, magnetodisc, and tail current system. The tail currents are combined with the magnetopause closure currents. All inner magnetospheric magnetic field sources are screened by the magnetopause currents. It guarantees a zero normal magnetic field component for the inner magnetospheric field at the whole magnetopause surface. By changing magnetospheric scale (subsolar distance), the model gives a possibility to study the solar wind influence on the magnetospheric structure and auroral activity. A dependence of the magnetospheric size on the solar wind dynamic pressure psw (proportional to psw-0.23) is obtained. It is a stronger dependence than in the case of the Earth's magnetosphere (psw-1/6). The model of Jupiter's magnetospheric which is presented is a unique one, as it allows one to study the solar wind and interplanetary magnetic field (IMF) effects.
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Paty, Carol, Chris S. Arridge, Ian J. Cohen, Gina A. DiBraccio, Robert W. Ebert, and Abigail M. Rymer. "Ice giant magnetospheres." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 378, no. 2187 (November 9, 2020): 20190480. http://dx.doi.org/10.1098/rsta.2019.0480.

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The ice giant planets provide some of the most interesting natural laboratories for studying the influence of large obliquities, rapid rotation, highly asymmetric magnetic fields and wide-ranging Alfvénic and sonic Mach numbers on magnetospheric processes. The geometries of the solar wind–magnetosphere interaction at the ice giants vary dramatically on diurnal timescales due to the large tilt of the magnetic axis relative to each planet's rotational axis and the apparent off-centred nature of the magnetic field. There is also a seasonal effect on this interaction geometry due to the large obliquity of each planet (especially Uranus). With in situ observations at Uranus and Neptune limited to a single encounter by the Voyager 2 spacecraft, a growing number of analytical and numerical models have been put forward to characterize these unique magnetospheres and test hypotheses related to the magnetic structures and the distribution of plasma observed. Yet many questions regarding magnetospheric structure and dynamics, magnetospheric coupling to the ionosphere and atmosphere, and potential interactions with orbiting satellites remain unanswered. Continuing to study and explore ice giant magnetospheres is important for comparative planetology as they represent critical benchmarks on a broad spectrum of planetary magnetospheric interactions, and provide insight beyond the scope of our own Solar System with implications for exoplanet magnetospheres and magnetic reversals. This article is part of a discussion meeting issue ‘Future exploration of ice giant systems'.
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Belenkaya, E. S., I. I. Alexeev, V. V. Kalegaev, and M. S. Blokhina. "Definition of Saturn's magnetospheric model parameters for the Pioneer 11 flyby." Annales Geophysicae 24, no. 3 (May 19, 2006): 1145–56. http://dx.doi.org/10.5194/angeo-24-1145-2006.

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Abstract. This paper presents a description of a method for selection parameters for a global paraboloid model of Saturn's magnetosphere. The model is based on the preexisting paraboloid terrestrial and Jovian models of the magnetospheric field. Interaction of the solar wind with the magnetosphere, i.e. the magnetotail current system, and the magnetopause currents screening all magnetospheric field sources, is taken into account. The input model parameters are determined from observations of the Pioneer 11 inbound flyby.
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Lopez, R. E., V. G. Merkin, and J. G. Lyon. "The role of the bow shock in solar wind-magnetosphere coupling." Annales Geophysicae 29, no. 6 (June 25, 2011): 1129–35. http://dx.doi.org/10.5194/angeo-29-1129-2011.

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Abstract. In this paper we examine the role of the bow shock in coupling solar wind energy to the magnetosphere using global magnetohydrodynamic simulations of the solar wind-magnetosphere interaction with southward IMF. During typical solar wind conditions, there are two significant dynamo currents in the magnetospheric system, one in the high-latitude mantle region tailward of the cusp and the other in the bow shock. As the magnitude of the (southward) IMF increases and the solar wind becomes a low Mach number flow, there is a significant change in solar wind-magnetosphere coupling. The high-latitude magnetopause dynamo becomes insignificant compared to the bow shock and a large load appears right outside the magnetopause. This leaves the bow shock current as the only substantial dynamo current in the system, and the only place where a significant amount of mechanical energy is extracted from the solar wind. That energy appears primarily as electromagnetic energy, and the Poynting flux generated at the bow shock feeds energy back into the plasma, reaccelerating it to solar wind speeds. Some small fraction of that Poynting flux is directed into the magnetosphere, supplying the energy needed for magnetospheric dynamics. Thus during periods when the solar wind flow has a low Mach number, the main dynamo in the solar wind-magnetosphere system is the bow shock.
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Lai, Ching-Ming, and Jean-Fu Kiang. "Comparative Study on Planetary Magnetosphere in the Solar System." Sensors 20, no. 6 (March 17, 2020): 1673. http://dx.doi.org/10.3390/s20061673.

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The magnetospheric responses to solar wind of Mercury, Earth, Jupiter and Uranus are compared via magnetohydrodynamic (MHD) simulations. The tilt angle of each planetary field and the polarity of solar wind are also considered. Magnetic reconnection is illustrated and explicated with the interaction between the magnetic field distributions of the solar wind and the magnetosphere.
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Arridge, C. S., N. Achilleos, and P. Guio. "Electric field variability and classifications of Titan's magnetoplasma environment." Annales Geophysicae 29, no. 7 (July 19, 2011): 1253–58. http://dx.doi.org/10.5194/angeo-29-1253-2011.

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Abstract. The atmosphere of Saturn's largest moon Titan is driven by photochemistry, charged particle precipitation from Saturn's upstream magnetosphere, and presumably by the diffusion of the magnetospheric field into the outer ionosphere, amongst other processes. Ion pickup, controlled by the upstream convection electric field, plays a role in the loss of this atmosphere. The interaction of Titan with Saturn's magnetosphere results in the formation of a flow-induced magnetosphere. The upstream magnetoplasma environment of Titan is a complex and highly variable system and significant quasi-periodic modulations of the plasma in this region of Saturn's magnetosphere have been reported. In this paper we quantitatively investigate the effect of these quasi-periodic modulations on the convection electric field at Titan. We show that the electric field can be significantly perturbed away from the nominal radial orientation inferred from Voyager 1 observations, and demonstrate that upstream categorisation schemes must be used with care when undertaking quantitative studies of Titan's magnetospheric interaction, particularly where assumptions regarding the orientation of the convection electric field are made.
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Stumpo, Mirko, Giuseppe Consolini, Tommaso Alberti, and Virgilio Quattrociocchi. "Measuring Information Coupling between the Solar Wind and the Magnetosphere–Ionosphere System." Entropy 22, no. 3 (February 28, 2020): 276. http://dx.doi.org/10.3390/e22030276.

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The interaction between the solar wind and the Earth’s magnetosphere–ionosphere system is very complex, being essentially the result of the interplay between an external driver, the solar wind, and internal processes to the magnetosphere–ionosphere system. In this framework, modelling the Earth’s magnetosphere–ionosphere response to the changes of the solar wind conditions requires a correct identification of the causality relations between the different parameters/quantities used to monitor this coupling. Nowadays, in the framework of complex dynamical systems, both linear statistical tools and Granger causality models drastically fail to detect causal relationships between time series. Conversely, information theory-based concepts can provide powerful model-free statistical quantities capable of disentangling the complex nature of the causal relationships. In this work, we discuss how to deal with the problem of measuring causal information in the solar wind–magnetosphere–ionosphere system. We show that a time delay of about 30–60 min is found between solar wind and magnetospheric and ionospheric overall dynamics as monitored by geomagnetic indices, with a great information transfer observed between the z component of the interplanetary magnetic field and geomagnetic indices, while a lower transfer is found when other solar wind parameters are considered. This suggests that the best candidate for modelling the geomagnetic response to solar wind changes is the interplanetary magnetic field component B z . A discussion of the relevance of our results in the framework of Space Weather is also provided.
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Nichols, J. D., and S. W. H. Cowley. "Magnetosphere-ionosphere coupling currents in Jupiter's middle magnetosphere: effect of precipitation-induced enhancement of the ionospheric Pedersen conductivity." Annales Geophysicae 22, no. 5 (April 8, 2004): 1799–827. http://dx.doi.org/10.5194/angeo-22-1799-2004.

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Abstract. We consider the effect of precipitation-induced enhancement of the Jovian ionospheric Pedersen conductivity on the magnetosphere-ionosphere coupling current system which is associated with the breakdown of the corotation of iogenic plasma in Jupiter's middle magnetosphere. In previous studies the Pedersen conductivity has been taken to be simply a constant, while it is expected to be significantly enhanced in the regions of upward-directed auroral field-aligned current, implying downward precipitating electrons. We develop an empirical model of the modulation of the Pedersen conductivity with field-aligned current density based on the modelling results of Millward et al. and compute the currents flowing in the system with the conductivity self-consistently dependent on the auroral precipitation. In addition, we consider two simplified models of the conductivity which provide an insight into the behaviour of the solutions. We compare the results to those obtained when the conductivity is taken to be constant, and find that the empirical conductivity model helps resolve some outstanding discrepancies between theory and observation of the plasma angular velocity and current system. Specifically, we find that the field-aligned current is concentrated in a peak of magnitude ~0.25µAm-2 in the inner region of the middle magnetosphere at ~20 RJ, rather than being more uniformly distributed as found with constant conductivity models. This peak maps to ~17° in the ionosphere, and is consistent with the position of the main oval auroras. The energy flux associated with the field-aligned current is ~10mWm-2 (corresponding to a UV luminosity of ~100kR), in a region ~0.6° in width, and the Pedersen conductivity is elevated from a background of ~0.05mho to ~0.7mho. Correspondingly, the total equatorial radial current increases greatly in the region of peak field-aligned current, and plateaus with increasing distance thereafter. This form is consistent with the observed profile of the current derived from Galileo magnetic field data. In addition, we find that the solutions using the empirical conductivity model produce an angular velocity profile which maintains the plasma near to rigid corotation out to much further distances than the constant conductivity model would suggest. Again, this is consistent with observations. Our results therefore suggest that, while the constant conductivity solutions provide an important indication that the main oval is indeed a result of the breakdown of the corotation of iogenic plasma, they do not explain the details of the observations. In order to resolve some of these discrepancies, one must take into account the elevation of the Pedersen conductivity as a result of auroral electron precipitation.Key words. Magnetospheric physics (current systems, magnetosphere-ionosphere interactions, planetary magnetospheres)70d
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Dissertations / Theses on the topic "Magnetosphere system"

1

Rosenqvist, Lisa. "Energy Transfer and Conversion in the Magnetosphere-Ionosphere System." Doctoral thesis, Uppsala University, Department of Astronomy and Space Physics, 2008. http://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-8716.

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Magnetized planets, such as Earth, are strongly influenced by the solar wind. The Sun is very dynamic, releasing varying amounts of energy, resulting in a fluctuating energy and momentum exchange between the solar wind and planetary magnetospheres. The efficiency of this coupling is thought to be controlled by magnetic reconnection occurring at the boundary between solar wind and planetary magnetic fields. One of the main tasks in space physics research is to increase the understanding of this coupling between the Sun and other solar system bodies. Perhaps the most important aspect regards the transfer of energy from the solar wind to the terrestrial magnetosphere as this is the main source for driving plasma processes in the magnetosphere-ionosphere system. This may also have a direct practical influence on our life here on Earth as it is responsible for Space Weather effects. In this thesis I investigate both the global scale of the varying solar-terrestrial coupling and local phenomena in more detail. I use mainly the European Space Agency Cluster mission which provide unprecedented three-dimensional observations via its formation of four identical spacecraft. The Cluster data are complimented with observations from a broad range of instruments both onboard spacecraft and from groundbased magnetometers and radars.

A period of very strong solar driving in late October 2003 is investigated. We show that some of the strongest substorms in the history of magnetic recordings were triggered by pressure pulses impacting a quasi-stable magnetosphere. We make for the first time direct estimates of the local energy flow into the magnetotail using Cluster measurements. Observational estimates suggest a good energy balance between the magnetosphere-ionosphere system while empirical proxies seem to suffer from over/under estimations during such extreme conditions.

Another period of extreme interplanetary conditions give rise to accelerated flows along the magnetopause which could account for an enhanced energy coupling between the solar wind and the magnetosphere. We discuss whether such conditions could explain the simultaneous observation of a large auroral spiral across the polar cap.

Contrary to extreme conditions the energy conversion across the dayside magnetopause has been estimated during an extended period of steady interplanetary conditions. A new method to determine the rate at which reconnection occurs is described that utilizes the magnitude of the local energy conversion from Cluster. The observations show a varying reconnection rate which support the previous interpretation that reconnection is continuous but its rate is modulated.

Finally, we compare local energy estimates from Cluster with a global magnetohydrodynamic simulation. The results show that the observations are reliably reproduced by the model and may be used to validate and scale global magnetohydrodynamic models.

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Gane, Stuart Carlos. "Continuous pulsation dynamics in the high-latitude magnetosphere-ionosphere system." Thesis, University of Leicester, 2011. http://hdl.handle.net/2381/9695.

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The thesis investigates Ultra Low Frequency waves in the band 0.1 Hz to 5 Hz in the terrestrial magnetosphere-ionosphere system. Utilising mid-high latitude ground-based induction coil magnetometers, continuous (Pc1-2) and irregular (Pi1-c) pulsations are explored through the application of digital spectral analysis. An assessment of two spectral analysis techniques is conducted. From which it is concluded that, for routine ground-based analysis of Pc1-2 pulsations, treating the horizontal components of magnetic field variation as a single complex signal is computationally beneficial with minimal loss of useful information. Polarisation parameters and values of cross spectral phase are derived using a weighted histogram technique and are subsequently used to distinguish discrete pulsations and infer their location through simple triangulation. The results of a statistical study of ~1200 discrete Pc1-2 events over the full year of 2007, during the declining phase of solar cycle 23, are presented. This study, for the first time, reports the ground-based polarisation properties of Pc1-2 waves as a function of latitude. The derived diurnal frequency behaviour supports the suggestion that the Ionospheric Alfvén Resonator may play a part in the filtration of ground-based Pc1 observations. Pc1-2 behaviour over the course of 26 geomagnetic storms is also presented, with support being found for the association of pulsation enhancement with plasmaspheric plume formation in the recovery phase. A case study, combining coherent and incoherent radar, in situ particle measurements and ground based magnetometry, has focused on high latitude Pi-c activity during a period of enhanced dayside reconnection. This study has provided support for the association of Electromagnetic Ion cyclotron waves with the SuperDARN spectral width enhancements observed in the flanks of the ionospheric cusp.
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Nakata, Hiroyuki. "The standing toroidal mode oscillations in the magnetosphere-ionosphere system." 京都大学 (Kyoto University), 2000. http://hdl.handle.net/2433/157196.

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要旨pdfファイル:タイトル「磁気圏電離圏結合系における定在トロイダルモード振動」
本文データは平成22年度国立国会図書館の学位論文(博士)のデジタル化実施により作成された画像ファイルを基にpdf変換したものである
Kyoto University (京都大学)
0048
新制・課程博士
博士(理学)
甲第8164号
理博第2186号
新制||理||1156(附属図書館)
UT51-2000-F68
京都大学大学院理学研究科地球惑星科学専攻
(主査)教授 藤田 茂, 教授 荒木 徹, 助教授 町田 忍
学位規則第4条第1項該当
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Bunce, Emma J. "Large-scale current systems in the Jovian magnetosphere." Thesis, University of Leicester, 2001. http://hdl.handle.net/2381/30647.

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The studies contained within this thesis focus on the large-scale azimuthal and radial current systems of Jupiter's middle magnetosphere, i.e. currents with radial ranges of 20-50 RJ. In the first study using magnetometer data from Pioneer-10 and -11, Voyager-1 and -2, and Ulysses, it is discovered that the azimuthal current in the middle magnetosphere is not axi-symmetric as had been assumed for the last twenty-five years, but that it is stronger on the nightside than on the dayside at a given radial distance. A simple empirical model is formulated, which reasonably describes the data in the domain of interest both in radial distance and local time, and allows direct calculation of the current divergence associated with the asymmetry. In a similar way, in the following chapter the radial currents have been computed for the dawn sector of the jovian magnetosphere along various fly-by trajectories. Combination of these radial current estimations with the azimuthal current model allows the total divergence of the equatorial current to be calculated. These current densities mapped to the ionosphere are surprisingly large at ~1A m-2. In order to carry the current, the magnetosphere electrons must be strongly accelerated along the field lines into the ionosphere by voltages of the order of 100 kV. The resulting energy flux is enough to produce deep, bright (Mega Rayleigh) aurora and thus provides the first natural explanation of the main jovian auroral oval. In the final study, newly-available data from the Galileo orbiter mission are combined with the fly-by data in order to compare them to the model derived in the first study. The model is then re-derived for the entire data set, which significantly improves the associated fractional errors.
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Wei, Xing. "Optimization of Strongly Nonlinear Dynamical Systems Using a Modified Genetic Algorithm With Micro-Movement (MGAM)." DigitalCommons@USU, 2009. https://digitalcommons.usu.edu/etd/450.

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The genetic algorithm (GA) is a popular random search and optimization method inspired by the concepts of crossover, random mutation, and natural selection from evolutionary biology. The real-valued genetic algorithm (RGA) is an improved version of the genetic algorithm designed for direct operation on real-valued variables. In this work, a modified version of a genetic algorithm is introduced, which is called a modified genetic algorithm with micro-movement (MGAM). It implements a particle swarm optimization(PSO)-inspired micro-movement phase that helps to improve the convergence rate, while employing the e'cient GA mechanism for maintaining population diversity. In order to test the capability of the MGAM, we firrst implement it on five generally used test functions. Then we test the MGAM on two typical nonlinear dynamical systems. The performance of the MGAM is compared to a basic RGA on all these applications. Finally, we implement the MGAM on the most important application, which is the plasma physics-based model of the solar wind-driven magnetosphere-ionosphere system (WINDMI). In order to use this model for real-time prediction of geomagnetic activity, the model parameters require up-dating every 6-8 hours. We use the MGAM to train the parameters of the model in order to achieve the lowest mean square error (MSE) against the measured auroral electrojet (AL) and Dst indices. The performance of the MGAM is compared to the RGA on historical geomagnetic storm datasets. While the MGAM performs substantially better than the RGA when evaluating standard test functions, the improvement is about 6-12 percent when used on the 20D nonlinear dynamical WINDMI model.
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Ziemba, Timothy Martin. "Experimental investigation of the mini-magnetospheric plasma propulsion prototype /." Thesis, Connect to this title online; UW restricted, 2003. http://hdl.handle.net/1773/9962.

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Lachin, Anoosh. "Low frequency waves in the solar system." Thesis, Imperial College London, 1998. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.267713.

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Roussos, Elias. "Interactions of weakly or non-magnetized bodies with solar system plasmas Mars and the moons of Saturn." [Katlenburg-Lindau] Copernicus Publ, 2008. http://d-nb.info/988508095/04.

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Cramoysan, Mark. "Modelling current systems associated with substorms : results and use in the location of the substorm current wedge." Thesis, University of York, 1992. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.306513.

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Retinò, Alessandro. "Magnetic Reconnection in Space Plasmas : Cluster Spacecraft Observations." Doctoral thesis, Uppsala University, Department of Astronomy and Space Physics, 2007. http://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-7891.

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Magnetic reconnection is a universal process occurring at boundaries between magnetized plasmas, where changes in the topology of the magnetic field lead to the transport of charged particles across the boundaries and to the conversion of electromagnetic energy into kinetic and thermal energy of the particles. Reconnection occurs in laboratory plasmas, in solar system plasmas and it is considered to play a key role in many other space environments such as magnetized stars and accretion disks around stars and planets under formation. Magnetic reconnection is a multi-scale plasma process where the small spatial and temporal scales are strongly coupled to the large scales. Reconnection is initiated rapidly in small regions by microphysical processes but it affects very large volumes of space for long times. The best laboratory to experimentally study magnetic reconnection at different scales is the near-Earth space, the so-called Geospace, where Cluster spacecraft in situ measurements are available. The European Space Agency Cluster mission is composed of four-spacecraft flying in a formation and this allows, for the first time, simultaneous four-point measurements at different scales, thanks to the changeable spacecraft separation. In this thesis Cluster observations of magnetic reconnection in Geospace are presented both at large and at small scales.

At large temporal (a few hours) and spatial (several thousands km) scales, both fluid and kinetic evidence of reconnection is provided. The evidence consist of ions accelerated and transmitted across the Earth’s magnetopause. The observations show that component reconnection occurs at the magnetopause and that reconnection is continuous in time.

The microphysics of reconnection is investigated at smaller temporal (a few ion gyroperiods) and spatial (a few ion gyroradii) scales. Two regions are important for the microphysics: the X-region, around the X-line, where reconnection is initiated and the separatrix region, away from the X-line, where most of the energy conversion occurs. Observations of a separatrix region at the magnetopause are shown and the microphysics is described in detail. The separatrix region is shown to be highly structured and dynamic even away from the X-line.

Finally the discovery of magnetic reconnection in turbulent plasma is presented by showing, for the first time, in situ evidence of reconnection in a thin current sheet found in the turbulent plasma downstream of the quasi-parallel Earth’s bow shock. It is shown that turbulent reconnection is fast and that electromagnetic energy is converted into heating and acceleration of particles in turbulent plasma. It is also shown that reconnecting current sheets are abundant in turbulent plasma and that reconnection can be an efficient energy dissipation mechanism.

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Books on the topic "Magnetosphere system"

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Chappell, Charles R., Robert W. Schunk, Peter M. Banks, James L. Burch, and Richard M. Thorne, eds. Magnetosphere-Ionosphere Coupling in the Solar System. Hoboken, NJ, USA: John Wiley & Sons, Inc., 2016. http://dx.doi.org/10.1002/9781119066880.

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United States. National Aeronautics and Space Administration., ed. Modeling of the magnetosphere-ionosphere-atmosphere system. [Washington, DC: National Aeronautics and Space Administration, 1994.

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H, Waite J., Burch J. L. 1942-, Moore R. L. 1942-, AGU Books Board, and Yosemite Conference on Outstanding Problems in Solar System Plasma Physics: Theory and Instrumentation (1988 : Yosemite National Park, Calif.), eds. Solar system plasma physics. Washington, DC: American Geophysical Union, 1989.

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Cravens, Thomas E. Physics of solar system plasmas. Cambridge: Cambridge University Press, 1997.

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Keiling, Andreas, Caitríona M. Jackman, and Peter A. Delamere. Magnetotails in the solar system. Washington, D.C: American Geophysical Union, 2015.

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1943-, Priest E. R., and Summer School on Solar System Plasmas (1984 : Imperial College), eds. Solar system magnetic fields. Dordrecht, Holland: D. Reidel Pub. Co., 1985.

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1942-, Burch J. L., and Waite J. H, eds. Solar system plasmas in space and time. Washington, DC: American Geophysical Union, 1994.

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United States. National Aeronautics and Space Administration., ed. Semi-annual report on NASA grant NAGW5-1097: MIAMI, modeling of the magnetosphere-ionosphere-atmosphere system, 1 November 1996 to 31 March 1997. [Washington, DC: National Aeronautics and Space Administration, 1997.

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1943-, Priest E. R., and Hood Alan W, eds. Advances in solar system magnetohydrodynamics. Cambridge [England]: Cambridge University Press, 1991.

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K, Biernat H., ed. The solar wind-magnetosphere system 2: Proceedings of the international workshop held in Graz, September 27-29, 1995. Wien: Verlag der Österreichische Akademie der Wissenschaften, 1997.

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Book chapters on the topic "Magnetosphere system"

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Bertotti, Bruno, and Paolo Farinella. "Magnetosphere." In Physics of the Earth and the Solar System, 177–203. Dordrecht: Springer Netherlands, 1990. http://dx.doi.org/10.1007/978-94-009-1916-7_9.

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Delamere, P. A. "Solar Wind Interaction with Giant Magnetospheres and Earth's Magnetosphere." In Magnetotails in the Solar System, 217–33. Hoboken, NJ: John Wiley & Sons, Inc, 2015. http://dx.doi.org/10.1002/9781118842324.ch13.

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Walker, Raymond J., and Keiichiro Fukazawa. "Simulation Studies of Magnetosphere and Ionosphere Coupling in Saturn's Magnetosphere." In Magnetosphere-Ionosphere Coupling in the Solar System, 335–44. Hoboken, NJ, USA: John Wiley & Sons, Inc., 2016. http://dx.doi.org/10.1002/9781119066880.ch26.

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Horanyi, Mihaly. "Charged Dust in the Earth'S Magnetosphere." In Solar System Plasma Physics, 457–60. Washington, D. C.: American Geophysical Union, 2013. http://dx.doi.org/10.1029/gm054p0457.

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Westlake, Joseph H., Thomas E. Cravens, Robert E. Johnson, Stephen A. Ledvina, Janet G. Luhmann, Donald G. Mitchell, Matthew S. Richard, et al. "Titan's Interaction with Saturn's Magnetosphere." In Magnetosphere-Ionosphere Coupling in the Solar System, 291–305. Hoboken, NJ, USA: John Wiley & Sons, Inc., 2016. http://dx.doi.org/10.1002/9781119066880.ch23.

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Gallagher, D. L. "The inner magnetosphere imager mission." In Solar System Plasmas in Space and Time, 265–74. Washington, D. C.: American Geophysical Union, 1994. http://dx.doi.org/10.1029/gm084p0265.

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Cheng, A. F., and S. M. Krimigis. "Energetic Neutral Particle Imaging of Saturn'S Magnetosphere." In Solar System Plasma Physics, 253–60. Washington, D. C.: American Geophysical Union, 2013. http://dx.doi.org/10.1029/gm054p0253.

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Bolton, Scott J., Fran Bagenal, Michel Blanc, Timothy Cassidy, Emmanuel Chané, Caitriona Jackman, Xianzhe Jia, et al. "Jupiter’s Magnetosphere: Plasma Sources and Transport." In Plasma Sources of Solar System Magnetospheres, 209–36. New York, NY: Springer New York, 2016. http://dx.doi.org/10.1007/978-1-4939-3544-4_6.

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Burch, James L. "Magnetosphere-Ionosphere Coupling, Past to Future." In Magnetosphere-Ionosphere Coupling in the Solar System, 1–17. Hoboken, NJ, USA: John Wiley & Sons, Inc., 2016. http://dx.doi.org/10.1002/9781119066880.ch1.

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Walker, Raymond J., Tatsuki Ogino, and Maha Ashour-Abdalla. "Simulating the Magnetosphere: The Structure of the Magnetotail." In Solar System Plasma Physics, 61–68. Washington, D. C.: American Geophysical Union, 2013. http://dx.doi.org/10.1029/gm054p0061.

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Conference papers on the topic "Magnetosphere system"

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Sharma, A. Surjalal, A. Sen, S. Sharma, and P. N. Guzdar. "The Magnetosphere: A Complex Driven System." In INTERNATIONAL SYMPOSIUM ON WAVES, COHERENT STRUCTURES AND TURBULENCE IN PLASMAS. AIP, 2010. http://dx.doi.org/10.1063/1.3526148.

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V. Vorobev, Andrei, and Gulnara R. Shakirova. "Geoinformation System for Analytical Control and Forecast of the Earth’s Magnetosphere Parameters." In 2nd International Conference on Geographical Information Systems Theory, Applications and Management. SCITEPRESS - Science and and Technology Publications, 2016. http://dx.doi.org/10.5220/0005730201930200.

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Nwankwo, Victor Uchenna J., William Denig, Muyiwa P. Ajakaiye, Wahabbi Akanni, Johnson Fatokun, Sandip K. Chakrabarti, Jean-Pierre Raulin, Emilia Correia, and John E. Enoh. "Simulation of atmospheric drag effect on low Earth orbit satellites during intervals of perturbed and quiet geomagnetic conditions in the magnetosphere-ionosphere system." In 2020 International Conference in Mathematics, Computer Engineering and Computer Science (ICMCECS). IEEE, 2020. http://dx.doi.org/10.1109/icmcecs47690.2020.247003.

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D'Huys, Elke, Petra Vanlommel, Jan Janssens, and Ronald Van der Linden. "Come fly with us: services provided by the Space Weather Education Centre." In Symposium on Space Educational Activities (SSAE). Universitat Politècnica de Catalunya, 2022. http://dx.doi.org/10.5821/conference-9788419184405.004.

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The Solar-Terrestrial Centre of Excellence brings together and supports sun-space-earth research and services present at the federal level in Belgium. In 2019, the STCE was a founding member of a European network, PECASUS, that provides space weather services for civil aviation. Our expertise in solar observations and research combined with the experience of our Global Navigation Satellite System and solar particle radiation group proved to be crucial. The STCE also strongly invests in education and training as these are a backbone of quality research and services, and therefore created the Space Weather Education Centre. This centre offers the Space Weather Introductory Course covering the Sun, solar storms, heliosphere, ionosphere, magnetosphere, instruments and methods to observe solar and space weather activity, as well as reading and interpreting our space weather bulletins. This course is taught to future space weather advisory staff, both military and civilian. It is based upon the STCE’s expertise gained through scientific research, involvement in space missions and space weather monitoring, and on its forecasting capabilities. The course is given by qualified staff. In addition to the Space Weather Introductory Course, the STCE has been and remains involved in a wide range of outreach activities, from public lectures, over dedicated classes and workshops at schools, organization of public events like open doors, publications in popular journals and on online media, scientific newsletters and press releases, to the participation in science festivals and the organization of events for the scientific community. In this paper, we present more details of our educational programme, reflect on the methodologies used, and provide an overview of the obtained results
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Krimigis, Stamatios M., Dimitris Vassiliadis, Shing F. Fung, Xi Shao, Ioannis A. Daglis, and Joseph D. Huba. "Saturn’s magnetosphere: An example of dynamic planetary systems." In MODERN CHALLENGES IN NONLINEAR PLASMA PHYSICS: A Festschrift Honoring the Career of Dennis Papadopoulos. AIP, 2011. http://dx.doi.org/10.1063/1.3544327.

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Mao, Yao-Ting, David Auslander, David Pankow, and John Sample. "Estimating Angular Velocity, Attitude Orientation With Controller Design for Three Units CubeSat." In ASME 2014 Dynamic Systems and Control Conference. American Society of Mechanical Engineers, 2014. http://dx.doi.org/10.1115/dscc2014-5895.

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CINEMA (CubeSat for Ions, Neutrals, Electrons and MAgneticfields) will image energetic neutral atoms (ENAs) in the magnetosphere, and make measurements of electrons, ions, and magnetic fields at high latitudes. To satisfy the mission requirements, the three unit cubesat was designed. The spin axis needs to be in the ecliptic normal and the spin rate needs to be 4 rpm. The only power source for CINEMA is the solar panels. External torques are generated by an orthogonal pair of coils acting with the earths magnetic field. This paper provides the control strategy, given the limited power and available sensors, to optimize the convergence of the spin and attitude control.
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Atwell, Bill, Brandon Reddell, Bill Bartholet, John Nealy, Martha Clowdsley, Brooke Anderson, Thomas Miller, and Lawrence W. Townsend. "Parametric Shielding Strategies for Jupiter Magnetospheric Missions." In International Conference On Environmental Systems. 400 Commonwealth Drive, Warrendale, PA, United States: SAE International, 2005. http://dx.doi.org/10.4271/2005-01-2834.

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Sharma, A. Surjalal. "Complexity in nature and data-enabled science: The Earth's magnetosphere." In INTERNATIONAL CONFERENCE ON COMPLEX PROCESSES IN PLASMAS AND NONLINEAR DYNAMICAL SYSTEMS. AIP Publishing LLC, 2014. http://dx.doi.org/10.1063/1.4865343.

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Ogawa, Hiroyuki, Tsutomu Yamazaki, Akira Okamoto, Naoko Iwata, and Shun Okazaki. "BepiColombo Mercury Magnetospheric Orbiter Flight Model Thermal Analysis." In 42nd International Conference on Environmental Systems. Reston, Virigina: American Institute of Aeronautics and Astronautics, 2012. http://dx.doi.org/10.2514/6.2012-3578.

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Steffy, S. V., and S. S. Ghosh. "Interpretation of non-conventional coherent structures in magnetospheric plasma system." In 2019 URSI Asia-Pacific Radio Science Conference (AP-RASC). IEEE, 2019. http://dx.doi.org/10.23919/ursiap-rasc.2019.8738136.

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Reports on the topic "Magnetosphere system"

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Branduardi-Raymont, Graziella, and et al. SMILE Definition Study Report. ESA SCI, December 2018. http://dx.doi.org/10.5270/esa.smile.definition_study_report-2018-12.

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The SMILE definition study report describes a novel self-standing mission dedicated to observing solar wind-magnetosphere coupling via simultaneous in situ solar wind/magnetosheath plasma and magnetic field measurements, X-Ray images of the magnetosheath and magnetic cusps, and UV images of global auroral distributions defining system-level consequences. The Solar wind Magnetosphere Ionosphere Link Explorer (SMILE) will complement all solar, solar wind and in situ magnetospheric observations, including both space- and ground-based observatories, to enable the first-ever observations of the full chain of events that drive the Sun-Earth connection.
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Forbes, Jeffrey M. Self-Consistent Modeling of the Ionosphere-Thermosphere-Magnetosphere System. Fort Belvoir, VA: Defense Technical Information Center, May 1992. http://dx.doi.org/10.21236/ada253232.

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BARKHATOV, NIKOLAY, and SERGEY REVUNOV. A software-computational neural network tool for predicting the electromagnetic state of the polar magnetosphere, taking into account the process that simulates its slow loading by the kinetic energy of the solar wind. SIB-Expertise, December 2021. http://dx.doi.org/10.12731/er0519.07122021.

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The auroral activity indices AU, AL, AE, introduced into geophysics at the beginning of the space era, although they have certain drawbacks, are still widely used to monitor geomagnetic activity at high latitudes. The AU index reflects the intensity of the eastern electric jet, while the AL index is determined by the intensity of the western electric jet. There are many regression relationships linking the indices of magnetic activity with a wide range of phenomena observed in the Earth's magnetosphere and atmosphere. These relationships determine the importance of monitoring and predicting geomagnetic activity for research in various areas of solar-terrestrial physics. The most dramatic phenomena in the magnetosphere and high-latitude ionosphere occur during periods of magnetospheric substorms, a sensitive indicator of which is the time variation and value of the AL index. Currently, AL index forecasting is carried out by various methods using both dynamic systems and artificial intelligence. Forecasting is based on the close relationship between the state of the magnetosphere and the parameters of the solar wind and the interplanetary magnetic field (IMF). This application proposes an algorithm for describing the process of substorm formation using an instrument in the form of an Elman-type ANN by reconstructing the AL index using the dynamics of the new integral parameter we introduced. The use of an integral parameter at the input of the ANN makes it possible to simulate the structure and intellectual properties of the biological nervous system, since in this way an additional realization of the memory of the prehistory of the modeled process is provided.
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Meng, C. I., and P. T. Newell. Investigations of Magnetosphere-Ionosphere Coupling Relevant to Operational Systems. Fort Belvoir, VA: Defense Technical Information Center, February 1988. http://dx.doi.org/10.21236/ada195972.

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Hilmer, R. V. A Magnetospheric Neutral Sheet-Oriented Coordinate System for MSM and MSFM Applications. Fort Belvoir, VA: Defense Technical Information Center, July 1997. http://dx.doi.org/10.21236/ada338067.

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