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Gotowa bibliografia na temat „Earth's Magnetosheath”

Autor: Grafiati

Data publikacji: 6 września 2023

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Artykuły w czasopismach na temat "Earth's Magnetosheath"

Artemyev, A. V., C. Shi, Y. Lin, Y. Nishimura, C. Gonzalez, J. Verniero, X. Wang, M. Velli, A. Tenerani i N. Sioulas. "Ion Kinetics of Plasma Flows: Earth's Magnetosheath versus Solar Wind". Astrophysical Journal 939, nr 2 (1.11.2022): 85. http://dx.doi.org/10.3847/1538-4357/ac96e4.

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Abstract Revealing the formation, dynamics, and contribution to plasma heating of magnetic field fluctuations in the solar wind is an important task for heliospheric physics and for a general plasma turbulence theory. Spacecraft observations in the solar wind are limited to spatially localized measurements, so that the evolution of fluctuation properties with solar wind propagation is mostly studied via statistical analyses of data sets collected by different spacecraft at various radial distances from the Sun. In this study we investigate the evolution of turbulence in the Earth’s magnetosheath, a plasma system sharing many properties with the solar wind. The near-Earth space environment is being explored by multiple spacecraft missions, which may allow us to trace the evolution of magnetosheath fluctuations with simultaneous measurements at different distances from their origin, the Earth’s bow shock. We compare ARTEMIS and Magnetospheric Multiscale (MMS) Mission measurements in the Earth magnetosheath and Parker Solar Probe measurements of the solar wind at different radial distances. The comparison is supported by three numerical simulations of the magnetosheath magnetic and plasma fluctuations: global hybrid simulation resolving ion kinetic and including effects of Earth’s dipole field and realistic bow shock, hybrid and Hall-MHD simulations in expanding boxes that mimic the magnetosheath volume expansion with the radial distance from the dayside bow shock. The comparison shows that the magnetosheath can be considered as a miniaturized version of the solar wind system with much stronger plasma thermal anisotropy and an almost equal amount of forward and backward propagating Alfvén waves. Thus, many processes, such as turbulence development and kinetic instability contributions to plasma heating, occurring on slow timescales and over large distances in the solar wind, occur more rapidly in the magnetosheath and can be investigated in detail by multiple near-Earth spacecraft.

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Turc, Lucile, Vertti Tarvus, Andrew P. Dimmock, Markus Battarbee, Urs Ganse, Andreas Johlander, Maxime Grandin, Yann Pfau-Kempf, Maxime Dubart i Minna Palmroth. "Asymmetries in the Earth's dayside magnetosheath: results from global hybrid-Vlasov simulations". Annales Geophysicae 38, nr 5 (6.10.2020): 1045–62. http://dx.doi.org/10.5194/angeo-38-1045-2020.

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Abstract. Bounded by the bow shock and the magnetopause, the magnetosheath forms the interface between solar wind and magnetospheric plasmas and regulates solar wind–magnetosphere coupling. Previous works have revealed pronounced dawn–dusk asymmetries in the magnetosheath properties. The dependence of these asymmetries on the upstream parameters remains however largely unknown. One of the main sources of these asymmetries is the bow shock configuration, which is typically quasi-parallel on the dawn side and quasi-perpendicular on the dusk side of the terrestrial magnetosheath because of the Parker spiral orientation of the interplanetary magnetic field (IMF) at Earth. Most of these previous studies rely on collections of spacecraft measurements associated with a wide range of upstream conditions which are processed in order to obtain average values of the magnetosheath parameters. In this work, we use a different approach and quantify the magnetosheath asymmetries in global hybrid-Vlasov simulations performed with the Vlasiator model. We concentrate on three parameters: the magnetic field strength, the plasma density, and the flow velocity. We find that the Vlasiator model reproduces the polarity of the asymmetries accurately but that their level tends to be higher than in spacecraft measurements, probably because the magnetosheath parameters are obtained from a single set of upstream conditions in the simulation, making the asymmetries more prominent. A set of three runs with different upstream conditions allows us to investigate for the first time how the asymmetries change when the angle between the IMF and the Sun–Earth line is reduced and when the Alfvén Mach number decreases. We find that a more radial IMF results in a stronger magnetic field asymmetry and a larger variability of the magnetosheath density. In contrast, a lower Alfvén Mach number leads to a reduced magnetic field asymmetry and a decrease in the variability of the magnetosheath density, the latter likely due to weaker foreshock processes. Our results highlight the strong impact of the quasi-parallel shock and its associated foreshock on global magnetosheath properties, in particular on the magnetosheath density, which is extremely sensitive to transient quasi-parallel shock processes, even with the perfectly steady upstream conditions in our simulations. This could explain the large variability of the density asymmetry levels obtained from spacecraft measurements in previous studies.

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Longmore, M., S. J. Schwartz i E. A. Lucek. "Rotation of the magnetic field in Earth's magnetosheath by bulk magnetosheath plasma flow". Annales Geophysicae 24, nr 1 (7.03.2006): 339–54. http://dx.doi.org/10.5194/angeo-24-339-2006.

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Abstract. Orientations of the observed magnetic field in Earth's dayside magnetosheath are compared with the predicted field line-draping pattern from the Kobel and Flückiger static magnetic field model. A rotation of the overall magnetosheath draping pattern with respect to the model prediction is observed. For an earthward Parker spiral, the sense of the rotation is typically clockwise for northward IMF and anticlockwise for southward IMF. The rotation is consistent with an interpretation which considers the twisting of the magnetic field lines by the bulk plasma flow in the magnetosheath. Histogram distributions describing the differences between the observed and model magnetic field clock angles in the magnetosheath confirm the existence and sense of the rotation. A statistically significant mean value of the IMF rotation in the range 5°-30° is observed in all regions of the magnetosheath, for all IMF directions, although the associated standard deviation implies large uncertainty in the determination of an accurate value for the rotation. We discuss the role of field-flow coupling effects and dayside merging on field line draping in the magnetosheath in view of the evidence presented here and that which has previously been reported by Kaymaz et al. (1992).

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Song, P. "Forecasting Earth's magnetopause, magnetosheath, and bow shock". IEEE Transactions on Plasma Science 28, nr 6 (2000): 1966–75. http://dx.doi.org/10.1109/27.902225.

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Walsh, B. M., D. G. Sibeck, Y. Wang i D. H. Fairfield. "Dawn-dusk asymmetries in the Earth's magnetosheath". Journal of Geophysical Research: Space Physics 117, A12 (grudzień 2012): n/a. http://dx.doi.org/10.1029/2012ja018240.

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ONSAGER, T. G., i M. F. THOMSEN. "The Earth's Foreshock, Bow Shock, and Magnetosheath". Reviews of Geophysics 29, S2 (styczeń 1991): 998–1007. http://dx.doi.org/10.1002/rog.1991.29.s2.998.

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Guicking, L., K. H. Glassmeier, H. U. Auster, Y. Narita i G. Kleindienst. "Low-frequency magnetic field fluctuations in Earth's plasma environment observed by THEMIS". Annales Geophysicae 30, nr 8 (27.08.2012): 1271–83. http://dx.doi.org/10.5194/angeo-30-1271-2012.

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Abstract. Low-frequency magnetic wave activity in Earth's plasma environment was determined based on a statistical analysis of THEMIS magnetic field data. We observe that the spatial distribution of low-frequency magnetic field fluctuations reveals highest values in the magnetosheath, but the observations differ qualitatively from observations at Venus presented in a previous study since significant wave activity at Earth is also observed in the nightside magnetosheath. Outside the magnetosheath the low-frequency wave activity level is generally very low. By means of an analytical streamline model for the magnetosheath plasma flow, we are able to investigate the spatial and temporal evolution of wave intensity along particular streamlines in order to characterise possible wave generation mechanisms. We observe a decay of wave intensity along the streamlines, but contrary to the situation at Venus, we obtain good qualitative agreement with the theoretical concept of freely evolving/decaying turbulence. Differences between the dawn region and the dusk region can be observed only further away from the magnetopause. We conclude that wave generation mechanisms may be primarily attributed to processes at or in the vicinity of the bow shock. The difference with the observations of the Venusian magnetosheath we interpret to be the result of the different types of solar wind interaction processes since the Earth possesses a global magnetic field while Venus does not, and therefore the observed magnetic wave activities may be caused by diverse magnetic field controlled characteristics of wave generation processes.

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Turc, L., D. Fontaine, P. Savoini i E. K. J. Kilpua. "Magnetic clouds' structure in the magnetosheath as observed by Cluster and Geotail: four case studies". Annales Geophysicae 32, nr 10 (15.10.2014): 1247–61. http://dx.doi.org/10.5194/angeo-32-1247-2014.

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Abstract. Magnetic clouds (MCs) are large-scale magnetic flux ropes ejected from the Sun into the interplanetary space. They play a central role in solar–terrestrial relations as they can efficiently drive magnetic activity in the near-Earth environment. Their impact on the Earth's magnetosphere is often attributed to the presence of southward magnetic fields inside the MC, as observed in the upstream solar wind. However, when they arrive in the vicinity of the Earth, MCs first encounter the bow shock, which is expected to modify their properties, including their magnetic field strength and direction. If these changes are significant, they can in turn affect the interaction of the MC with the magnetosphere. In this paper, we use data from the Cluster and Geotail spacecraft inside the magnetosheath and from the Advanced Composition Explorer (ACE) upstream of the Earth's environment to investigate the impact of the bow shock's crossing on the magnetic structure of MCs. Through four example MCs, we show that the evolution of the MC's structure from the solar wind to the magnetosheath differs largely from one event to another. The smooth rotation of the MC can either be preserved inside the magnetosheath, be modified, i.e. the magnetic field still rotates slowly but at different angles, or even disappear. The alteration of the magnetic field orientation across the bow shock can vary with time during the MC's passage and with the location inside the magnetosheath. We examine the conditions encountered at the bow shock from direct observations, when Cluster or Geotail cross it, or indirectly by applying a magnetosheath model. We obtain a good agreement between the observed and modelled magnetic field direction and shock configuration, which varies from quasi-perpendicular to quasi-parallel in our study. We find that the variations in the angle between the magnetic fields in the solar wind and in the magnetosheath are anti-correlated with the variations in the shock obliquity. When the shock is in a quasi-parallel regime, the magnetic field direction varies significantly from the solar wind to the magnetosheath. In such cases, the magnetic field reaching the magnetopause cannot be approximated by the upstream magnetic field. Therefore, it is important to take into account the conditions at the bow shock when estimating the impact of an MC with the Earth's environment because these conditions are crucial in determining the magnetosheath magnetic field, which then interacts with the magnetosphere.

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Hou, Chuanpeng, Jiansen He, Die Duan, Xingyu Zhu, Wenya Li, Daniel Verscharen, Terry Liu i Tieyan Wang. "Efficient Energy Conversion through Vortex Arrays in the Turbulent Magnetosheath". Astrophysical Journal 946, nr 1 (1.03.2023): 13. http://dx.doi.org/10.3847/1538-4357/acb927.

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Abstract Turbulence is often enhanced when transmitted through a collisionless plasma shock. We investigate how the enhanced turbulent energy in the Earth's magnetosheath effectively dissipates via vortex arrays. This research topic is of great importance as it relates to particle energization at astrophysical shocks across the universe. Wave modes and intermittent coherent structures are the key candidate mechanisms for energy conversion in turbulent plasmas. Here, by comparing in-situ measurements in the Earth's magnetosheath with a theoretical model, we find the existence of vortex arrays at the transition between the downstream regions of the Earth's bow shock. Vortex arrays consist of quasi-orthogonal kinetic waves and exhibit both high volumetric filling factors and strong local energy conversion, thereby showing a greater dissipative energization than traditional waves and coherent structures. Therefore, we propose that vortex arrays are a promising mechanism for efficient energy conversion in the sheath regions downstream of astrophysical shocks.

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Paschalidis, N. P., S. M. Krimigis, E. T. Sarris, D. G. Sibeck, R. W. McEntire, S. P. Christon i L. J. Zanetti. "Ion burst event in the Earth's dayside magnetosheath". Geophysical Research Letters 18, nr 3 (marzec 1991): 377–80. http://dx.doi.org/10.1029/91gl00140.

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Rozprawy doktorskie na temat "Earth's Magnetosheath"

Archer, Martin. "Dynamic pressure pulses in Earth's dayside magnetosheath". Thesis, Imperial College London, 2014. http://hdl.handle.net/10044/1/24743.

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Solar wind mass, energy and momentum can be transferred to Earth's magnetosphere at the magnetopause with the shocked magnetosheath acting as an interface between the two regions. In particular the magnetosheath pressure is important in terms of the position and motion of the magnetopause, which in turn can have effects throughout the dayside magnetosphere. A variety of transient phenomena often occur in the magnetosheath and in this thesis one example is studied, namely pulses in the magnetosheath dynamic pressure, using multipoint spacecraft observations to investigate their origins and magnetospheric impacts and illuminate dayside magnetospheric dynamics. Simultaneous observations in the solar wind, foreshock and magnetosheath reveal an interval of dynamic pressure pulses that did not exist upstream of the bow shock in the pristine solar wind or foreshock and appear consistent with previous simulations of solar wind discontinuities interacting with the bow shock, which predict large amplitude pulses when the local geometry of the shock changes. A statistical study of these structures, however, reveals their predominant origin near the quasi-parallel shock, typically under steady interplanetary magnetic fields, suggestive that the foreshock is important in their generation. The enhanced pressure on the magnetopause due to these pulses can perturb the boundary, exciting ultra-low frequency waves in the magnetosphere and travelling convection vortices in the ionosphere, similar to the response to pressure variations of solar wind origin. However, in this case the response is smoother and on longer timescales than the sharp, impulsive pressure variations and often a collective effect of numerous pulses. Conditions at the magnetopause are often inferred from suitably time lagged measurements of the pristine solar wind taken far upstream of Earth at the L1 Lagrangian point. However, such methods cannot predict the precise locations and times of dynamic pressure pulses in the magnetosheath, which directly drive magnetospheric dynamics.

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Longmore, Melissa Mary. "Cluster multi-spacecraft observations at the Earth's foreshock and a survey of Earth's magnetosheath". Thesis, Queen Mary, University of London, 2005. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.425338.

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Constantinescu, Ovidiu Dragoş. "Wave sources and structures in the Earth's magnetosheath and adjacent regions". Katlenburg-Lindau : Copernicus, 2007. http://d-nb.info/994457952/34.

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Constantinescu, Ovidiu Dragoş [Verfasser]. "Wave sources and structures in the Earth's magnetosheath and adjacent regions / von Ovidiu Dragoş Constantinescu". Katlenburg-Lindau : Copernicus GmbH, 2007. http://d-nb.info/994457952/34.

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g, Ufot Ekong Ufot. "Analysis of low frequency plasma waves in turbulent magnetosheath : downstream of the Earth's bow shock". Thesis, University of Sussex, 2011. http://sro.sussex.ac.uk/id/eprint/6324/.

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The knowledge of the dynamics and characteristics of space plasma during solar-terrestrial coupling has been greatly enriched by process that aids the determination of the instantaneous frequencies which support the non-stationary and non-linear nature of signals. Such plasmas are observed in the magnetosheath in the downstream of bow shock. In this thesis a technique was applied which extracts the various contributing oscillatory modes reflecting the waveforms observed in the space by Cluster spacecraft instruments such as FGM, CIS and EFW, and decompose the frequency of each extracted mode using Instantaneous Frequency method that is based on Simple Hilbert Transform (SHT). This is achieved through the use of Empirical Mode Decomposition (EMD). To eliminate the negative frequency of the various extracted modes referred to as intrinsic mode function which appears with Fourier transform, we apply Hilbert transform leading to analytic representation of the signals. This process aids the determination of the instantaneous frequencies of the extracted modes. The combined process of EMD and Hilbert transform is called the Hilbert-Huang transform. The results in this thesis have been based on the improved EMD. To contribute to the understanding of plasma dynamics, the computed instantaneous frequencies are compared with the results obtained from the application of Simple Hilbert Transform. Instantaneous frequencies of overriding waves are easily separated as opposed to the application of just SHT. They offer the advantage of 3-dimensional study of the spatial characteristics of waves. The understanding of the instantaneous wave number has been achieved through the EMD and SHT combination. This provides the results which give the wave vector for a known frequency at a given instant of time. The instantaneous dispersion relation is determined using the knowledge of the instantaneous frequency and wave vector in the satellite frame, the plasma bulk velocity and the spacecraft velocity (found to be negligible compared with the plasma bulk velocity). This is accomplished using a Doppler shift relation. Wave modes identifications have been carried out by considering the proton temperature anisotropies, plasma beta and plasma bulk velocity and instantaneous phase velocity in the satellite frame. We report Alfvén mode close to the bow shock, spreading out to mirror mode which dominates the middle of magnetosheath. The mirror mode then diminishes towards the magnetopause.

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Wallace, Aletta M. J. (Aletta Margaret Jensen). "Analysis of shock propagation in the magnetosheath". Thesis, Massachusetts Institute of Technology, 2003. http://hdl.handle.net/1721.1/114318.

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Thesis: S.B. in Planetary Science and Astronomy, Massachusetts Institute of Technology, Department of Earth, Atmospheric, and Planetary Sciences, 2003.
Cataloged from PDF version of thesis.
Includes bibliographical references (pages 25-26).
Four interplanetary shock waves and disturbances are analyzed. Data recorded by multiple spacecraft are compared in order to determine how the speed of these events is modified when they cross Earth's bow shock into the magnetosheath. To accomplish this, it was necessary to find shocks that were seen by spacecraft both in the solar wind and inside the magnetosheath. Using a velocity coplanarity and a Rankine-Hugoniot methods of shock normal analysis, the speeds of these events in the solar wind were calculated. The time of their arrival at a spacecraft in the magnetosheath was determined. The predicted arrival time, assuming a constant shock speed from the spacecraft in the solar wind to the spacecraft in the magnetosheath is then compared to the actual arrival time. The resulting data support the conclusion that there is no change in the speed of the shock as it propagates through the magnetosheath.
by Aletta M. J. Wallace.
S.B. in Planetary Science and Astronomy

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Grönlund, Arthur. "Statistical Survey of Earth’s Magnetopause Using MMS Data : Pressure Balance, Total Pressure Contributions and Magnetopause Velocity near the Subsolar Point, Dawn- and Dusk Flanks". Thesis, KTH, Skolan för elektroteknik och datavetenskap (EECS), 2021. http://urn.kb.se/resolve?urn=urn:nbn:se:kth:diva-295200.

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The magnetopause is an important feature in near-Earth space, where the continuously emitted solar wind from the sun meets the magnetic field of the Earth. This boundary region between the so-called magnetosheath on the outside and magnetosphere on the inside is a constantly back-and-forth moving discontinuity upheld by a pressure balance on both sides, upon which an important process in mass and energy transportation through the universe called magnetic reconnection occurs. To gain further understanding about the magnetopause, this study aimed to produce additional statistical scientific material concerning the discontinuity, including the total pressure difference across it, pressure values and total pressure contributions in the magnetosheath and magnetosphere bordering it, and velocity of the magnetopause related to pressure difference. This was done by analysing data from the MMS-project during crossings of the magnetopause in late 2017 and throughout 2018 at the subsolar point and dawn-/dusk flanks. While the results show in general good agreement with previous studies, some intriguing features were noted, including a pressure difference bias towards higher mean total pressures in the magnetosheath in all regions, as well as shift in dominating pressure in the magnetosphere from magnetic pressure at the subsolar point to thermal pressure on the flanks. Further study to confirm these features ought to be conducted. Finally, no clear connection was revealed between magnetopause velocity and pressure imbalance.
Magnetopausen är en viktig struktur i den jordnära rymden, där den ständigt utskickade solvinden från solen möter jordens magnetfält. Detta gränsområde mellan det så kallade magnetosheath på utsidan och magnetosfären på insidan är en diskontinuitet i ständig rörelse fram och tillbaka, upprätthållen av en tryckbalans på båda sidor, på vars yta en mycket viktig process för mass- och energitransport i universum sker kallad magnetisk rekonnektion. För att öka förståelsen för magnetopausen, har denna studie haft som mål att skapa ytterligare statistiskt material gällande diskontinuiteten. Detta inkluderar den totala tryckskillnaden över den, tryckvärden och deras bidrag till det totala trycket i magnetosheath och magnetosfären som gränsar den, samt magnetosfärens hastighet kopplat till tryckskillnaden över den. Detta gjordes genom analys av data från MMS-projektet, specifikt korsningar av magnetopausen i slutet av 2017 och under 2018 vid subsolar point och morgon- /kvällsflankerna. Om än resultaten visar på generellt sätt god överensstämmelse med tidigare studier, noterades en del intressanta resultat. Främst av dessa var en tydlig tendens för högre totalt tryck i magnetosheath jämfört med magnetosfären i alla undersökta regioner, samt ett oväntat skifte av dominerande tryck i magnetosfären från magnetiskt tryck vid subsolar point till termiskt tryck vid flankerna. Fortsatta studier för att bekräfta dessa resultat bör genomföras. Gällande magnetopaushastighet kopplat till tryckskillnad kunde ingen klar koppling ses från resultaten.

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Hadid, Lina. "Observations in-situ de la turbulence compressible dans les magnétogaines planétaires et le vent solaire". Thesis, Université Paris-Saclay (ComUE), 2016. http://www.theses.fr/2016SACLS255/document.

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Parmi les différents plasmas spatiaux, le vent solaire et les magnétogaines planétaires représentent les meilleurs laboratoires pour l’étude des propriétés de la turbulence. Les fluctuations de densité dans le vent solaire étant faibles, à basses fréquences ces dernières sont généralement décrites par la théorie de la MHD incompressible. Malgré son incompressibilité, l’effet de la compressibilité dans le vent solaire a fait l’objet de nombreux travaux depuis des décennies, à la fois théoriques,numériques et observationnels.Le but de ma thèse est d’étudier le rôle de la compressibilité dans les magnétogaines planétaires(de la Terre et de Saturne) en comparaison avec un milieu beaucoup plus étudié et moins compressible (quasi incompressible), le vent solaire. Ce travail a été réalisé en utilisant des données in-situ de trois sondes spatiales, Cassini, Cluster et THEMIS B/ARTEMIS P1.La première partie de mon travail a été consacrée à l’étude des propriétés de la turbulence dans la magnétogaine de Saturne aux échelles MHD et sub-ionique, en comparaison avec celle de la Terre en utilisant les données Cassini et Cluster respectivement. Ensuite j’ai appliqué la loiexacte de la turbulence isotherme et compressible dans le vent rapide et lent en utilisant les données THEMIS B/ARTEMIS P1, afin d’étudier l’effet et le rôle de la compressibilité sur le taux de transfert de l’énergie dans la zone inertielle. Enfin, une première application de ce modèle dans la magnétogaine de la Terre est présentée en utilisant les données Cluster
Among the different astrophysical plasmas, the solar wind and the planetary magnetosheathsrepresent the best laboratories for studying the properties of fully developed plasma turbulence.Because of the relatively weak density fluctuations (∼ 10%) in the solar wind, the low frequencyfluctuations are usually described using the incompressible MHD theory. Nevertheless, the effectof the compressibility (in particular in the fast wind) has been a subject of active research withinthe space physics community over the last three decades.My thesis is essentially dedicated to the study of compressible turbulence in different plasma environments,the planetary magnetosheaths (of Saturn and Earth) and the fast and slow solar wind.This was done using in-situ spacecraft data from the Cassini, Cluster and THEMIS/ARTEMISsatellites.I first investigated the properties of MHD and kinetic scale turbulence in the magnetosheathof Saturn using Cassini data at the MHD scales and compared them to known features of thesolar wind turbulence. This work was completed with a more detailed analysis performed in themagnetosheath of Earth using the Cluster data. Then, by applying the recently derived exactlaw of compressible isothermal MHD turbulence to the in-situ observations from THEMIS andCLUSTER spacecrafts, a detailed study regarding the effect of the compressibility on the energycascade (dissipation) rate in the fast and the slow wind is presented. Several new empirical lawsare obtained, which include the power-law scaling of the energy cascade rate as function of theturbulent Mach number. Eventually, an application of this exact model to a more compressiblemedium, the magnetosheath of Earth, using the Cluster data provides the first estimation of theenergy dissipation rate in the magnetosheath, which is found to be up to two orders of magnitudehigher than that observed in the solar wind

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Jelínek, Karel. "Dynamika okolozemní rázové vlny a magnetopauzy". Doctoral thesis, 2012. http://www.nusl.cz/ntk/nusl-309848.

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viii Title: Dynamics of the bow shock and magnetopause Author: Karel Jelínek Department: Department of Surface and Plasma Science Supervisor: Prof. RNDr. Zdeněk Němeček, DrSc. Department of Surface and Plasma Science e-mail address: zdenek.nemecek@mff.cuni.cz Abstract: The interplanetary space is a unique laboratory which allows us to dis- cover (i) a behavior of the plasma under different conditions, (ii) origin of its insta- bilities, and (iii) its interaction with obstacles such as the Earth's magnetosphere. The present thesis analyzes the outer Earth's magnetosphere. The results are based on the in situ sensing by a variety of the spacecraft (e.g., IMP-8, INTERBALL-1, MAGION-4, Geotail, Cluster-II and Themis). The solar wind curently monitored by the WIND and ACE spacecraft near the La- grange point L1 affects by its dynamic pressure the Earth's magnetic field which acts as a counter-pressure and the boundary where these pressures are balanced is the magnetopause. Due to supersonic solar wind speed, the bow shock forms in front of the magnetopause and a region in between, where plasma flows around an obstacle is named the magnetosheath. The thesis contributes to a deaper understanding of the dependence of magnetopause and bow shock shapes and positions, especially, (1) on the orientation of the inter-...

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Książki na temat "Earth's Magnetosheath"

United States. National Aeronautics and Space Administration., red. Origins of energetic ions in the earth's magnetosheath. [Washington, DC: National Aeronautics and Space Administration, 1994.

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United States. National Aeronautics and Space Administration., red. Origins of energetic ions in the earth's magnetosheath. [Washington, DC: National Aeronautics and Space Administration, 1994.

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United States. National Aeronautics and Space Administration., red. Origins of energetic ions in the Earth's magnetosheath: Final report for contract year 1. Palo Alto, Calif: Lockheed Palo Alto Research Laboratory, 1992.

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L, Grabbe Crockett, i United States. National Aeronautics and Space Administration., red. Towards an MHD theory for the standoff distance of earth's bow shock. [Washington, DC: National Aeronautics and Space Administration, 1997.

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United States. National Aeronautics and Space Administration., red. "Studies of magnetopause structure": Final report for NAGW-1054. [Washington, DC: National Aeronautics and Space Administration, 1991.

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W, Greenstadt Eugene, Coroniti Ferdinand V i United States. National Aeronautics and Space Administration., red. Flank solar wind interaction: Final report July 1991 through June 1994. [Washington, DC]: National Aeronautics and Space Administration, 1994.

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W, Greenstadt Eugene, i United States. National Aeronautics and Space Administration., red. Flank solar wind interaction: Annual report, June 1991 through July 1992. Redondo Beach, CA: TRW Space and Technology Group, Applied Technology Division, 1992.

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Części książek na temat "Earth's Magnetosheath"

Dimmock, A. P., K. Nykyri, A. Osmane, H. Karimabadi i T. I. Pulkkinen. "Dawn-Dusk Asymmetries of the Earth's Dayside Magnetosheath in the Magnetosheath Interplanetary Medium Reference Frame". W Dawn-Dusk Asymmetries in Planetary Plasma Environments, 49–72. Hoboken, NJ, USA: John Wiley & Sons, Inc., 2017. http://dx.doi.org/10.1002/9781119216346.ch5.

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Newell, Patrick T., i Ching-I. Meng. "Magnetosheath injections deep inside the closed LLBL: A review of observations". W Earth's Low-Latitude Boundary Layer, 149–56. Washington, D. C.: American Geophysical Union, 2003. http://dx.doi.org/10.1029/133gm15.

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Denton, Richard E., Brian J. Anderson, Stephen A. Fuselier, S. Peter Gary i Mary K. Hudson. "Ion Anisotropy-driven waves in the Earth's magnetosheath and plasma depletion layer". W Solar System Plasmas in Space and Time, 111–19. Washington, D. C.: American Geophysical Union, 1994. http://dx.doi.org/10.1029/gm084p0111.

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Yamauchi, M., R. Lundin, O. Norberg, I. Sandahl, L. Eliasson i D. Winningham. "Signatures of direct magnetosheath plasma injections onto closed field-line regions based on observations at mid- and low-altitudes". W Earth's Low-Latitude Boundary Layer, 179–88. Washington, D. C.: American Geophysical Union, 2003. http://dx.doi.org/10.1029/133gm18.

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Øieroset, Marit, David L. Mitchell, Tai D. Phan, Robert P. Lin, Dana H. Crider i Mario H. Acuña. "The Magnetic Field Pile-Up and Density Depletion in the Martian Magnetosheath: A Comparison with the Plasma Depletion Layer Upstream of the Earth’s Magnetopause". W Mars’ Magnetism and Its Interaction with the Solar Wind, 185–202. Dordrecht: Springer Netherlands, 2004. http://dx.doi.org/10.1007/978-0-306-48604-3_4.

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GÉNOT, V., E. BUDNIK, C. JACQUEY, I. DANDOURAS i E. LUCEK. "MIRROR MODES OBSERVED WITH CLUSTER IN THE EARTH'S MAGNETOSHEATH: STATISTICAL STUDY AND IMF/SOLAR WIND DEPENDENCE". W Advances in Geosciences, 263–83. World Scientific Publishing Company, 2009. http://dx.doi.org/10.1142/9789812836205_0019.

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Streszczenia konferencji na temat "Earth's Magnetosheath"

Robertson, Ina P., Thomas E. Cravens, Michael R. Collier, David G. Sibeck, Kip D. Kuntz i Steven L. Snowden. "Solar wind charge exchange and Earth's magnetosheath". W SOLAR WIND 13: Proceedings of the Thirteenth International Solar Wind Conference. AIP, 2013. http://dx.doi.org/10.1063/1.4811077.

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Tawfik, A., M. A. Amer, O. M. Shalabiea i M. S. El-Nawawy. "The Periodicity of the Alfven Mode Waves in the Earth’s Magnetosheath". W MODERN TRENDS IN PHYSICS RESEARCH: Second International Conference on Modern Trends in Physics Research MTPR-06. AIP, 2007. http://dx.doi.org/10.1063/1.2711133.

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Lewis, H. R., X. Li, J. LaBelle, T. D. Phan i R. A. Treumann. "Characteristics of the ion pressure tensor in the earth’s magnetosheath: AMPTE/IRM observations". W International conference on plasma physics ICPP 1994. AIP, 1995. http://dx.doi.org/10.1063/1.49000.

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Breneman, A. W., C. A. Cattell, K. Kersten, A. Paradise, S. Schreiner, P. J. Kellogg, K. Goetz i L. B. Wilson. "STEREO and wind observations of intense electron cyclotron harmonic waves at the earths bow shock and inside the magnetosheath". W 2014 XXXIth URSI General Assembly and Scientific Symposium (URSI GASS). IEEE, 2014. http://dx.doi.org/10.1109/ursigass.2014.6929903.

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Raporty organizacyjne na temat "Earth's Magnetosheath"

Chang, S. W., J. D. Scudder, J. F. Fennell, R. Friedel i R. P. Lepping. Energetic Magnetosheath Ions Connected to the Earth's Bow Shock: Possible Source of CEPs. Fort Belvoir, VA: Defense Technical Information Center, grudzień 2001. http://dx.doi.org/10.21236/ada399602.

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

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Streszczenie:

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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