Thematische Bibliographien / Auroral electrons

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Auswahl der wissenschaftlichen Literatur zum Thema „Auroral electrons“

Autor: Grafiati

Veröffentlicht am 5. April 2025

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Zeitschriftenartikel zum Thema "Auroral electrons"

Kozelov, Boris V., und Elena E. Titova. „Conjunction Ground Triangulation of Auroras and Magnetospheric Processes Observed by the Van Allen Probe Satellite near 6 Re“. Universe 9, Nr. 8 (29.07.2023): 353. http://dx.doi.org/10.3390/universe9080353.

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Conjunction observations of auroras with electron distributions and broadband electrostatic fluctuations on Van Allen Probe A satellite in the equatorial region are considered. Using triangulation measurements, the energy spectra of the precipitating electrons in the rayed auroral structures were determined for the 17 March 2015 event. A comparison of the spectra of precipitating electrons in the auroral rays with satellite measurements of electrons in the equatorial region related to the aurora showed their agreement. The concomitance between Van Allen Probe A broadband electric waves and auroral variations measured by the ground-based auroral camera was observed on 17 March 2015. This suggests that broadband electrostatic waves may be responsible for electron precipitation, leading to the formation of rayed structures in the aurora.

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Vichare, Geeta, Ankush Bhaskar, Rahul Rawat, Virendra Yadav, Wageesh Mishra, Dorje Angchuk und Anand Kumar Singh. „Low-latitude Auroras: Insights from 2023 April 23 Solar Storm“. Astrophysical Journal 977, Nr. 2 (01.12.2024): 171. https://doi.org/10.3847/1538-4357/ad8dd3.

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Abstract In 2023 April, a low-latitude aurora observed by the all-sky camera at Hanle, Ladakh, India (33°14’N geographic latitude), generated significant interest. This was the first such aurora recorded from the Indian region in the space era and occurred during a moderate solar storm. This study explores this low-latitude auroral sighting, which happened during the sheath-region passage of an interplanetary coronal mass ejection. We analyze in situ multispacecraft particle measurements and geomagnetic field observations from both ground-based and satellite-based magnetometers. The auroral observations at Hanle coincided with intense substorm activity. Our findings indicate that the aurora did not actually reach India; the equatorward boundary was beyond 50°N geographic latitude. Enhanced electron fluxes with energies below 100 eV were detected at 54°N geographic latitude at about 830 km altitude in the predawn sector (4–5 hr local time). In the midnight sector, the equatorward boundary is estimated to be around 52°N geographic latitude, based on Hanle observations and considering emission altitudes of 600–650 km due to low-energy electrons. Thus, the low-latitude red aurora observed from India resulted from the emissions at higher altitudes due to low-energy electron precipitation in the auroral oval and a slight equatorward expansion of the auroral oval. The low-energy electrons likely originated from the plasma sheet and were precipitated due to enhanced wave–particle interactions from strong magnetosphere compression during high solar wind pressure. This study is crucial in understanding low-latitude auroras in the modern space era.

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Samara, M., R. G. Michell, K. Asamura, M. Hirahara, D. L. Hampton und H. C. Stenbaek-Nielsen. „Ground-based observations of diffuse auroral structures in conjunction with Reimei measurements“. Annales Geophysicae 28, Nr. 3 (26.03.2010): 873–81. http://dx.doi.org/10.5194/angeo-28-873-2010.

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Abstract. We present results from ground-based auroral observations coordinated with the Japanese satellite, Reimei, that took place during the winters of 2006, 2007 and 2008 at Poker Flat, Alaska. Comparable temporal and spatial resolution for the optical and in situ particle data, allowed for investigation of small scale and/or rapidly time-varying auroral structures. Four satellite passes through diffuse auroral structures were identified. The structures within the aurora, whether stationary or time-varying (pulsating aurora), were most closely correlated with the highest energy precipitating electrons measured by these detectors (8 to 12 keV). This relation is found to be consistent across all four examples, revealing that the electron precipitation responsible for these diffuse auroral structures is primarily that of the ≥8 keV electrons.

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Yahnin, A. G., V. A. Sergeev, B. B. Gvozdevsky und S. Vennerstrøm. „Magnetospheric source region of discrete auroras inferred from their relationship with isotropy boundaries of energetic particles“. Annales Geophysicae 15, Nr. 8 (31.08.1997): 943–58. http://dx.doi.org/10.1007/s00585-997-0943-z.

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Abstract. According to observations, the discrete auroral arcs can sometimes be found, either deep inside the auroral oval or at the poleward border of the wide (so-called double) auroral oval, which map to very different regions of the magnetotail. To find common physical conditions for the auroral-arc generation in these magnetotail regions, we study the spatial relationship between the diffuse and discrete auroras and the isotropic boundaries (IBs) of the precipitating energetic particles which can be used to characterise locally the equatorial magnetic field in the tail. From comparison of ground observation of auroral forms with meridional profiles of particle flux measured simultaneously by the low-altitude NOAA satellites above the ground observation region, we found that (1) discrete auroral arcs are always situated polewards from (or very close to) the IB of >30-keV electrons, whereas (2) the IB of the >30-keV protons is often seen inside the diffuse aurora. These relationships hold true for both quiet and active (substorm) conditions in the premidnight-nightside (18-01-h) MLT sector considered. In some events the auroral arcs occupy a wide latitudinal range. The most equatorial of these arcs was found at the poleward edge of the diffuse auroras (but anyway in the vicinity of the electron IB), the most poleward arcs were simultaneously observed on the closed field lines near the polar-cap boundary. These observations disagree with the notion that the discrete aurora originate exclusively in the near-Earth portion of plasma sheet or exclusively on the PSBL field lines. Result (1) may imply a fundamental feature of auroral-arc formation: they originate in the current-sheet regions having very curved and tailward-stretched magnetic field lines.

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Blixt, E. M., M. J. Kosch und J. Semeter. „Relative drift between black aurora and the ionospheric plasma“. Annales Geophysicae 23, Nr. 5 (27.07.2005): 1611–21. http://dx.doi.org/10.5194/angeo-23-1611-2005.

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Abstract. Black auroras are recognized as spatially well-defined regions within uniform diffuse aurora where the optical emission is significantly reduced. Although a well studied phenomenon, there is no generally accepted theory for black auroras. One theory suggests that black regions are formed when energetic magnetospheric electrons no longer have access to the loss cone. If this blocking mechanism drifts with the source electron population in the magnetosphere, black auroras in the ionosphere should drift eastward with a velocity that increases with the energy of the precipitating electrons in the surrounding aurora, since the gradient-B curvature drift is energy dependent. It is the purpose of this paper to test this hypothesis. To do so we have used simultaneous measurements by the European Incoherent Scatter (EISCAT) radar and an auroral TV camera at Tromsø, Norway. We have analyzed 8 periods in which a black aurora occurred frequently to determine their relative drift with respect to the ionospheric plasma. The black aurora was found to drift eastward with a velocity of 1.5–4km/s, which is in accordance with earlier observations. However, one case was found where a black patch was moving westward, this being the first report of such behaviour in the literature. In general, the drift was parallel to the ionospheric flow but at a much higher velocity. This suggests that the generating mechanism is not of ionospheric origin. The characteristic energy of the precipitating electron population was estimated through inversion of E-region plasma density profiles. We show that the drift speed of the black patches increased with the energy of the precipitating electrons in a way consistent with the gradient-B curvature drift, suggesting a magnetospheric mechanism for the black aurora. As expected, a comparison of the drift speeds with a rudimentary dipole field model of the gradient-B curvature drift speed only yields order-of-magnitude agreement, which most likely is due to the nightside disturbed magnetosphere being significantly stretched. Keywords. Auroral ionosphere; MI interaction; Energetic particles, precipitating

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Sergienko, T., I. Sandahl, B. Gustavsson, L. Andersson, U. Brändström und Å. Steen. „A study of fine structure of diffuse aurora with ALIS-FAST measurements“. Annales Geophysicae 26, Nr. 11 (21.10.2008): 3185–95. http://dx.doi.org/10.5194/angeo-26-3185-2008.

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Abstract. We present results of an investigation of the fine structure of the night sector diffuse auroral zone, observed simultaneously with optical instruments (ALIS) from the ground and the FAST electron spectrometer from space 16 February 1997. Both the optical and particle data show that the diffuse auroral zone consisted of two regions. The equatorward part of the diffuse aurora was occupied by a pattern of regular, parallel auroral stripes. The auroral stripes were significantly brighter than the background luminosity, had widths of approximately 5 km and moved southward with a velocity of about 100 m/s. The second region, located between the region with auroral stripes and the discrete auroral arcs to the north, was filled with weak and almost homogeneous luminosity, against which short-lived auroral rays and small patches appeared chaotically. From analysis of the electron differential fluxes corresponding to the different regions of the diffuse aurora and based on existing theories of the scattering process we conclude the following: Strong pitch angle diffusion by electron cyclotron harmonic waves (ECH) of plasma sheet electrons in the energy range from a few hundred eV to 3–4 keV was responsible for the electron precipitation, that produced the background luminosity within the whole diffuse zone. The fine structure, represented by the auroral stripes, was created by precipitation of electrons above 3–4 keV as a result of pitch angle diffusion into the loss cone by whistler mode waves. A so called "internal gravity wave" (Safargaleev and Maltsev, 1986) may explain the formation of the regular spatial pattern formed by the auroral stripes in the equatorward part of the diffuse auroral zone.

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Blomberg, L. G., J. A. Cumnock, I. I. Alexeev, E. S. Belenkaya, S. Yu Bobrovnikov und V. V. Kalegaev. „Transpolar aurora: time evolution, associated convection patterns, and a possible cause“. Annales Geophysicae 23, Nr. 5 (28.07.2005): 1917–30. http://dx.doi.org/10.5194/angeo-23-1917-2005.

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Abstract. We present two event studies illustrating the detailed relationships between plasma convection, field-aligned currents, and polar auroral emissions, as well as illustrating the influence of the Interplanetary Magnetic Field's y-component on theta aurora development. The transpolar arc of the theta aurorae moves across the entire polar region and becomes part of the opposite side of the auroral oval. Electric and magnetic field and precipitating particle data are provided by DMSP, while the POLAR UVI instrument provides measurements of auroral emissions. Ionospheric electrostatic potential patterns are calculated at different times during the evolution of the theta aurora using the KTH model. These model patterns are compared to the convection predicted by mapping the magnetopause electric field to the ionosphere using the Paraboloid Model of the magnetosphere. The model predicts that parallel electric fields are set up along the magnetic field lines projecting to the transpolar aurora. Their possible role in the acceleration of the auroral electrons is discussed. Keywords. Ionosphere (Plasma convection; Polar ionosphere) – Magnetospheric physics (Magnetosphereionosphere interactions)

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Kong, Wanqiu, Zejun Hu, Jiaji Wu, Tan Qu und Gwanggil Jeon. „A Comparative Study of Estimating Auroral Electron Energy from Ground-Based Hyperspectral Imagery and DMSP-SSJ5 Particle Data“. Remote Sensing 12, Nr. 14 (14.07.2020): 2259. http://dx.doi.org/10.3390/rs12142259.

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Aurora, the spectacular phenomenon commonly occurring in high latitudes, is caused by the precipitation of energetic particles penetrating the Earth’s atmosphere. Being the result of solar-terrestrial interactions, electron precipitation significantly contributes to auroral production. To evaluate its magnitude, a physical quantity describing the characteristics of precipitating auroral electrons—their characteristic energy—is adopted. In this paper, this quantity is derived from joint data observed by the ground-based auroral spectroscopic imager located in Antarctica Zhongshan Station and the particle detectors “Special Sensor J5 (SSJ5)” on the Defense Meteorological Satellite Program (DMSP) satellites. A postprocessing scheme of ground-based spectral data is proposed to infer the characteristic energy that successively uses classical brute-force, recursive brute-force and self-consistent approximation strategies for step-up speed improvement. Then, the inferred characteristic energies are compared to the average energies calibrated from the relevant electron data detected by SSJ5 to confirm whether this inference is valid. Regarding DMSP F18/SSJ5, these two energy estimations about auroral electrons deviate slightly from each other and show a strong linear relationship. It sheds light on further applications of the valuable aurora spectral data.

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Lummerzheim, D., und J. Lilensten. „Electron transport and energy degradation in the ionosphere: evaluation of the numerical solution, comparison with laboratory experiments and auroral observations“. Annales Geophysicae 12, Nr. 10/11 (31.08.1994): 1039–51. http://dx.doi.org/10.1007/s00585-994-1039-7.

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Abstract. Auroral electron transport calculations are a critical part of auroral models. We evaluate a numerical solution to the transport and energy degradation problem. The numerical solution is verified by reproducing simplified problems to which analytic solutions exist, internal self-consistency tests, comparison with laboratory experiments of electron beams penetrating a collision chamber, and by comparison with auroral observations, particularly the emission ratio of the N2 second positive to N+2 first negative emissions. Our numerical solutions agree with range measurements in collision chambers. The calculated N22P to N+21N emission ratio is independent of the spectral characteristics of the incident electrons, and agrees with the value observed in aurora. Using different sets of energy loss cross sections and different functions to describe the energy distribution of secondary electrons that emerge from ionization collisions, we discuss the uncertainties of the solutions to the electron transport equation resulting from the uncertainties of these input parameters.

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Milan, S. E., A. Grocott, C. Forsyth, S. M. Imber, P. D. Boakes und B. Hubert. „A superposed epoch analysis of auroral evolution during substorm growth, onset and recovery: open magnetic flux control of substorm intensity“. Annales Geophysicae 27, Nr. 2 (11.02.2009): 659–68. http://dx.doi.org/10.5194/angeo-27-659-2009.

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Abstract. We perform two superposed epoch analyses of the auroral evolution during substorms using the FUV instrument on the Imager for Magnetopause-to-Aurora Global Explorer (IMAGE) spacecraft. The larger of the two studies includes nearly 2000 substorms. We subdivide the substorms by onset latitude, a measure of the open magnetic flux in the magnetosphere, and determine average auroral images before and after substorm onset, for both electron and proton aurora. Our results indicate that substorms are more intense in terms of auroral brightness when the open flux content of the magnetosphere is larger, and that magnetic flux closure is more significant. The increase in auroral brightness at onset is larger for electrons than protons. We also show that there is a dawn-dusk offset in the location of the electron and proton aurora that mirrors the relative locations of the region 1 and region 2 current systems. Superposed epoch analyses of the solar wind, interplanetary magnetic field, and geomagnetic indices for the substorms under study indicate that dayside reconnection is expected to occur at a faster rate prior to low latitude onsets, but also that the ring current is enhanced for these events.

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Dissertationen zum Thema "Auroral electrons"

Schroeder, James William Ryan. „Exploring the Alfvén-wave acceleration of auroral electrons in the laboratory“. Diss., University of Iowa, 2017. https://ir.uiowa.edu/etd/5846.

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Inertial Alfvén waves occur in plasmas where the Alfvén speed is greater than the electron thermal speed and the scale of wave field structure across the background magnetic field is comparable to the electron skin depth. Such waves have an electric field aligned with the background magnetic field that can accelerate electrons. It is likely that electrons are accelerated by inertial Alfvén waves in the auroral magnetosphere and contribute to the generation of auroras. While rocket and satellite measurements show a high level of coincidence between inertial Alfvén waves and auroral activity, definitive measurements of electrons being accelerated by inertial Alfvén waves are lacking. Continued uncertainty stems from the difficulty of making a conclusive interpretation of measurements from spacecraft flying through a complex and transient process. A laboratory experiment can avoid some of the ambiguity contained in spacecraft measurements. Experiments have been performed in the Large Plasma Device (LAPD) at UCLA. Inertial Alfvén waves were produced while simultaneously measuring the suprathermal tails of the electron distribution function. Measurements of the distribution function use resonant absorption of whistler mode waves. During a burst of inertial Alfvén waves, the measured portion of the distribution function oscillates at the Alfvén wave frequency. The phase space response of the electrons is well-described by a linear solution to the Boltzmann equation. Experiments have been repeated using electrostatic and inductive Alfvén wave antennas. The oscillation of the distribution function is described by a purely Alfvénic model when the Alfvén wave is produced by the inductive antenna. However, when the electrostatic antenna is used, measured oscillations of the distribution function are described by a model combining Alfvénic and non-Alfvénic effects. Indications of a nonlinear interaction between electrons and inertial Alfvén waves are present in recent data.

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Hénaff, Gwendal. „Modeling, development, and test of a 3D-printed plasma camera for in-situ measurements in space“. Electronic Thesis or Diss., Institut polytechnique de Paris, 2024. http://www.theses.fr/2024IPPAX139.

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Les principaux phénomènes régissant la dynamique des plasmas spatiaux, que ce soit l'accélération des particules chargées, la reconnection magnétique ou la dissipation turbulente de l'énergie électromagnétique, sont de nature multi-échelle. Afin de comprendre leur rôle dans le fonctionnement du système Soleil-Terre, que ce soit dans le vent solaire, à la magnétopause ou dans la magnétosphère terrestre, il est indispensable de développer une instrumentation à la fois compacte et performante qui permette le déploiement de constellations de satellites. Cependant, les instruments de référence utilisés pour mesurer la distribution en énergie des particules chargées ont un champ de vue limité. L'ajout de systèmes de déflection électrostatique contourne cette limitation avec l'inconvénient d'alourdir ces instruments, de ralentir leur cadence de mesure et finalement de réduire leur performance. La multiplication des capteurs est alors nécessaire pour recouvrir les performances souhaitées, avec un impact sur le dimensionnement des satellites et finalement sur le nombre de satellites pouvant être déployés. La caractérisation des flux de particules chargées pour l'étude de la météorologie de l'espace souffre des mêmes limitations, celle-ci étant réalisée avec des instruments compacts et au champ de vue limité.La première étape de ce projet de recherche a consisté à développer une méthode de conception d'une nouvelle gamme de spectromètres plasmas qui dépassent ces limitations. Les spectromètres étudiés reposent sur une topologie torique innovante, offrant un champ de vue hémisphérique instantané qui évite l'utilisation de déflecteurs électrostatiques. Leur système de détection planaire font d'eux de véritables caméras plasmas. Les méthodes développées ont permis la génération numérique et la caractérisation par simulation d'un large éventail de caméras plasmas avec différentes résolutions angulaires et qui pourraient répondre à ces besoins scientifiques variés.Un modèle d'instrument répondant aux enjeux de météorologie de l'espace à ensuite été conçu avec une gamme en énergie allant jusqu'à 22 keV. Il possède une capacité duale de détection ions/électrons qui évite l'utilisation de capteurs différents pour la mesure des électrons et pour celle des ions. Destiné à être embarqué sur nanosatellite, il présente une masse de 1,8 kg et un diamètre de 19 cm. Un procédé de fabrication par impression 3D, et de fonctionnalisation du matériau imprimé a été défini et mis en œuvre. Un système de conversion ions/électrons utilisant des feuilles de carbone et permettant l'utilisation duale de cette caméra plasma a également été mis au point. Un instrument intégrant l'optique électrostatique et un système de détection dual simplifié a ensuite été testé sous faisceau d'électrons afin d'obtenir des réponses expérimentales précises en énergie et en angle. Les tests sous faisceau ont montré un comportement très proche de la simulation, renforçant ainsi la confiance dans la modélisation numérique. Le fonctionnement du système de conversion a été testé sous faisceau d'électrons et d'ions. L'une des perspectives à court terme de cette thèse est le développement, avec le soutien du CNES, d'un modèle complet de cette caméra plasma afin de rendre possible la démonstration en vol de cet instrument dédié à la météorologie de l'espace
Key phenomena governing the dynamics of space plasmas - including charged particle acceleration, magnetic reconnection and the turbulent dissipation of electromagnetic energy - are multi-scale in nature. In order to understand their role in the Sun-Earth relationship, whether in the solar wind, at the magnetopause or in the Earth's magnetosphere, it is essential to develop instrumentation that is both compact and high-performance, enabling the deployment of satellite constellations. However, the reference instruments used to measure the energy distribution of charged particles have a limited field of view. Adding electrostatic deflection systems circumvents this limitation, with the disadvantage of making these instruments heavier, slowing down their measurement rate, and therefore reducing their performance. In this case, more sensors are needed to achieve the desired performance, impacting satellite size and, ultimately, the number of satellites that can be deployed. The characterization of charged particle fluxes for studying space weather, conducted using compact instruments with a limited field of view, faces the same limitations.The first step in this research project was to develop a method for designing a new range of plasma spectrometers that overcome these limitations. These spectrometers are based on an innovative toroidal topology, offering an instantaneous hemispherical field of view that eliminates the need for electrostatic deflectors. Their planar detection system makes them true plasma cameras. The methods developed have enabled the numerical generation and characterization by simulating a wide range of plasma cameras with different angular resolutions that could meet these various scientific needs.A model instrument was then designed to meet the challenges of space weather applications, with an energy range of up to 22 keV. It features dual ion/electron detection capability, avoiding the need for separate sensors for electron and ion measurements. Intended for nanosatellites, it has a mass of 1.8 kg and a diameter of 19 cm. A 3D-printing manufacturing process and functionalization of the material have been defined and implemented. An ion/electron conversion system using carbon foils, enabling dual use of this plasma camera, has also been developed. An instrument integrating the electrostatic optics and a simplified dual detection system has been tested under an electron beam to obtain precise experimental responses in terms of energy and angle. The beam tests showed behavior very close to the simulation, reinforcing confidence in the numerical modeling. The principle of the conversion system was tested under electron and ion beams. One of the short-term prospects of this thesis is the development, with the support of CNES, of a complete model of this plasma camera, with the aim to demonstrate in orbit the performances of this instrument dedicated to space weather applications

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Ahlberg, Carl Daniel, und Wera Mauritz. „Modeling Far Ultraviolet Auroral Ovals at Ganymede“. Thesis, KTH, Skolan för elektroteknik och datavetenskap (EECS), 2018. http://urn.kb.se/resolve?urn=urn:nbn:se:kth:diva-239382.

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Ganymede, one of Jupiters moons, differs from other moons in the Solar System as it has its own magnetic field. This rare property shapes the morphology on the existing far ultraviolet oxygen auroral ovals on the celestial body in the northern and southern hemisphere created by high energy electrons colliding into the atmosphere.With the help of the Hubble Space Telescope (HST) this phenomenon has been captured and analyzed multiple times during the past 20 years using the on-board Space Telescope Imaging Spectrograph (STIS). The ultimate goal of this project is recreating the far ultraviolet oxygen auroral emissions on Ganymede as a 3D computer model in MATLAB by using the data recovered from HST.The method used to reach this goal was to implement a model with main characteristics of the auroral ovals, project it onto a plane and then use a Cauchy distribution to filter the model. To compare the model with images from HST, a χ2-value was calculated for every pixel in each image. To further improvethe model the Nelder-Mead Simplex optimization method was applied.The project succeeded in such a way that the final model created views of the locations and the appearance of the bright spots that represent the auroral ovals around Ganymede with an accurate result in relation to the given data.

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Werden, Scott H. „Energetic electron precipitation in the aurora as determined by X-ray imaging /“. Thesis, Connect to this title online; UW restricted, 1988. http://hdl.handle.net/1773/6826.

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Chua, Damien Han. „Ionospheric influence on the global characteristics of electron precipitation during auroral substorms /“. Thesis, Connect to this title online; UW restricted, 2002. http://hdl.handle.net/1773/6740.

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Williams, John Denis. „An investigation into pulsating aurora /“. Thesis, Connect to this title online; UW restricted, 2002. http://hdl.handle.net/1773/6820.

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Kopf, Andrew James. „A multi-instrument study of auroral hiss at Saturn“. Diss., University of Iowa, 2010. https://ir.uiowa.edu/etd/692.

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Over the last fifty years, a multitude of spacecraft and rocket experiments have studied plasma wave emissions from Earth's auroral regions. One such emission is auroral hiss, a low-frequency whistler-mode wave that is produced in the auroral zone. Observations from Earth-orbiting spacecraft show that auroral hiss is generated by field-aligned electron beams, with the resulting plasma wave emission propagating along the resonance cone. This propagation results in auroral hiss appearing as a V-shaped funnel when observed on a frequency-time spectrogram. This thesis presents the first comprehensive study of auroral hiss at a planet other than Earth, using the Cassini spacecraft to study auroral hiss at Saturn. NASA's Cassini spacecraft, currently in orbit around Saturn, has allowed for the first opportunity to study this emission in detail at another planet. Since 2006, the Cassini spacecraft has twice been in a series of high inclination orbits, allowing investigation and measurements of Saturnian auroral phenomena. During this time, the Radio and Plasma Wave Science (RPWS) Investigation on Cassini detected low frequency whistler mode emissions propagating upward along the auroral field lines, much like terrestrial auroral hiss. Comparisons of RPWS data with observations from several other Cassini instruments, including the Dual-Technique Magnetometer (MAG), Magnetospheric Imaging Instrument (MIMI), and the Cassini Plasma Spectrometer (CAPS), have revealed a complete picture of this emission at Saturn. Observations from these instruments have been used to make a variety of determinations about auroral hiss at Saturn. RPWS has only observed this emission when Cassini was at high-latitudes, although these observations have shown no preference for local time. Tracking the times this emission has been observed revealed a clear periodicity in the emission. Further study later revealed not one but two rotational modulations, one in each hemisphere, rotating at rates of 813.9 and 800.7 degrees per day in the northern and southern hemispheres, respectively. These rates match with observations of the clock-like Saturn Kilometric Radiation. Study of the field-aligned current structures in the auroral regions revealed a strong upward-directed current in both hemispheres on the lower-latitude side of the auroral hiss emission. Along with correlating particle densities, these observations were used to infer the presence of a high-density plasmasphere at low latitudes, with the series of field-aligned current structures lining up with the outer boundary at L-shell values of around 12-15. Analysis of electron beams observed in conjunction with auroral hiss shows that these beams produce large growth rates for whistler-mode waves propagating along the resonance cone, similar to terrestrial auroral hiss. Analytical calculation of the normalized growth rates of ten electron beam events on Day 291, 2008, yielded a wide range of growth rates, from 0.004 to over 6.85 times the real frequency. The latter, a non-physical result, came from a violation of the weak growth approximation, suggesting there was so much growth that the analytical calculation was not valid in this instance. Numerical calculation using a plasma dispersion-solving code called WHAMP produced a growth rate of about 0.3, a still very large number, suggesting the detected beams may be the source of the observed auroral hiss plasma wave emission.

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Cardoso, Flavia Reis. „Auroral electron precipitating energy during magnetic storms with peculiar long recovery phase features“. Instituto Nacional de Pesquisas Espaciais, 2010. http://urlib.net/sid.inpe.br/mtc-m19/2010/11.06.23.26.

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Aurora, emissões geradas por colisões entre elétrons energéticos e partículas atmosféricas, é frequentemente observada na região polar. Embora muito se sabe sobre a aurora, ainda existem inúmeras questões sem respostas. Por exemplo, não se conhece qual a fonte das partículas energéticas ou por quais processos tais partículas são energizadas. A compreensão do comportamento da aurora é um problema científico importante porque provê informação sobre os processos que ocorrem durante a interação vento solar-magnetosfera. A zona auroral é significantemente afetada por tempestades magnéticas e subtempestades. Ocasionalmente, tempestades magnéticas exibem fase de recuperação longa que pode perdurar por vários dias. Durante tais eventos, os eletrojatos aurorais podem apresentar atividade de longa duração e alta intensidade. Esses eventos são conhecidos como eventos HILDCAA (\textit{High Intensity Long Duration Continuous AE Activity}). A potência injetada na magnetosfera/ionosfera, carregada por precipitação de elétrons, é um importante parâmetro que pode ser estimado pelo instrumento \textit{Ultraviolet Imager} (UVI) a bordo do satélite Polar. Esse instrumento monitora a morfologia espacial e a evolução temporal da aurora na faixa do ultravioleta distante em ambas condições de luz e escuridão. Aplicando as correções necessárias ao instrumento e a remoção de \textit{dayglow}, é possível calcular a energia que chega à zona auroral. Nosso objetivo é obter informação quantitativa sobre a fonte de energia de tempestades magnéticas com longa (LRP) e curta (SRP) fase de recuperação, estimando a quantidade de energia de precipitação depositada. A energia de precipitação foi encontrada altamente variável para eventos LRP. Uma significante entrada de energia durante longas fases de recuperação de tempestades magnéticas implica em fonte de energia adicional para manter a atividade magnética no eletrojato auroral, o qual acredita-se estar relacionado com flutuações de velocidade e do campo magnético do vento solar. Por outro lado, o campo magnético interplanetário IMF permaneceu na direção sul por algum tempo em eventos SRP. Todos os resultados sugerem que os eventos LRP poderiam ser uma consequência de um sistema conduzido pelo vento solar e os eventos SRP seriam associados a processos de descarregamento de energia.
Aurora, light emissions generated by collisions between energetic electrons and atmospheric particles, is often seen in the polar region. Although much is known about the aurora, there are still many questions unanswered. For example, it is not well known what is the source of the energetic particles or by what processes the particles are energized. Understanding the behavior of the aurora is an important scientific problem because it provides information about the processes occurring during the solar wind-magnetosphere interaction. The auroral zone is significantly affected by magnetic storms and substorms. Occasionally, magnetic storms exhibit a long recovery phase which can last for several days. During such events, the auroral electrojet can display high-intensity, long duration activity. These events are known as HILDCAA events (High Intensity Long Duration Continuous AE Activity). The power input to the magnetosphere/ionosphere carried by precipitating electrons is an important parameter which can be estimated by the Ultraviolet Imager (UVI) on board the Polar satellite. This instrument monitors the spatial morphology and temporal evolution of the aurora in the far ultraviolet range in both sunlight and darkness. Applying the necessary instrument corrections and the dayglow removal, it is possible to evaluate the energy coming into the auroral zone. Our goal is to obtain quantitative information about the energy source for magnetic storms with long (LRP) and short (SRP) recovery phases by estimating the amount of precipitation energy input. Precipitation energy has been found highly variable for LRP. A significant energy input during long storm recovery phases implies additional energy source to maintain the magnetic activity in the auroral electrojet which is believed to be related to the fluctuating solar wind magnetic field and velocity. On the other hand, IMF (interplanetary magnetic field) remained southward for a while in SRP events. All the results suggest LRP could be a consequence of a solar wind driven system and SRP would be associated to an energy unloading process.

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Fillingim, Matthew Owen. „Kinetic processes in the plasma sheet observed during auroral activity /“. Thesis, Connect to this title online; UW restricted, 2002. http://hdl.handle.net/1773/6824.

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Wykes, William John. „Enhanced pitch angle diffusion due to stochastic electron-whistler wave-particle interactions“. Thesis, University of Warwick, 2001. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.367162.

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Bücher zum Thema "Auroral electrons"

Calvert, W. Uji lectures on the aurora: A theory of the aurora based upon electron scattering into the loss cone by the cyclotron maser instability. Iowa City, Iowa: W. Calvert, 1997.

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Lazutin, Leonid L. X-Ray Emission of Auroral Electrons and Magnetospheric Dynamics. Herausgegeben von Theodore J. Rosenberg. Berlin, Heidelberg: Springer Berlin Heidelberg, 1986. http://dx.doi.org/10.1007/978-3-642-70398-0.

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United States. National Aeronautics and Space Administration., Hrsg. Comment on "Bremsstrahlung X rays from Jovian auroral electrons". San Antonio, Tex: Southwest Research Institute, 1991.

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1953-, Snyder David B., Jongeward Gary A und United States. National Aeronautics and Space Administration., Hrsg. Auroral interactions with ISSA. [Washington, DC]: National Aeronautics and Space Administration, 1994.

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D, Morgan D., und United States. National Aeronautics and Space Administration., Hrsg. Perpendicular electron heating by absorption of auroral kilometric radiation. [Washington, DC: National Aeronautics and Space Administration, 1994.

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Waite, J. H. The Jovian aurora: Electron or ion precipitation? [Washington, DC?: National Aeronautics and Space Administration, 1988.

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United States. National Aeronautics and Space Administration., Hrsg. A comprehensive analysis of electron conical distributions from multi-satellite databases: Final report. Iowa City, IA: University of Iowa, 1994.

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R, Sharber J., und United States. National Aeronautics and Space Administration., Hrsg. An electron sensor for the Pulsating Aurora 2 (PULSAUR 2) Mission. San Antonio, TX: Southwest Research Institute, 1996.

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H, Waite J., und United States. National Aeronautics and Space Administration., Hrsg. Superthermal electron processes in the upper atmosphere of Uranus: Aurora and electroglow. [Washington, DC?: National Aeronautics and Space Administration, 1988.

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United States. National Aeronautics and Space Administration., Hrsg. A study of the spatial scales of discrete polar auroral arcs. El Segundo, Calif: Aerospace Corp., 1989.

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Buchteile zum Thema "Auroral electrons"

Chaston, C. C. „ULF Waves and Auroral Electrons“. In Magnetospheric ULF Waves: Synthesis and New Directions, 239–57. Washington, D. C.: American Geophysical Union, 2006. http://dx.doi.org/10.1029/169gm16.

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Temerin, M., C. Carlson und J. P. Mcfadden. „The Acceleration of Electrons by Electromagnetic Ion Cyclotron Waves“. In Auroral Plasma Dynamics, 155–61. Washington, D. C.: American Geophysical Union, 2013. http://dx.doi.org/10.1029/gm080p0155.

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Swift, Daniel W. „The Generation of Electric Potentials Responsible for the Acceleration of Auroral Electrons“. In Physics of Auroral Arc Formation, 288–95. Washington, D. C.: American Geophysical Union, 2013. http://dx.doi.org/10.1029/gm025p0288.

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Lazutin, Leonid L. „Auroral Electrons in the Midnight Sector and Magnetospheric Disturbances“. In Physics and Chemistry in Space, 93–154. Berlin, Heidelberg: Springer Berlin Heidelberg, 1986. http://dx.doi.org/10.1007/978-3-642-70398-0_4.

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Watt, C. E. J., und R. Rankin. „Alfvén Wave Acceleration of Auroral Electrons in Warm Magnetospheric Plasma“. In Auroral Phenomenology and Magnetospheric Processes: Earth and Other Planets, 251–60. Washington, D. C.: American Geophysical Union, 2012. http://dx.doi.org/10.1029/2011gm001171.

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Brown, D. G., P. G. Richards, J. L. Horwitz und G. R. Wilson. „Semikinetic simulation of effects of lonization by precipitating auroral electrons on ionospheric plasma transport“. In Cross‐Scale Coupling in Space Plasmas, 97–103. Washington, D. C.: American Geophysical Union, 1995. http://dx.doi.org/10.1029/gm093p0097.

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Nemzek, Robert J. „Diffusion of Echo 7 Electron Beams During Bounce Motion“. In Auroral Plasma Dynamics, 173–81. Washington, D. C.: American Geophysical Union, 2013. http://dx.doi.org/10.1029/gm080p0173.

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Klumpar, D. M. „Statistical Distributions of the Auroral Electron Albedo in the Magnetosphere“. In Auroral Plasma Dynamics, 163–71. Washington, D. C.: American Geophysical Union, 2013. http://dx.doi.org/10.1029/gm080p0163.

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Lysak, Robert L. „Electron and Ion Acceleration by Strong Electrostatic Turbulence“. In Physics of Auroral Arc Formation, 444–50. Washington, D. C.: American Geophysical Union, 2013. http://dx.doi.org/10.1029/gm025p0444.

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Kaneda, Eisuke, Toshifumi Mukai und Kunio Hirao. „Synoptic Features of Auroral System and Corresponding Electron Precipitation Observed by Kyokko“. In Physics of Auroral Arc Formation, 24–30. Washington, D. C.: American Geophysical Union, 2013. http://dx.doi.org/10.1029/gm025p0024.

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Konferenzberichte zum Thema "Auroral electrons"

Dashkevich, Zh V., B. V. Kozelov, A. G. Demekhov, Y. Miyoshi, S. Kasahara, S. Yokota, A. Matsuoka et al. „Evolution of the energetic electron flux observed by ARASE satellite and simultaneous aurora in the case of March 31, 2017, 00-01 UT.“ In Physics of Auroral Phenomena. FRC KSC RAS, 2020. http://dx.doi.org/10.37614/2588-0039.2020.43.022.

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The data of simultaneous observation of the energetic electron flux by ARASE satellite and aurora by ground-based all-sky imager in Murmansk region (Russia) have been analyzed for the time interval 00:00-01:00 UT on March 31, 2017. The energy spectra of middle-energy (7-90 keV) electrons observed by MEPe detectors in and near the loss cone have been used for simulation of the auroral emissions in the atmosphere. The temporal evolution of the simulated emission intensity has been compared with the observed emission in the magnetic field-aligned footprint point for the satellite. It was found that the projection along magnetic field has been distorted by the developing disturbance.

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Wu, Ya-dong, Ya-nan Li und Shi-kui Dong. „Statistical Flux and Energy Deposition of Auroral Electrons“. In Proceedings of the 12th Asia Pacific Physics Conference (APPC12). Journal of the Physical Society of Japan, 2014. http://dx.doi.org/10.7566/jpscp.1.015101.

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Ballatore, Paola. „Relationship Among Pc5 Micropulsations, Auroral Activity and Relativistic Electrons: Preliminary Observations“. In PLASMAS IN THE LABORATORY AND IN THE UNIVERSE: New Insights and New Challenges. AIP, 2004. http://dx.doi.org/10.1063/1.1718449.

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Ashour-Abdalla, Maha, Meng Zhou, Mostafa El-Alaoui, David Schriver, Robert Richard und Raymond Walker. „The acceleration of electrons in the magnetotail and their auroral signatures“. In 2011 XXXth URSI General Assembly and Scientific Symposium. IEEE, 2011. http://dx.doi.org/10.1109/ursigass.2011.6051066.

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Schroeder, J. W. R., G. G. Howes, F. Skiff, C. A. Kletzing, T. A. Carter, S. Vincena und S. Dorfman. „Resonant interactions of Alfvén waves and electrons in the LAPD and the acceleration of auroral electrons“. In 2021 International Conference on Electromagnetics in Advanced Applications (ICEAA). IEEE, 2021. http://dx.doi.org/10.1109/iceaa52647.2021.9539786.

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Tsurutani, B. T., G. S. Lakhina, A. Sen, P. K. Kaw, E. Echer, M. V. Alves, E. da Costa et al. „Interplanetary Alfvén Waves, HILDCAAs, Acceleration of Magnetospheric Relativistic “Killer” Electrons and Auroral Zone Heating“. In 14th International Congress of the Brazilian Geophysical Society & EXPOGEF, Rio de Janeiro, Brazil, 3-6 August 2015. Brazilian Geophysical Society, 2015. http://dx.doi.org/10.1190/sbgf2015-301.

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Cucicov, Dorin. „Mytherrella: an interactive installation hallucinating mythological auroral formations“. In 28th International Symposium on Electronic Art. Paris: Ecole des arts decoratifs - PSL, 2024. http://dx.doi.org/10.69564/isea2023-7-short-cucicov-mytherrella.

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SHORT PAPER. Up until very recently, mythological tales predominated in the explanation of the polar auroras. Today, we understand that the polar lights are a phenomenon brought on by the solar winds' interaction with the magnetosphere of the Earth leading to precipitation of energetic particles on the topside ionised atmosphere. However, for a long time, this phenomenon inspired vibrant trans-border stories with a profound impact on local communities. In our interactive installation, Mytherrella, we aimed to create a dynamic environment in which scientific data and mythological storytelling unearth new imaginaries about the aurora borealis. The generative video integrated in the installation uses a custom real-time StyleGAN algorithm that continuously samples from a model trained on a large set of all-sky auroral images acquired in Kiruna, Sweden. This method enables live interaction with the generated video, producing novel synthetic auroral formations that are unpredictable while remaining within the bounds of the learned features. By combining the dataset with a relatively small number of alternative-style images, the diversity of the generated content is increased, creating a divergent effect that reinforces the mythological narrative. We share the technique of interactive video generation as well as the research process behind the creation of the work.

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Kirillov, A. S., R. Werner und V. Guineva. „The simulation of vibrational populations of electronically excited N2and O2molecules in the middle atmosphere of the Earth during precipitations of high-energetic particles.“ In Physics of Auroral Phenomena. FRC KSC RAS, 2020. http://dx.doi.org/10.37614/2588-0039.2020.43.037.

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We study the electronic kinetics of molecular nitrogen and molecular oxygen in the middle atmosphere of the Earth during precipitations of high-energetic protons and electrons.The role of molecular inelastic collisions in intermolecularelectron energy transfer processes is investigated.It is shown that inelastic molecular collisions influence on vibrational populations of electronically excited molecular oxygen. It is pointed out on very important role of the collisions of N2(A3u+) with O2molecules on the electronic excitation of Herzberg states of molecular oxygenat the altitudes of the middle atmosphere.

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Belakhovsky, Vladimir, Yaqi Jin und Wojciech Miloch. „Impact of the substorms and polar cap patches on GPS radio waves at polar latitudes.“ In Physics of Auroral Phenomena. FRC KSC RAS, 2020. http://dx.doi.org/10.37614/2588-0039.2020.43.020.

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The comparative research of the influence of substrorm precipitation and polar cap patches (PCP) on the GPS signals disturbances in the polar ionosphere was done. For this aim we use the GPS scintillation receivers at Ny-Ålesund, operated by the University of Oslo. The presence of the auroral particle precipitation and polar cap patches was determined by using data from the EISCAT 42m radar on Svalbard. We consider tens of events when the simultaneous EISCAT 42m and GPS data were available. We demonstrate that substorm-associated precipitations can lead to a strong GPS phase (σΦ) scintillations up to ~2 radians which is much stronger than those usually produced by PCPs. At the same PCPs can lead to strong ROT (rate of total electron content) variations. So our observations suggest that the substorms and PCPs, being different types of the high-latitude disturbances, lead to the development of different types and scales of ionospheric irregularities.

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Kleimenova, N. G., J. Manninen, T. Turunen, L. I. Gromova, Yu V. Fedorenko, A. S. Nikitenko und O. M. Lebed. „Unexpected high-frequency “birds”-type VLF emissions.“ In Physics of Auroral Phenomena. FRC KSC RAS, 2020. http://dx.doi.org/10.37614/2588-0039.2020.43.008.

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The new typeof daytime natural VLF whistler mode emissions of the magnetospheric origin was recently found in the VLF observations at Kannuslehto station (L ~ 5.5) in Northern Finland.These VLF events occurred at the frequencies above 4-5 kHzeven up to 15 kHz. Here we present the different spectra of this peculiar daytime high-frequency VLF emissions observed under quiet geomagnetic conditions at auroral latitudes at Kannuslehto (Finland) and Lovozero (Russia) stations. These high-frequency waves cannot be attributed to typical well known VLF chorus and hiss. They became visible on the spectrograms only after the filtering out sferics originating by the lightning discharges and hiding all natural high-frequency signals. After this filtering, it was found a large collection of different natural VLF signals observed as a sequence of right-polarized short (less than 1-2 minutes) patches at frequencies above 4-5 kHz, i.e. at higher frequencythan a half the equatorial electron gyrofrequency at the L-shell of Kannuslehto and Lovozero. These emissions were called “birds” due to their chirped sounds. It was established that the “birds” are typically occur during the daytime only under quiet space weather conditions. But in this time, small magnetic substorms were could be observed in the night sector of the Earth. Here we also show the recently observed series of the “bird-mode” emissions with various bizarre quasi-periodic dynamic spectra, sometimes consisting of two (and even more) frequency bands. The “birds” occur simultaneously at Kannuslehto and Lovozero with similar spectral structure demonstrating their common source. It seems that the “birds” emissions are generated deep inside the magnetosphere at the low L-shells. But the real nature, the generation region and propagation behavior of these VLF emissions remain still unknown. Moreover, nobody can explain how the waves could reach the ground at the auroral latitudes like Kannuslehto and Lovozero as well as which magnetospheric driver could generate this very complicated spectral feature of the emissions.

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Berichte der Organisationen zum Thema "Auroral electrons"

Bounar, K. H., und W. J. McNeil. Persistence of Auroral Electron Flux Events from DMSP/F9 Electron Measurements. Fort Belvoir, VA: Defense Technical Information Center, Januar 1992. http://dx.doi.org/10.21236/ada251241.

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Howes, Gregory. Final Technical Report for DE-SC0014599 Physics of the Aurora: Laboratory Measurements of Electron Acceleration by Inertial Alfven Waves. Office of Scientific and Technical Information (OSTI), Dezember 2023. http://dx.doi.org/10.2172/2251517.

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