Gotowe bibliografie tematyczne / Magnetospheric magnetic field

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Gotowa bibliografia na temat „Magnetospheric magnetic field”

Autor: Grafiati
Data publikacji: 6 września 2023

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Artykuły w czasopismach na temat "Magnetospheric magnetic field"

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Pensionerov, Ivan A., Elena S. Belenkaya, Stanley W. H. Cowley, Igor I. Alexeev, Vladimir V. Kalegaev i David A. Parunakian. "Magnetodisc modelling in Jupiter's magnetosphere using Juno magnetic field data and the paraboloid magnetic field model". Annales Geophysicae 37, nr 1 (5.02.2019): 101–9. http://dx.doi.org/10.5194/angeo-37-101-2019.

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Abstract. One of the main features of Jupiter's magnetosphere is its equatorial magnetodisc, which significantly increases the field strength and size of the magnetosphere. Analysis of Juno measurements of the magnetic field during the first 10 orbits covering the dawn to pre-dawn sector of the magnetosphere (∼03:30–06:00 local time) has allowed us to determine optimal parameters of the magnetodisc using the paraboloid magnetospheric magnetic field model, which employs analytic expressions for the magnetospheric current systems. Specifically, within the model we determine the size of the Jovian magnetodisc and the magnetic field strength at its outer edge.
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Paty, Carol, Chris S. Arridge, Ian J. Cohen, Gina A. DiBraccio, Robert W. Ebert i Abigail M. Rymer. "Ice giant magnetospheres". Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 378, nr 2187 (9.11.2020): 20190480. http://dx.doi.org/10.1098/rsta.2019.0480.

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The ice giant planets provide some of the most interesting natural laboratories for studying the influence of large obliquities, rapid rotation, highly asymmetric magnetic fields and wide-ranging Alfvénic and sonic Mach numbers on magnetospheric processes. The geometries of the solar wind–magnetosphere interaction at the ice giants vary dramatically on diurnal timescales due to the large tilt of the magnetic axis relative to each planet's rotational axis and the apparent off-centred nature of the magnetic field. There is also a seasonal effect on this interaction geometry due to the large obliquity of each planet (especially Uranus). With in situ observations at Uranus and Neptune limited to a single encounter by the Voyager 2 spacecraft, a growing number of analytical and numerical models have been put forward to characterize these unique magnetospheres and test hypotheses related to the magnetic structures and the distribution of plasma observed. Yet many questions regarding magnetospheric structure and dynamics, magnetospheric coupling to the ionosphere and atmosphere, and potential interactions with orbiting satellites remain unanswered. Continuing to study and explore ice giant magnetospheres is important for comparative planetology as they represent critical benchmarks on a broad spectrum of planetary magnetospheric interactions, and provide insight beyond the scope of our own Solar System with implications for exoplanet magnetospheres and magnetic reversals. This article is part of a discussion meeting issue ‘Future exploration of ice giant systems'.
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Alexeev, I. I., i E. S. Belenkaya. "Modeling of the Jovian Magnetosphere". Annales Geophysicae 23, nr 3 (30.03.2005): 809–26. http://dx.doi.org/10.5194/angeo-23-809-2005.

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Abstract. This paper presents a global model of the Jovian magnetosphere which is valid not only in the equatorial plane and near the planet, as most of the existing models are, but also at high latitudes and in the outer regions of the magnetosphere. The model includes the Jovian dipole, magnetodisc, and tail current system. The tail currents are combined with the magnetopause closure currents. All inner magnetospheric magnetic field sources are screened by the magnetopause currents. It guarantees a zero normal magnetic field component for the inner magnetospheric field at the whole magnetopause surface. By changing magnetospheric scale (subsolar distance), the model gives a possibility to study the solar wind influence on the magnetospheric structure and auroral activity. A dependence of the magnetospheric size on the solar wind dynamic pressure psw (proportional to psw-0.23) is obtained. It is a stronger dependence than in the case of the Earth's magnetosphere (psw-1/6). The model of Jupiter's magnetospheric which is presented is a unique one, as it allows one to study the solar wind and interplanetary magnetic field (IMF) effects.
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Kalegaev, Vladimir V., Natalia A. Vlasova, Ilya S. Nazarkov i Sophia A. Melkova. "Magnetospheric access for solar protons during the January 2005 SEP event". Journal of Space Weather and Space Climate 8 (2018): A55. http://dx.doi.org/10.1051/swsc/2018040.

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The early phase of the extraordinary solar energetic particle 20 January, 2005 event having the highest peak flux of any SEP in the past 50 years of protons with energies > 100 MeV is studied. Solar energetic particles (>16 MeV) entry to the Earth’s magnetosphere on January 20, 2005 under northward interplanetary magnetic field conditions is considered based on multi-satellite data analysis and magnetic field simulation. Solar wind parameters and interplanetary magnetic field data, as well as calculations in terms of the A2000 magnetospheric magnetic field model were used to specify conditions in the Earth’s environment corresponding to solar proton event. It was shown that during the early phase of the event energetic particle penetration into the magnetosphere took place in the regions on the magnetopause where the magnetospheric and interplanetary magnetic field vectors are parallel. Complex analysis of the experimental data on particle fluxes in the interplanetary medium (data from ACE spacecraft) and on low-altitude (POES) and geosynchronous (GOES) orbits inside the Earth’s magnetosphere show two regions on the magnetopause responsible for particle access to the magnetosphere: the near equatorial day-side region and open field lines window at the high-latitude magnetospheric boundary. Calculations in terms of A2000 magnetospheric magnetic field model and comparison with SuperDARN images support the link between high-latitude solar energetic particle precipitations and the region at the magnetopause where the magnetospheric field is coupled with northward IMF, allowing solar particles entrance into the magnetosphere and access to the northern polar cap.
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Krtička, J., Z. Mikulášek, P. Kurfürst i M. E. Oksala. "Photometric signatures of corotating magnetospheres of hot stars governed by higher-order magnetic multipoles". Astronomy & Astrophysics 659 (marzec 2022): A37. http://dx.doi.org/10.1051/0004-6361/202141997.

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Context. The light curves of magnetic, chemically peculiar stars typically show periodic variability due to surface spots that in most cases can be modeled by low-order harmonic expansion. However, high-precision satellite photometry reveals tiny complex features in the light curves of some of these stars that are difficult to explain as caused by a surface phenomenon under reasonable assumptions. These features might originate from light extinction in corotating magnetospheric clouds supported by a complex magnetic field dominated by higher-order multipoles. Aims. We aim to understand the photometric signatures of corotating magnetospheres that are governed by higher-order multipoles. Methods. We determined the location of magnetospheric clouds from the minima of the effective potential along the magnetic field lines for different orders of multipoles and their combination. From the derived magnetospheric density distribution, we calculated light curves accounting for absorption and subsequent emission of light. Results. For axisymmetric multipoles, the rigidly rotating magnetosphere model is able to explain the observed tiny features in the light curves only when the higher-order multipoles dominate the magnetic field not only at the stellar surface, but even at the Kepler radius. However, even a relatively weak nonaxisymmetric component leads to warping of equilibrium surfaces. This introduces structures that can explain the tiny features observed in the light curves of chemically peculiar stars. The light emission contributes to the light variability only if a significant fraction of light is absorbed in the magnetosphere.
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Jasinski, Jamie M., Neil Murphy, Xianzhe Jia i James A. Slavin. "Neptune’s Pole-on Magnetosphere: Dayside Reconnection Observations by Voyager 2". Planetary Science Journal 3, nr 4 (1.04.2022): 76. http://dx.doi.org/10.3847/psj/ac5967.

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Abstract The “pole-on” configuration occurs when the polar magnetosphere of a planet is directed into the solar wind velocity vector. Such magnetospheric configurations are unique to the ice giant planets. This means that magnetic reconnection, a process that couples a magnetosphere to the solar wind, will be different at the ice giants when they are pole-on compared to other planets. The only available in situ measurements of a pole-on magnetosphere are from the Neptune flyby by Voyager 2, which we analyze in this paper. We show that dayside magnetopause conditions were conducive to magnetic reconnection. A plasma depletion layer in the magnetosheath adjacent to the magnetopause was observed. Plasma measurements inside the magnetospheric cusp show evidence of multiple reconnection taking place at the magnetopause before the spacecraft crossed the open–closed field line boundary. A possible traveling compression region from a nearby passing flux rope was also observed, providing further supporting evidence that multiple X-line reconnection occurred during the flyby. During a perfectly pole-on configuration, reconnection will not depend on the orientation of the interplanetary magnetic field, as is the case at other planetary magnetospheres. The rate of reconnection will not vary because the area of the dayside magnetopause where antiparallel shears occur will be approximately equal for all interplanetary magnetic field orientations. Therefore, we suggest that rotating into and out of the pole-on configuration will likely drive the “on–off”/“switch-like” dynamics observed in simulations. Consequently, the pole-on configuration is most likely an important rotational phase for driving ice giant magnetospheric dynamics.
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Peymirat, C., i D. Fontaine. "A numerical method to compute Euler potentials for non dipolar magnetic fields". Annales Geophysicae 17, nr 3 (31.03.1999): 328–37. http://dx.doi.org/10.1007/s00585-999-0328-6.

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Abstract. The magnetospheric magnetic field may be conveniently described by two scalar functions (α, β), known as the Euler potentials. They are not uniquely defined, and they may be difficult to derive for configuration more complex than a simple dipole. We propose here a simple numerical method to compute one possible pair (α, β). In magnetospheric regions of closed field lines, α can be chosen as a function of the tube volume of unit magnetic flux. The method can be applied to a wide class of magnetic fields which describe the magnetospheric domain of closed field lines and the conjugated ionosphere. Here, it is used with the T87 Tsyganenko model. The results coincide with the dipolar potentials at close distances from the Earth. At larger distances, they display an increasing distortion with the radial distance (or the invariant latitude in the ionosphere) and the magnetic activity. In the magnetosphere, the contours of α and β are stretched towards the nightside. In the ionosphere, they also extend towards the nightside and present major distortions in a narrow ring at the polar cap boundary, which maps distant boundary layers in the magnetosphere.Key words. Ionosphere (ionosphere-magnetosphere interactions; modeling and forecasting). Magnetospheric physics (plasma convection).
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Zaharia, S., C. Z. Cheng i K. Maezawa. "3-D force-balanced magnetospheric configurations". Annales Geophysicae 22, nr 1 (1.01.2004): 251–65. http://dx.doi.org/10.5194/angeo-22-251-2004.

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Abstract. The knowledge of plasma pressure is essential for many physics applications in the magnetosphere, such as computing magnetospheric currents and deriving mag-netosphere-ionosphere coupling. A thorough knowledge of the 3-D pressure distribution has, however, eluded the community, as most in situ pressure observations are either in the ionosphere or the equatorial region of the magnetosphere. With the assumption of pressure isotropy there have been attempts to obtain the pressure at different locations,by either (a) mapping observed data (e.g. in the ionosphere) along the field lines of an empirical magnetospheric field model, or (b) computing a pressure profile in the equatorial plane (in 2-D) or along the Sun-Earth axis (in 1-D) that is in force balance with the magnetic stresses of an empirical model. However, the pressure distributions obtained through these methods are not in force balance with the empirical magnetic field at all locations. In order to find a global 3-D plasma pressure distribution in force balance with the magnetospheric magnetic field, we have developed the MAG-3-D code that solves the 3-D force balance equation computationally. Our calculation is performed in a flux coordinate system in which the magnetic field is expressed in terms of Euler potentials as . The pressure distribution, , is prescribed in the equatorial plane and is based on satellite measurements. In addition, computational boundary conditions for ψ surfaces are imposed using empirical field models. Our results provide 3-D distributions of magnetic field, plasma pressure, as well as parallel and transverse currents for both quiet-time and disturbed magnetospheric conditions. Key words. Magnetospheric physics (magnetospheric configuration and dynamics; magnetotail; plasma sheet)
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Vaisberg, O. L., L. A. Avanov, T. E. Moore i V. N. Smirnov. "Ion velocity distributions within the LLBL and their possible implication to multiple reconnections". Annales Geophysicae 22, nr 1 (1.01.2004): 213–36. http://dx.doi.org/10.5194/angeo-22-213-2004.

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Abstract. We analyze two LLBL crossings made by the Interball-Tail satellite under a southward or variable magnetosheath magnetic field: one crossing on the flank of the magnetosphere, and another one closer to the subsolar point. Three different types of ion velocity distributions within the LLBL are observed: (a) D-shaped distributions, (b) ion velocity distributions consisting of two counter-streaming components of magnetosheath-type, and (c) distributions with three components, one of which has nearly zero parallel velocity and two counter-streaming components. Only the (a) type fits to the single magnetic flux tube formed by reconnection between the magnetospheric and magnetosheath magnetic fields. We argue that two counter-streaming magnetosheath-like ion components observed by Interball within the LLBL cannot be explained by the reflection of the ions from the magnetic mirror deeper within the magnetosphere. Types (b) and (c) ion velocity distributions would form within spiral magnetic flux tubes consisting of a mixture of alternating segments originating from the magnetosheath and from magnetospheric plasma. The shapes of ion velocity distributions and their evolution with decreasing number density in the LLBL indicate that a significant part of the LLBL is located on magnetic field lines of long spiral flux tube islands at the magnetopause, as has been proposed and found to occur in magnetopause simulations. We consider these observations as evidence for multiple reconnection Χ-lines between magnetosheath and magnetospheric flux tubes. Key words. Magnetospheric physics (magnetopause, cusp and boundary layers; solar wind-magnetosphere interactions)
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Belenkaya, E. S., P. A. Bespalov, S. S. Davydenko i V. V. Kalegaev. "Magnetic field influence on aurorae and the Jovian plasma disk radial structure". Annales Geophysicae 24, nr 3 (19.05.2006): 973–88. http://dx.doi.org/10.5194/angeo-24-973-2006.

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Abstract. The Jovian paraboloid magnetospheric model is applied for the investigation of the planet's auroral emission and plasma disk structure in the middle magnetosphere. Jupiter's auroral emission demonstrates the electrodynamic coupling between the ionosphere and magnetosphere. For comparison of different regions in the ionospheric level and in the magnetosphere, the paraboloid model of the global magnetospheric magnetic field is used. This model provides mapping along highly-conducting magnetic field lines. The paraboloid magnetic field model is also applied for consideration of the stability of the background plasma disk in the rotating Jupiter magnetosphere with respect to the flute perturbations. Model radial distribution of the magnetic field and experimental data on the plasma angular velocity in the middle Jovian magnetosphere are used. A dispersion relation of the plasma perturbations in the case of a perfectly conducting ionosphere is obtained. Analyzing starting conditions of a flute instability in the disk, the "threshold" radial profile of the plasma density is determined. An application of the results obtained to the known data on the Jovian plasma disk is discussed.
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Rozprawy doktorskie na temat "Magnetospheric magnetic field"

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Schwarte, Judith. "Modelling the earth's magnetic field of magnetospheric origin from CHAMP data". [S.l. : s.n.], 2004. http://deposit.ddb.de/cgi-bin/dokserv?idn=971057001.

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Topliss, Stephen Mark. "Particle features at the equatorward edge of the cusp". Thesis, University College London (University of London), 2001. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.342233.

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Patra, Swadesh. "The Contribution of Magnetospheric Currents to Ground Magnetic Perturbation during Geomagnetic Storms". DigitalCommons@USU, 2013. https://digitalcommons.usu.edu/etd/1719.

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A geomagnetic storm is triggered in response to a disturbance in the solar wind. The earth's ring current gets energized during a geomagnetic storm, which leads to a decrease in the horizontal component of the geomagnetic field on the earth's surface. The Disturbance Storm Time (Dst) index, which is a measure of the intensity of the ring current, is calculated by taking the average of this decrease in the horizontal intensity across four low latitude magnetometer stations and removing the quiet time secular variations. The rate of decrease of the Dst index is an indicator of the deenergization of the ring current particles. But there are several issues with the Dst measurement as a proxy of the ring current energy. In particular, the percentage contribution of the tail current effect to the Dst index is still debated. In this work, an effort has been made to separate and quantify the possible contribution of the tail current to the Dst index. The relative contribution for a selected set of storms for which the interplanetary magnetic field turned northward abruptly after the peak in Dst was observed is estimated. The WINDMI model of the nightside magnetosphere is used to investigate the contributions of ring current, magnetotail current, and magnetopause current on the observed two-phase decay of the Dst index. The role of different solar wind magnetosphere coupling functions on the Dst index calculated by the WINDMI model is also investigated. The performance of four other coupling functions in addition to the rectified vBs is evaluated. These coupling functions emphasize different physical mechanisms to explain the energy transfer into the magnetosphere due to solar wind velocity, dynamic pressure, magnetic field, and Mach number. One coupling function is due to Siscoe, another by Borovsky, and two by Newell. The results indicate that for a majority of cases, at most only vx, By, and Bz are needed to sufficiently account for the supply of energy to the ring current and geotail current components that contribute to the Dst index. The capabilities of the WINDMI model to reliably determine the state of the global magnetosphere are improved by employing the the Magnetotail (MT) index as a measurement constraint during large geomagnetic storms. The MT index is used as a proxy for the strength of the magnetotail current in the magnetosphere. The inclusion of the MT index as an optimization constraint in turn increases our confidence that the ring current contribution to the Dst index calculated by the WINDMI model is correct during large geomagnetic storms. To improve the models prediction of AL index, we also modify the ionospheric conductivity and fit to two substorms. The rate of reduction of convection in the magnetotail for some of these storms is numerically simulated by using inner magnetospheric models like the Fok Ring Current (FRC) and the Rice Convection Model along with the global BATSRUS model at the community coordinated modeling center. Model results are compared against magnetometer data by creating movie maps from several low-latitude magnetometer stations. The results indicate the contribution from the tail current to the Dst is important. In addition, the reduction of the cross-tail current during substorm dipolarization is predicted by the measured isotropic boundary locations. Several well known phenomena are identified in the magnetometer movie maps.
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Schwarte, Judith [Verfasser]. "Modelling the earth's magnetic field of magnetospheric origin from CHAMP data / Geoforschungszentrum Potsdam. Von Judith Schwarte". Potsdam : Geoforschungszentrum, 2004. http://d-nb.info/971057001/34.

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Winslow, Reka Moldovan. "Investigation of Mercury's magnetospheric and surface magnetic fields". Thesis, University of British Columbia, 2014. http://hdl.handle.net/2429/50100.

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This thesis is devoted to the study of Mercury’s magnetic field environment, to reveal the nature of the interaction between a weak planetary magnetic field and the interplanetary medium. Due to the lack of orbital spacecraft observations at Mercury prior to the MErcury Surface, Space Environment, GEochemistry, and Ranging (MESSENGER) mission, work in this thesis presents some of the first analysis and interpretation of observations in this unique and dynamic environment. The bow shock and magnetopause define the boundary regions of the planet’s magnetosphere, thereby representing the initial interaction of the planetary field with the solar wind. We established the time-averaged shapes and locations of these boundaries, and investigated their response to the solar wind and interplanetary magnetic field (IMF). We found that the solar wind parameters exert the dominant influence on the boundaries; we thus derived parameterized model shapes for the magnetopause and bow shock with solar wind ram pressure and Alfven Mach number, respectively. The cusp region is where solar wind plasma can gain access to the magnetosphere, and in Mercury’s unique case, the surface. As such, this area is expected to experience higher than average space weathering and be a source for the exosphere. Using magnetic field observations, we mapped the northern cusp’s latitudinal and longitudinal extent, average plasma pressure and observed its variation with the solar wind and IMF. From the derived plasma pressure estimates we calculated the flux of plasma to the surface. Mercury’s internal dipole field is not centered on the planet’s geographic equator but has a significant northward offset. We developed the technique of proton-reflection magnetometry to acquire the first measurements of Mercury’s surface field strength. Proton loss cones are evident in both the northern and southern hemispheres, providing confirmation of persistent proton precipitation to the surface in these regions. We used the size of the loss cones to estimate the surface magnetic field strength, which confirm the offset dipole structure of the planetary field. With additional proton-reflection magnetometry observations, we generated a global proton flux map to Mercury’s surface and searched for regional-scale surface magnetic fields in the northern hemisphere.
Science, Faculty of
Earth, Ocean and Atmospheric Sciences, Department of
Graduate
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Eriksson, Stefan. "Global Magnetospheric Plasma Convection". Doctoral thesis, Stockholm : Tekniska högsk, 2001. http://urn.kb.se/resolve?urn=urn:nbn:se:kth:diva-3230.

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Stetler, Fredrik. "Isolated magnetic field structures in the Saturn magnetosphere". Thesis, KTH, Rymd- och plasmafysik, 2017. http://urn.kb.se/resolve?urn=urn:nbn:se:kth:diva-214821.

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This report’s primary focus is to use the data gathered by the Cassini satellite and analyzeits magnetic field data around Saturn. By looking for isolated changes in magneticfield values locations of potential plasmoids can be determined and examined. Theseso called plasmoids are pockets of higher density plasma ,associated with an increaseor decrease of the magnetic field strength, inside the magnetosheath, which may be importantfor the interaction between the solar wind plasma and the magnetosphere. Thestudy has been made over 7 years, from the beginning of 2010 to the end of 2016. Duringthis period a number of magnetic field structures have been found and documentedin this report, along with analyzing some of their properties such as their width andmagnetic field strength.
Denna rapports primära fokus är att använda data insamlad av Cassini satelliten ochanalysera dess magnetiska fältdata runt Saturnus. Genom att titta efter isolerade förändringari magnetiska fältvärdena går det att lokalisera och examinera potentiella plasmoider.Dessa så kallade plasmoider är fickor med högre densitet av plasma, associerademed en ökning eller minskning av magnetisk fältdata, inne i magnetoskiktet, vilket kanvara viktigt för interaktionen mellan solvindens plasma och magnetosfären. Studien hargjorts över 7 års tid, från början av 2010 till slutet av 2016. Under denna period harett antal magnetiska fältstrukturer hittats och dokumenterats i denna rapport, genom attanalysera några av deras egenskaper så som deras bredd och magnetisk fältstyrka.
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Yuen, Rai. "Pulsar Magnetosphere Revisited: Emission Geometry and the Synthesis of the Vacuum-Dipole and the Rotating-Magnetosphere Models". Thesis, The University of Sydney, 2013. http://hdl.handle.net/2123/10011.

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We reconsider the vacuum-dipole model (VDM) and the corotating-magnetosphere model (CMM) for pulsar electrodynamics. Both the VDM and the CMM are fatally flawed as stand-alone models. The former model is used for deriving certain pulsar parameters, such as the surface magnetic field strength and characteristic age, but it lacks the plasma required to emit the observed radiation. The latter model introduces important concepts, such as the Goldreich-Julian charge density and corotation electric field, which form the basis for more detailed models, but it neglects the inductive electric field. When this field is included, the model is unstable to growth of large-amplitude electric oscillations when subject to a temporal perturbation. Furthermore, the predicted highly-relativistic magnetospheric plasma given by the two models is inconsistent with results obtained from observations with the Double Pulsar system. We therefore propose a way of synthesizing the VDM and the CMM for obliquely rotating pulsars. We first modify the VDM to a "minimal" model by assuming that the parallel component of the inductive electric field is screened by charges. We define a class of synthesized models as a linear combination of a fraction y times the minimal model and 1 - y times the CMM. We suggest that the synthesized model provides a basis for understanding the abrupt changes in the magnetospheres of some pulsars, which can alter their slowing down rates. The synthesized model also implies that the velocity of the magnetospheric plasma depends on y and the position of the emission point, which is determined numerically based on the obliquity and viewing angles for emission heights close to stellar surface in dipolar magnetic field structure. We also explore the field structure by including higher order terms in the ratio of the radius to the light-cylinder radius in the magnetic field and explore the implications of these additional terms.
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Bunting, Robert J. "Development and use of a current wedge modelling method for analysis of multiple onset substorms". Thesis, University of York, 1995. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.338555.

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Dimmock, Andrew. "The study of magnetic and electric field structures at planetary magnetospheres". Thesis, University of Sheffield, 2012. http://etheses.whiterose.ac.uk/2679/.

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Książki na temat "Magnetospheric magnetic field"

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United States. National Aeronautics and Space Administration., red. Magnetospheric substorms and tail dynamics: Final technical report. [Washington, DC: National Aeronautics and Space Administration, 1998.

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Curtis, S. The Magnetospheric Multiscale Mission--: Resolving fundamental processes in space plasmas : report of the NASA Science and Technology Definition Team for the Magnetospheric Multiscale (MMS) Mission. Greenbelt, Md: National Aeronautics and Space Administration, Goddard Space Flight Center, 1999.

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Moore, T. E. The geopause. [Washington, D.C: National Aeronautics and Space Administration, 1995.

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C, Delcourt D., i George C. Marshall Space Flight Center., red. The geopause. Huntsville, Ala: NASA Marshall Space Flight Center, 1995.

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1962-, Ohtani Shin-ichi, i AGU Chapman Conference on Magnetospheric Current Systems (1999 : Kona, Hawaii), red. Magnetospheric current systems. Washington, DC: American Geophysical Union, 2000.

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

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L, Horwitz James, Gallagher D. L i United States. National Aeronautics and Space Administration., red. Convection of plasmaspheric plasma into the outer magnetosphere and boundary layer region: Initial results. [Washington, D.C: National Aeronautics and Space Administration, 1998.

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The magnetic universe: The elusive traces of an invisible force. Baltimore: Johns Hopkins University Press, 2009.

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United States. National Aeronautics and Space Administration., red. [Data acquisition and analysis: Solar vector magnetosphere : final report, Aug. - Dec. 1991. Huntsville, Ala: University of Alabama in Huntsville, 1992.

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Verő, József. Hullámok a bolygóközi térből, vagy csak a magnetoszférából?: A geomágneses pulzációk eredete : Akadémiai székfoglaló 1996. október. Budapest: Akadémiai Kiadó, 1999.

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Części książek na temat "Magnetospheric magnetic field"

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Milan, S. E., L. B. N. Clausen, J. C. Coxon, J. A. Carter, M. T. Walach, K. Laundal, N. Østgaard i in. "Overview of Solar Wind–Magnetosphere–Ionosphere–Atmosphere Coupling and the Generation of Magnetospheric Currents". W Earth's Magnetic Field, 555–81. Dordrecht: Springer Netherlands, 2017. http://dx.doi.org/10.1007/978-94-024-1225-3_19.

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Olson, W. P., K. A. Pfitzer i G. J. Mroz. "Modeling the Magnetospheric Magnetic Field". W Quantitative Modeling of Magnetospheric Processes, 77–85. Washington, D. C.: American Geophysical Union, 2013. http://dx.doi.org/10.1029/gm021p0077.

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Lühr, Hermann, Chao Xiong, Nils Olsen i Guan Le. "Near-Earth Magnetic Field Effects of Large-Scale Magnetospheric Currents". W Earth's Magnetic Field, 529–53. Dordrecht: Springer Netherlands, 2017. http://dx.doi.org/10.1007/978-94-024-1225-3_18.

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Finlay, C. C., V. Lesur, E. Thébault, F. Vervelidou, A. Morschhauser i R. Shore. "Challenges Handling Magnetospheric and Ionospheric Signals in Internal Geomagnetic Field Modelling". W Earth's Magnetic Field, 161–93. Dordrecht: Springer Netherlands, 2017. http://dx.doi.org/10.1007/978-94-024-1225-3_7.

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Koskinen, Hannu E. J., i Emilia K. J. Kilpua. "Radiation Belts and Their Environment". W Astronomy and Astrophysics Library, 1–25. Cham: Springer International Publishing, 2021. http://dx.doi.org/10.1007/978-3-030-82167-8_1.

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AbstractThe Van Allen radiation belts of high-energy electrons and ions, mostly protons, are embedded in the Earth’s inner magnetosphere where the geomagnetic field is close to that of a magnetic dipole. Understanding of the belts requires a thorough knowledge of the inner magnetosphere and its dynamics, the coupling of the solar wind to the magnetosphere, and wave–particle interactions in different temporal and spatial scales. In this introductory chapter we briefly describe the basic structure of the inner magnetosphere, its different plasma regions and the basics of magnetospheric activity.
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Nagai, Tsugunobu. "An Empirical Model of Substorm-Related Magnetic Field Variations at Synchronous Orbit". W Magnetospheric Substorms, 91–95. Washington, D. C.: American Geophysical Union, 2013. http://dx.doi.org/10.1029/gm064p0091.

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Olsen, Nils, i Claudia Stolle. "Magnetic Signatures of Ionospheric and Magnetospheric Current Systems During Geomagnetic Quiet Conditions—An Overview". W Earth's Magnetic Field, 7–27. Dordrecht: Springer Netherlands, 2017. http://dx.doi.org/10.1007/978-94-024-1225-3_2.

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Mcpherron, Robert L. "The Synchronous Orbit Magnetic Field Data Set". W Quantitative Modeling of Magnetospheric Processes, 35–47. Washington, D. C.: American Geophysical Union, 2013. http://dx.doi.org/10.1029/gm021p0035.

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Jacquey, Christian. "Substorm associated tail current changes inferred from lobe magnetic field observations". W Magnetospheric Current Systems, 275–83. Washington, D. C.: American Geophysical Union, 2000. http://dx.doi.org/10.1029/gm118p0275.

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Horbury, T. S., A. Balogh, M. W. Dunlop, P. J. Cargill, E. A. Lucek, T. Oddy, P. Brown, C. Carr, K. H. Fornaçon i E. Georgescu. "Cluster magnetic field observations of magnetospheric boundaries". W Earth's Low-Latitude Boundary Layer, 63–69. Washington, D. C.: American Geophysical Union, 2003. http://dx.doi.org/10.1029/133gm06.

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Streszczenia konferencji na temat "Magnetospheric magnetic field"

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Vellante, M., M. Piersanti, B. Heilig, J. Reda i A. Del Corpo. "Magnetospheric plasma density inferred from field line resonances: Effects of using different magnetic field models". W 2014 XXXIth URSI General Assembly and Scientific Symposium (URSI GASS). IEEE, 2014. http://dx.doi.org/10.1109/ursigass.2014.6929941.

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Chamati, Maria. "CHARACTERISTICS OF Pc5 PULSATIONS ACTIVITY AT MID LATITUDES DURING DECEMBER 2019". W 22nd SGEM International Multidisciplinary Scientific GeoConference 2022. STEF92 Technology, 2022. http://dx.doi.org/10.5593/sgem2022/1.1/s05.059.

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Magnetospheric pulsations and the mechanisms underlying their generation are topics under active studies. The Pc5 (f =1.7�6.7 mHz) geomagnetic continuous pulsations, recorded at mid latitudes (L =1.6) during December 2019, with a low level of geomagnetic activity, are analyzed and discussed in this paper. The data sets of the series on geomagnetic field variations recorded at Panagjuriste Geomagnetic Observatory in Bulgaria are analyzed. The spectral characteristics of the pulsations were determined by Continuous Wavelet Analysis (CWT). It is demonstrated that Pc5 pulsation activity appears with all ranges of periods (140-600s) on December 6, 8, and 18, 2019, at time intervals of 02-17 UTC, 14-20 UTC, and 00-16 UTC, respectively. Then, the solar wind (SW) plasma speed, the flow dynamic pressure, and the geomagnetic index Kp are computed for every case of recorded Pc5 pulsations. It is suggested that recorded continuous pulsations in the Pc5 range are due to step-like or sudden increases in solar wind oscillations and variations of the flow dynamic pressure, which precede the appearance of pulsations and drive compressional magnetic field variations in the magnetosphere.
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Chamati, Maria, i Borislav Andonov. "Pc5 PULSATIONS OBSERVED DURING THE GEOMAGNETIC STORM ON 12 MAY 2021". W 22nd SGEM International Multidisciplinary Scientific GeoConference 2022. STEF92 Technology, 2022. http://dx.doi.org/10.5593/sgem2022/1.1/s05.063.

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The study of ultra-low frequency (ULF) waves and geomagnetic pulsations plays an important role in better understanding the mechanisms of their generation and spread in the magnetosphere and on the ground. The magnetospheric ULF waves, which provide useful information about the conditions in the solar wind and in the magnetosphere, can be detected on the ground by different types of magnetometers and recorded as geomagnetic pulsations � continuous and irregular. This paper aims to study the characteristics of Pc5 geomagnetic continuous pulsations recorded at mid latitudes during the strong geomagnetic storm (Kp =7) that occurred on May 12, 2021. The sets of time series of data at sampling period 1s, recorded along the three geomagnetic directions (X, Y and Z), are shown and analyzed. A spectral analysis, based on the Morlet Wavelet transform, is applied. It shows powerful geomagnetic disturbances in the Pc5 band (1.7-6.7 mHz) in two-time intervals: 00-02 UTC- before the beginning of the storm and 10-15 UTC- during the storm. Furthermore, the Fast Fourier Transform (FFT) band pass filter is applied to the data series, and Pc5 pulsations are shown. It was concluded that their emergence was correlated with the dynamics of changes in the interplanetary magnetic field (IMF) Bz component, solar wind plasma speed, and flow dynamic pressure.
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Melrose, Don. "Oscillating pair creation in pulsar magnetospheres". W MAGNETIC FIELDS IN THE UNIVERSE: From Laboratory and Stars to Primordial Structures. AIP, 2005. http://dx.doi.org/10.1063/1.2077191.

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

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CINEMA (CubeSat for Ions, Neutrals, Electrons and MAgneticfields) will image energetic neutral atoms (ENAs) in the magnetosphere, and make measurements of electrons, ions, and magnetic fields at high latitudes. To satisfy the mission requirements, the three unit cubesat was designed. The spin axis needs to be in the ecliptic normal and the spin rate needs to be 4 rpm. The only power source for CINEMA is the solar panels. External torques are generated by an orthogonal pair of coils acting with the earths magnetic field. This paper provides the control strategy, given the limited power and available sensors, to optimize the convergence of the spin and attitude control.
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Asimopolos, Laurentiu, Natalia-Silvia Asimopolos i Adrian-Aristide Asimopolos. "COMPARATIVE AND SPECTRAL STUDIES BETWEEN GEOMAGNETIC SERIES RECORDED IN INTERMAGNET OBSERVATORIES". W 22nd SGEM International Multidisciplinary Scientific GeoConference 2022. STEF92 Technology, 2022. http://dx.doi.org/10.5593/sgem2022/6.1/s28.36.

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The main objectives of this study are: analysis of the associated spectrum of the geomagnetic field, time of occurrence of geomagnetic storms and comparisons between recordings made at various geomagnetic observatories in the INTERMAGNET network, in terms of frequency intensity identified and correlations during geomagnetic disturbances. A geomagnetic storm is a temporary disturbance of the Earth's magnetosphere caused by ejections of solar corona mass, coronal holes or solar flares. The data used in this paper are recorded from the Surlari Observatory, and additional information for the characterization of the analyzed geomagnetic storms, we obtained from specialized sites such as www.intermagnet.org and www.noaa.gov. The information about the geomagnetic data from other observatories, as well as about the planetary physical parameters allowed us to make comparative studies between the data recorded in different observatories. We used and calculated filtered data, spectral analysis, wavelet algorithms with different mathematical functions at different levels, the variation of the correlation coefficients for the magnetic components recorded at different latitudes and longitudes.
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Ma, Qianli, Wen Li i Xiao-Jia Zhang. "Modeling Electron Scattering and Acceleration by Whistler Mode Chorus Waves in Jupiter's Magnetosphere: Effects of Magnetic Field Model, Total Electron Density, and Electron Injections". W 2021 XXXIVth General Assembly and Scientific Symposium of the International Union of Radio Science (URSI GASS). IEEE, 2021. http://dx.doi.org/10.23919/ursigass51995.2021.9560536.

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Raporty organizacyjne na temat "Magnetospheric magnetic field"

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

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The auroral activity indices AU, AL, AE, introduced into geophysics at the beginning of the space era, although they have certain drawbacks, are still widely used to monitor geomagnetic activity at high latitudes. The AU index reflects the intensity of the eastern electric jet, while the AL index is determined by the intensity of the western electric jet. There are many regression relationships linking the indices of magnetic activity with a wide range of phenomena observed in the Earth's magnetosphere and atmosphere. These relationships determine the importance of monitoring and predicting geomagnetic activity for research in various areas of solar-terrestrial physics. The most dramatic phenomena in the magnetosphere and high-latitude ionosphere occur during periods of magnetospheric substorms, a sensitive indicator of which is the time variation and value of the AL index. Currently, AL index forecasting is carried out by various methods using both dynamic systems and artificial intelligence. Forecasting is based on the close relationship between the state of the magnetosphere and the parameters of the solar wind and the interplanetary magnetic field (IMF). This application proposes an algorithm for describing the process of substorm formation using an instrument in the form of an Elman-type ANN by reconstructing the AL index using the dynamics of the new integral parameter we introduced. The use of an integral parameter at the input of the ANN makes it possible to simulate the structure and intellectual properties of the biological nervous system, since in this way an additional realization of the memory of the prehistory of the modeled process is provided.
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Huang, Tian-Sen, Philippe Le-Sager i Yuri V. Petrov. Proposal Coupling of Earth's Magnetosphere and Ionosphere in a Realistic Magnetic Field. Fort Belvoir, VA: Defense Technical Information Center, maj 2000. http://dx.doi.org/10.21236/ada387201.

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Van Allen, James A. Energetic Particles and Magnetic Fields in the Earth's Magnetosphere and Interplanetary Space. Fort Belvoir, VA: Defense Technical Information Center, wrzesień 1997. http://dx.doi.org/10.21236/ada628212.

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Lee, L. C., i S. I. Akasofu. [A study of the magnetic field annihilation process in the magnetosphere and some geotechnical applications]. Office of Scientific and Technical Information (OSTI), styczeń 1993. http://dx.doi.org/10.2172/6873123.

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Lee, L. C., i S. L. Akasofu. [A study of the magnetic field annihilation process in the magnetosphere and some geotechnical applications]. Office of Scientific and Technical Information (OSTI), styczeń 1993. http://dx.doi.org/10.2172/6610443.

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Lee, L. C., i S. L. Akasofu. [A study of the magnetic field annihilation process in the magnetosphere and some geotechnical applications]. Progress report. Office of Scientific and Technical Information (OSTI), maj 1993. http://dx.doi.org/10.2172/10147941.

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Lee, L. C., i S. I. Akasofu. [A study of the magnetic field annihilation process in the magnetosphere and some geotechnical applications]. Progress report. Office of Scientific and Technical Information (OSTI), maj 1993. http://dx.doi.org/10.2172/10147946.

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[A study of the magnetic field annihilation process in the magnetosphere and some geotechnical applications]. Office of Scientific and Technical Information (OSTI), styczeń 1993. http://dx.doi.org/10.2172/6584414.

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[A study of the magnetic field annihilation process in the magnetosphere and some geotechnical applications]. Office of Scientific and Technical Information (OSTI), styczeń 1993. http://dx.doi.org/10.2172/6610452.

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