標(biāo)題: Titlebook: Dynamics of the Magnetosphere; Proceedings of the A S.-I. Akasofu Conference proceedings 1980 D. Reidel Publishing Company, Dordrecht, Holl [打印本頁] 作者: Philanthropist 時(shí)間: 2025-3-21 19:57
書目名稱Dynamics of the Magnetosphere影響因子(影響力)
書目名稱Dynamics of the Magnetosphere影響因子(影響力)學(xué)科排名
書目名稱Dynamics of the Magnetosphere網(wǎng)絡(luò)公開度
書目名稱Dynamics of the Magnetosphere網(wǎng)絡(luò)公開度學(xué)科排名
書目名稱Dynamics of the Magnetosphere被引頻次
書目名稱Dynamics of the Magnetosphere被引頻次學(xué)科排名
書目名稱Dynamics of the Magnetosphere年度引用
書目名稱Dynamics of the Magnetosphere年度引用學(xué)科排名
書目名稱Dynamics of the Magnetosphere讀者反饋
書目名稱Dynamics of the Magnetosphere讀者反饋學(xué)科排名
作者: CONE 時(shí)間: 2025-3-21 22:56
Electric Fields and Currents in the Earth’s Magnetospherech . -field is a result of deviation from the normal level of solar wind velocity or density or of either IMF component..A concept of magnetospheric substorms, divided into convection-driven and anticonvectional disturbances, is outlined.作者: painkillers 時(shí)間: 2025-3-22 02:58 作者: MUT 時(shí)間: 2025-3-22 05:38
Searching Your Phone and Using Speech, substorms appear to be associated with an increase of the region of the tail-like field or an increase of magnetospheric stresses and associated increase of magnetopause currents. We suggest the dayside field reconfiguration results from an increase of near-tail magnetopause currents which are connected through the night-side electrojet.作者: largesse 時(shí)間: 2025-3-22 11:38 作者: 總 時(shí)間: 2025-3-22 12:56
Investing in Sales and Marketing Too Earlyto support the view that tearing modes grow to finite amplitudes. Future work will have to determine whether collision-free or collision-dominated (based on microturbulence) processes play the major role.作者: 總 時(shí)間: 2025-3-22 18:54 作者: 雀斑 時(shí)間: 2025-3-22 22:08 作者: MOTTO 時(shí)間: 2025-3-23 05:13
Magnetic Substorm Characteristics Described by Magnetic Potential Maps for 26 – 28 March 1976ll into three categories, morning, evening and midnight, which may occur simultaneously or independently. During recovery of these ten substorms the westward electrojet is always in the morning sector.作者: Gesture 時(shí)間: 2025-3-23 08:22 作者: 影響 時(shí)間: 2025-3-23 10:33
Substorms and Magnetospheric Energy Transfer Processess also pointed out that the major entry of substorm energy into the magnetosphere occurs through the boundaries of the lobes of the magnetotail. This paper is not intended to be a complete theory of the magnetospheric substorm — rather the intention of this paper is to point out directions of research deserving of more attention.作者: MERIT 時(shí)間: 2025-3-23 17:20 作者: ABIDE 時(shí)間: 2025-3-23 20:20 作者: Addictive 時(shí)間: 2025-3-24 01:05
Dynamics of the Magnetospheric Plasmaenergized, and eventually escape. We conclude that the convection picture naturally implies that a significant fraction of plasma-sheet ions come from the ionosphere. The ring-current injection is discussed in terms of observations and recent computer-simulation results.作者: chassis 時(shí)間: 2025-3-24 05:00
The Auroral Electrojetse shall show how their magnetic fields combine to yield the observed magnetic perturbation at the earth’s surface. We shall treat the case of the steady-state electrojet system and we shall also show how it is altered during substorms. Finally, we outline the physical processes through which three-dimensional current systems are generated.作者: 心胸開闊 時(shí)間: 2025-3-24 10:15 作者: gimmick 時(shí)間: 2025-3-24 11:10 作者: Obsessed 時(shí)間: 2025-3-24 15:11
Fabio Claudio Ferracchiati,Emanuele Garofaloenergized, and eventually escape. We conclude that the convection picture naturally implies that a significant fraction of plasma-sheet ions come from the ionosphere. The ring-current injection is discussed in terms of observations and recent computer-simulation results.作者: 迎合 時(shí)間: 2025-3-24 21:44 作者: 圓柱 時(shí)間: 2025-3-25 02:42 作者: 失眠癥 時(shí)間: 2025-3-25 04:55 作者: nautical 時(shí)間: 2025-3-25 08:03 作者: instate 時(shí)間: 2025-3-25 14:10 作者: 女歌星 時(shí)間: 2025-3-25 19:18
Drawing with Vertices and Matriceshe interplanetary magnetic field. “Polar cap” is defined here as the region of open geomagnetic field lines encircled by the auroral oval. The first part of the paper reports the progress in the observation and understanding of polar cap size variations as related to changes of the interplanetary ma作者: Galactogogue 時(shí)間: 2025-3-25 23:10
Windows Phone 7 Game Developments may flow easily between the two regions, and that polar-cap electric fields and currents respond sensitively to variations in the interplanetary magnetic field (IMF). The effects of the solar-magnetospheric x, y, and z components of the IMF have proved to be quite distinct. Strong southward compon作者: 恭維 時(shí)間: 2025-3-26 01:32
Getting Started with Silverlighted associations between IMF changes and variations within the geomagnetic tail. The most firmly established among these was the good correlation between increases in the magnetic field intensity inside the tail lobes and intervals of southward-oriented IMF.作者: 發(fā)酵 時(shí)間: 2025-3-26 04:33
Setting up and Using Facebook and Twittereld, the magnetopause. This paper reviews the possibilities for convective and diffusive transport across the boundary and discusses the dependence of such processes on the orientation of the interplanetary magnetic field. It is first shown that, in the absence of transport processes, the magnetoshe作者: preservative 時(shí)間: 2025-3-26 11:43 作者: Liability 時(shí)間: 2025-3-26 12:50
Searching Your Phone and Using Speechusp movements to be monitored and correlated with substorm activity and interplanetary magnetic field direction. We conclude that any erosion of dayside field is not a direct result of southward turning B.. Instead, the cusp position is intimately related to substorm timing and intensity. Intensific作者: 移動(dòng) 時(shí)間: 2025-3-26 17:01 作者: Agility 時(shí)間: 2025-3-26 22:09
Organizing and Sharing Pictures and Videoscurrents originated far from the earth and that they flowed into and away from the polar atmosphere along the geomagnetic field lines. The existence of such field-aligned or . currents was disputed because it was not possible to unambiguously identify current systems that are field-aligned and those作者: 漸強(qiáng) 時(shí)間: 2025-3-27 04:53 作者: 我怕被刺穿 時(shí)間: 2025-3-27 08:23
Fabio Claudio Ferracchiati,Emanuele Garofaloffects of the two-stream and gradient-drift plasma instabilities. These instabilities require relative streaming of the electrons and ions. Measurements at VHF frequencies have shown that the instabilities generally are excited when the streaming velocity is in excess of 300 to 400 m/s. At UHF frequ作者: aptitude 時(shí)間: 2025-3-27 09:32
User Interface with Expression Blend, The main results of calculations include the well-known patterns of space distribution E. and j. j., based on the satellite measurements (OGO-5,6, TRIAD),etc) and, besides, some essential additions. For example, ionospheric projection of the magnetospheric cleft (of polar cap boundary) or the outer作者: 大量 時(shí)間: 2025-3-27 13:51
https://doi.org/10.1007/978-1-4302-4141-6 from 52 northern hemisphere observatories are used to create magnetic potential contour plots representing so called “equivalent ionospheric current” systems. Contour plots of 10 isolated and storm-time substorms for 26 – 28 March 1976 demonstrate the dynamic behavior of the westward and eastward e作者: 錯(cuò)事 時(shí)間: 2025-3-27 17:46
https://doi.org/10.1007/978-1-4302-4141-6eometries are reviewed. An assessment of their role in collisionless tearing based on analytic theory, computer simulations and experimental evidence, supports the dominant role of lower hybrid waves. The relevance of microturbulence on macroscopic stationary and time dependent models of merging is 作者: 遵循的規(guī)范 時(shí)間: 2025-3-28 00:08 作者: 結(jié)束 時(shí)間: 2025-3-28 04:10
,Options When Consultants Won’t Do, This is in contrast to the widely accepted premise that solar wind energy is accumulated in the magnetosphere and then released by an instability process occurring in the magnetotail. It is shown that much of the plasma sheet behavior associated with auroral substorms can be interpreted in terms of作者: 美食家 時(shí)間: 2025-3-28 08:48 作者: 襲擊 時(shí)間: 2025-3-28 11:02
https://doi.org/10.1007/978-94-009-9519-2Planet; Solar wind; ionosphere; magnetosphere; solar; transport作者: Prophylaxis 時(shí)間: 2025-3-28 18:04 作者: 震驚 時(shí)間: 2025-3-28 21:43
Interplanetary Magnetic Field Changes and the Magnetotailed associations between IMF changes and variations within the geomagnetic tail. The most firmly established among these was the good correlation between increases in the magnetic field intensity inside the tail lobes and intervals of southward-oriented IMF.作者: defendant 時(shí)間: 2025-3-29 00:02 作者: 演講 時(shí)間: 2025-3-29 06:57
Polar Cap Variations and the Interplanetary Magnetic Fieldhe interplanetary magnetic field. “Polar cap” is defined here as the region of open geomagnetic field lines encircled by the auroral oval. The first part of the paper reports the progress in the observation and understanding of polar cap size variations as related to changes of the interplanetary ma作者: uveitis 時(shí)間: 2025-3-29 08:47 作者: Atmosphere 時(shí)間: 2025-3-29 13:33
Interplanetary Magnetic Field Changes and the Magnetotailed associations between IMF changes and variations within the geomagnetic tail. The most firmly established among these was the good correlation between increases in the magnetic field intensity inside the tail lobes and intervals of southward-oriented IMF.作者: Root494 時(shí)間: 2025-3-29 19:19 作者: 冷淡周邊 時(shí)間: 2025-3-29 23:09 作者: Pudendal-Nerve 時(shí)間: 2025-3-30 03:10
Dayside Aurora, A Signature of the Dayside Cusp and its Correlation with Substorm Currentsusp movements to be monitored and correlated with substorm activity and interplanetary magnetic field direction. We conclude that any erosion of dayside field is not a direct result of southward turning B.. Instead, the cusp position is intimately related to substorm timing and intensity. Intensific作者: Mendacious 時(shí)間: 2025-3-30 05:55
Dynamics of the Magnetospheric Plasmasource of plasma-sheet plasma, including magnetopause boundary layers; (2) dynamics of plasma-sheet plasma in the tail; (3) injection of the ring current. We present a general theoretical picture of how particles of ionospheric or solar-wind origin circulate around the magnetospheric system, become 作者: lanugo 時(shí)間: 2025-3-30 09:41 作者: AORTA 時(shí)間: 2025-3-30 13:22
The Auroral Electrojetsosphere. These current systems permit energy imparted to the convective motion of magnetospheric plasma to be dissipated in the ionosphere through the process of Joule heating. In this paper we shall review the various component three-dimensional current systems which relate to the electrojets and w作者: 母豬 時(shí)間: 2025-3-30 19:19
Studies of Currents and Electric Fields in the Auroral Zone Ionosphere using Radar Auroral Backscattffects of the two-stream and gradient-drift plasma instabilities. These instabilities require relative streaming of the electrons and ions. Measurements at VHF frequencies have shown that the instabilities generally are excited when the streaming velocity is in excess of 300 to 400 m/s. At UHF frequ作者: 不要嚴(yán)酷 時(shí)間: 2025-3-31 00:05
Electric Fields and Currents in the Earth’s Magnetosphere The main results of calculations include the well-known patterns of space distribution E. and j. j., based on the satellite measurements (OGO-5,6, TRIAD),etc) and, besides, some essential additions. For example, ionospheric projection of the magnetospheric cleft (of polar cap boundary) or the outer作者: Guaff豪情痛飲 時(shí)間: 2025-3-31 04:35
Magnetic Substorm Characteristics Described by Magnetic Potential Maps for 26 – 28 March 1976 from 52 northern hemisphere observatories are used to create magnetic potential contour plots representing so called “equivalent ionospheric current” systems. Contour plots of 10 isolated and storm-time substorms for 26 – 28 March 1976 demonstrate the dynamic behavior of the westward and eastward e作者: URN 時(shí)間: 2025-3-31 05:14 作者: Foregery 時(shí)間: 2025-3-31 10:06
Macroinstabilities of the Magnetotaille process is an instability of the magnetotail. The stability theory of the tail is summarized and the major predictions are described. It is argued that the spontaneous reconnection (tearing) picture is consistent with observations made in the magnetotail. In particular, it can explain field-align作者: PACT 時(shí)間: 2025-3-31 16:45
Substorms and Magnetospheric Energy Transfer Processes This is in contrast to the widely accepted premise that solar wind energy is accumulated in the magnetosphere and then released by an instability process occurring in the magnetotail. It is shown that much of the plasma sheet behavior associated with auroral substorms can be interpreted in terms of作者: output 時(shí)間: 2025-3-31 19:17
Drawing with Vertices and Matriceson that the process of reconnection is occurring. However, it does not elucidate the physical mechanisms by which such reconnection occurs. The study of the physical processes at the magnetopause and their control by the IMF is actively being investigated on the ISEE mission. Initial results indicat
