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171.
H. Alfvén 《Space Science Reviews》1963,2(6):862-870
Different models of the magnetosphere are discussed critically. It is pointed out that there is a principal difference between the case when the impinging interplanetary plasma has no initial magnetization, B
0 = 0, (as in the Chapman-Ferraro theory), and the case when the plasma is initially magnetized, B
0 0, even if B
0 is very small.In the former case the plasma remains unmagnetized (like a superconductor) and cannot penetrate into the magnetosphere. Therefore the plasma is separated by a sharp boundary from the magnetosphere, (closed magnetosphere model).In the latter case when the plasma is magnetized (which is more realistic) there is a possibility that field lines run from the earth to infinity (open magnetosphere model). Particles from the interplanetary space may penetrate into the magnetosphere. At the same time there may be a number of discontinuity surfaces of different character, such as the Cahill discontinuity.It is important to make terrella experiments in order to study the complicated phenomena occurring when a magnetized plasma penetrates into a dipole field. 相似文献
172.
Le Contel Olivier Perraut Sylvaine Roux Alain Pellat René 《Space Science Reviews》2001,95(1-2):415-426
For <bi,be, the electron and ion bounce frequencies, the response of a plasma to an externally applied electromagnetic perturbation is nonlocal. This implies, via the quasi-neutrality equation, the development of an electrostatic potential which is constant for a given magnetic field line. In the near equatorial region the corresponding potential electric field is shown to oppose the effect of the induced electric field associated with the externally applied perturbation. Thus the effect of the induced electric field is partially shielded; the total azimuthal electric field (i.e. induced plus potential) tends to be small, which explains why the radial flow velocity is slow during quasi-steady conditions prevailing during the growth phase and after the active phase. The nonlocal response of the plasma also leads to the development of a parallel current that may generate current driven Alfvén (CDA) waves, which mode convert into shear Alfvén (SA) waves. CDA/SA waves are systematically observed at early breakup; they grow very fast and produce a parallel diffusion of electrons. As soon as the diffusion time is shorter than the bounce time (d<b), the nonlocal response vanishes. Thus the shielding disappears, and an enhanced transport is restored at the rate fixed by the induced electric field alone. We show that fast flows effectively occur when CDA waves have enough power to diffuse electrons (over d<b). Electron parallel diffusion also leads to an interruption of the parallel current and therefore to a disruption of the perpendicular current. 相似文献
173.
The Anisotropy Telescopes (ATs) instrument, part of the COSPIN experiment on board Ulysses, measures fluxes and anisotropies of protons in the MeV range. We survey data from this instrument throughout the Ulysses mission, with particular emphasis on solar maximum, when large particle intensities were measured. The only significant fluxes
detected by the ATs during solar minimum are those associated with corotating interaction regions. We focus on events characterised
by very large first-order anisotropies, indicating beam-like streaming along the magnetic field lines, and also on times of
unusually low and constant anisotropies. We describe the parameters associated with these events and put forward possible
physical explanations of the extreme anisotropies observed.
This revised version was published online in August 2006 with corrections to the Cover Date. 相似文献
174.
H. Alfvén D.A. Mendis 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》1983,3(3):95-104
The Voyager 1 and 2 observations of the fine structure of the Saturnian ring system demonstrate the importance of electric forces in controlling the dynamics of fine (charged) dust in the rings. A new theory (“gravito-electrodynamics”) which combines the electric and the gravitational forces on these grains leads to natural explanations of a number of observed ring phenomena. If plasma processes play a significant role in the dynamics of the ring system at the present time, it is difficult to avoid the conclusion that they also played an important and perhaps crucial role at cosmogonic times during the emplacement and subsequent condensation of the initial dusty plasma. We believe that the Saturnian ring system represents a “time-capsule” containing vital clues about the physical processes operating during the early stages of its formation. We will show that both its overall structure as well as its fine structure, as determined by Voyagers 1 and 2, indicate the crucial importance of plasma processes in its formation and subsequent evolution. 相似文献
175.
176.
J.-C. Hénoux 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》1984,4(7):227-237
Recent advances in the study of energy release in Flares are reviewed. Progress has been made in modelling coronal X-ray emission and the chromospheric response to energy imput. These advances are based on theoretical studies and on the comparison of complementary data obtained from spacecraft and ground-based observatories. We first review the modelling of the coronal flare derived from radio, X-ray and XUV observations. Then we summarize results on the chromospheric response to various energy imput. Observations of X-ray continuum intensity and polarization, transition zone lines and chromospheric lines do not show evidence of particle trapping by a turbulent front. Although they might be in agreement with trapping and partial precipitation. White light flares appear to result from energy deposited above the photosphere. They are probably due to electron bombardment. The implication of these results on the primary energy release process are discussed and prospects for new research are presented. 相似文献
177.
178.
E. A. Gurtovenko R. I. Kostik A. Tlamicha R. Zerull Aert Schadee A. Mészáros Y. Néeman R. H. Giese A. T. Sinclair J. Kleczek E. A. Trendelenburg Wolfgang Hillebrandt L. Sehnal W. de Graaff C. Slottje T. Courvisier H. F. van Beek B. Baud C. de Jager J. M. A. Danby B. V. Somov J. Cassinelli F. Verbunt 《Space Science Reviews》1986,44(1-2):177-188
179.
Venus and Mars likely had liquid water bodies on their surface early in the Solar System history. The surfaces of Venus and Mars are presently not a suitable habitat for life, but reservoirs of liquid water remain in the atmosphere of Venus and the subsurface of Mars, and with it also the possibility of microbial life. Microbial organisms may have adapted to live in these ecological niches by the evolutionary force of directional selection. Missions to our neighboring planets should therefore be planned to explore these potentially life-containing refuges and return samples for analysis. Sample return missions should also include ice samples from Mercury and the Moon, which may contain information about the biogenic material that catalyzed the early evolution of life on Earth (or elsewhere). To obtain such information, science-driven exploration is necessary through varying degrees of mission operation autonomy. A hierarchical mission design is envisioned that includes spaceborne (orbital), atmosphere (airborne), surface (mobile such as rover and stationary such as lander or sensor), and subsurface (e.g., ground-penetrating radar, drilling, etc.) agents working in concert to allow for sufficient mission safety and redundancy, to perform extensive and challenging reconnaissance, and to lead to a thorough search for evidence of life and habitability. 相似文献
180.
P. Démoulin J. C. Hénoux B. Schmieder C. H. Mandrini M. G. Rovira B. Somov 《Space Science Reviews》1994,68(1-4):129-130
We present a detailed analysis of the magnetic topology of flaring active region. TheH
kernels are found to be located at the intersection of the separatrices with the chromosphere when the shear, deduced from the fibrils or/and transverse magnetic field direction, is taken into account. We show that the kernels are magnetically connected by field lines passing close to the separator. We confirm, for other flares, previous studies which show that photospheric current concentrations are located at the borders of flare ribbons. Moreover we found two photospheric current concentrations of opposite sign, linked in the corona by field lines which follow separatrices. These give evidence that magnetic energy is released by reconnection processes in solar flares. 相似文献