A fundamental problem in applying linear tearing instability theory to the rapid processes (particle acceleration, heating) in flares was the characteristically slow rate of reconnection. This problem can be at least partially overcome if the tearin mode nonlinearly evolves to a regime in which the reconnection rate is substantially enhanced, such as that for the Petschek configuration. This possibility was often suggested, and some numerical simulations appear to provide support for such a...
Topics: NASA Technical Reports Server (NTRS), MATHEMATICAL MODELS, REATTACHED FLOW, SOLAR FLARES, TEARING...
The possibility that slow-mode shock compression may produce at least some of the increased brightness observed at the leading edge of coronal mass ejections is investigated. Among the reasons given for the possible existence of slow shocks are the following: (1) transient velocities are often greater than the upstream sound speed but less than the Alfven speed, (2) the presence of a slow shock is consistent with the flat top observed in some transients, and (3) the lateral extension of slow...
Topics: NASA Technical Reports Server (NTRS), CORONAS, CURRENT SHEETS, MAGNETOHYDRODYNAMIC WAVES, SHOCK...
Coronal mass ejections (CMEs) are now recognized as an important component of the large-scale evolution of the solar corona. Some representative observations of CMEs are reviewed with emphasis on more recent results. Recent observations and theory are examined as they relate to the following aspects of CMEs: (1) the role of waves in determining the white-light signature; and (2) the mechanism by which the CME is driven (or launched) into the corona.
Topics: NASA Technical Reports Server (NTRS), ASTRONOMICAL PHOTOGRAPHY, CORONAGRAPHS, SIGNATURE ANALYSIS,...
The overall objective of this research program is to obtain a better understanding of the interaction between the solar wind and the interstellar medium through the use of numerical solutions of the time-dependent magnetohydrodynamic (MHD) equations. The simulated results will be compared with observations where possible and with the results from previous analytic and numerical studies. The primary progress during the first two years has been to develop codes for 2-D models in both spherical...
Topics: NASA Technical Reports Server (NTRS), ASTRONOMICAL MODELS, INTERSTELLAR MATTER,...
Magnetic fields in the quiescent solar corona usually remain connected to photospheric (subcoronal) fields. Since the ratio between the plasma and magnetic pressures satisifies beta somewhat 1 below the corona, the frozen in field in this high inertia region is easily moved about by the continual motion of the photospheric plasma. In the corona, however, beta somewhat 0.1 and magnetic effects dominate. The response of coronal fields to photospheric motion is simulated by subjecting a coronal...
Topics: DTIC Archive, Steinolfson,R S, CALIFORNIA UNIV IRVINE DEPT OF PHYSICS, *MAGNETIC FIELDS, *SOLAR...
The primary objective of this research program is to improve our understanding of the dynamics and energetics of the solar corona both in the quiescent dynamic equilibrium state when coronal structure is dominated by the equatorial streamer belt and in the eruptive state when coronal plasma is ejected into the interplanetary medium. Numerical solutions of the time-dependent magnetohydrodynamic (MHD) equations and comparisons of the computed results with observations form the core of the...
Topics: NASA Technical Reports Server (NTRS), INTERPLANETARY MEDIUM, MAGNETOHYDRODYNAMICS,...
Numerical simulations of the formation and propagation of mass ejection, loop transients in coronal streamers are discussed. The simulations are accomplished with numerical solutions of the single fluid, ideal MHD equations of motion in the meridional plane. The streamer is produced by simulating the relaxation of an initially radial hydrodynamic flow coupled with a dipole magnetic field. The simulated transient then results from an energy release at the base of the streamer. The legs of the...
Topics: NASA Technical Reports Server (NTRS), CORONAL LOOPS, ENERGY TRANSFER, HYDRODYNAMICS,...
The analysis of data recorded by the Voyager 2 spacecraft indicates the presence of large-scale fluctuations in the solar wind ram pressure on the time scale of tens of days. The amplitude of the fluctuations is highly variable but often lies within a factor of 5 to 10 change from an average or mean value of the ram pressure. Since the spacecraft has presumably not encountered the termination shock yet, these fluctuations should eventually interact with the shock and thereby play a role in...
Topics: NASA Technical Reports Server (NTRS), FLOW EQUATIONS, GAS DYNAMICS, HELIOSPHERE, INTERPLANETARY...
The primary objective of this research program is the study of the magnetohydrodynamic (MHD) shocks and nonlinear simple waves produced as a result of the interaction of ejected lower coronal plasma with the ambient corona. The types of shocks and nonlinear simple waves produced for representative coronal conditions and disturbance velocities were determined. The wave system and the interactions between the ejecta and ambient corona were studied using both analytic theory and numerical...
Topics: NASA Technical Reports Server (NTRS), COMPUTERIZED SIMULATION, MAGNETOHYDRODYNAMICS, NUMERICAL...
A theoretical study of the formation of a coronal cavity and its relation to a quiescent prominence is presented. It is argued that the formation of a cavity is initiated by the condensation of plasma which is trapped by the coronal magnetic field in a closed streamer and which then flows down to the chromosphere along the field lines due to lack of stable magnetic support against gravity. The existence of a coronal cavity depends on the coronal magnetic field strength; with low strength, the...
Topics: NASA Technical Reports Server (NTRS), CAVITIES, CHROMOSPHERE, CORONAL HOLES, MAGNETIC FIELDS, SOLAR...
Numerical simulations are performed in the framework of nonlinear two-dimensional magnetohydrodynamics to investigate the influence of mass loading on the solar wind interaction with Venus. The principal physical features of the interaction of the solar wind with the atmosphere of Venus are presented. The formation of the bow shock, the magnetic barrier, and the magnetotail are some typical features of the interaction. The deceleration of the solar wind due to the mass loading near Venus is an...
Topics: NASA Technical Reports Server (NTRS), NUMERICAL ANALYSIS, VENUS (PLANET), SOLAR WIND, PLASMA...
A model is developed for the formation and propagation through the lower corona of the loop-like coronal transients in which mass is ejected from near the solar surface to the outer corona. It is assumed that the initial state for the transient is a coronal streamer. The initial state for the streamer is a polytropic, hydrodynamic solution to the steady-state radial equation of motion coupled with a force-free dipole magnetic field. The numerical solution of the complete time-dependent...
Topics: NASA Technical Reports Server (NTRS), SOLAR ACTIVITY, SOLAR CORONA, SOLAR SIMULATION, STELLAR MASS...
The overall objective of the proposed research was to use numerical solutions of the magnetohydrodynamic (MHD) equations along with comparisons of the computed results with observations to study the following topics: (1) ambient solar wind solutions that extend from the solar surface to 1 astronomical unit (AU), contain closed magnetic structures near the Sun, and are consistent with observed values; (2) magnetic and plasma structures in coronal mass ejections (CMES) as they propagate to the...
Topics: NASA Technical Reports Server (NTRS), SOLAR WIND, MAGNETOHYDRODYNAMICS, NUMERICAL ANALYSIS, CORONAL...
The primary objective of this research program is to improve our understanding of the physical processes occurring in the interaction of the solar wind with Venus. This will be accomplished through the use of numerical solutions of the two- and three-dimensional magnetohydrodynamic (MHD) equations and through comparisons of the computed results with available observations. A large portion of this effort involves the study of processes due to the presence of the magnetic field and the effects of...
Topics: NASA Technical Reports Server (NTRS), INTERPLANETARY MAGNETIC FIELDS, VENUS (PLANET),...
The overall objective of this research program is to obtain a better understanding of the interaction between the solar wind and the interstellar medium through the use of numerical solutions of the time-dependent magnetohydrodynamic (MHD) equations. The simulated results have been compared with observations where possible and with the results from previous analytic and numerical studies. The primary accomplishment of this project has been the development of codes for 2-D models in both...
Topics: NASA Technical Reports Server (NTRS), SOLAR WIND, INTERSTELLAR MATTER, TWO DIMENSIONAL MODELS,...
There have been major advances in the theory of magnetic reconnection and of magnetic instability, with important implications for the observations, as follows: (1) Fast and slow magnetic shock waves are produced by the magnetohydrodynamics of reconnection and are potential particle accelerators. (2) The impulsive bursty regime of reconnection gives a rapid release of magnetic energy in a series of bursts. (3) The radiative tearing mode creates cool filamentary structures in the reconnection...
Topics: NASA Technical Reports Server (NTRS), MAGNETIC DISTURBANCES, MAGNETOHYDRODYNAMIC STABILITY, SOLAR...
