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At least 235 records · Page 13
All sourcesNASA NTRSDOE OSTI
NASA NTRS1999

"Driverless" Shocks in the Interplanetary Medium

Many interplanetary shocks have been detected without an obvious driver behind them. These shocks have been thought to be either blast waves from solar flares or shocks due to sudden increase in solar wind speed caused by interactions between large scale open and closed field lines of the Sun. We investigated this problem using a set of interplanetary shock detected {\it in situ} by the Wind space craft and tracing their solar origins using low frequency radio data obtained by the Wind/WAVES experiment. For each of these "driverless shocks" we could find a unique coronal mass ejections (CME) event observed by the SOHO (Solar and Heliospheric Observatory) coronagraphs. We also found that these CMEs were ejected at large angles from the Sun-Earth line. It appears that the "driverless shocks" are actually driver shocks, but the drivers were not intercepted by the spacecraft. We conclude that the interplanetary shocks are much more extended than the driving CMEs.

Gopalswamy, N.↗
NASA NTRS1987

The bowshock and magnetopause

Results achieved in magnetopause and the bow-shock research during the years 1983-1986 are discussed. The review on bow-shock phenomenona includes work done on the terrestrial bow shock, interplanetary shocks, and bow shocks of other planets, describing research on macroscopic aspects of shocks as well as on the microphysics of quasi-perpendicular and quasi-parallel shocks. In the area of magnetopause research, global aspects of the boundary are first examined. Next, the issues of reconnection and energy transfer through the magnetopause, including viscous and surface-wave phenomena, are considered. Finally, flux-transfer events are discussed in terms of their characteristic magnetic signatures, energetic-particle anisotropies, and distribution with IMF orientations.

Elphic, R. C.↗
NASA NTRS1989

Anisotropy of shock-accelerated ion distributions in interplanetary space

The discrepancy between theory and observation is discussed with regard to the ability of interplanetary shock waves to accelerate a small percentage of the thermal ion population. The major point of departure rests with the spatial dependence of the energetic particle intensity and anisotropy in the region upstream of interplanetary shocks. It is argued that the discrepancy is due to the presence of solar flare particles forming an additional seed population which alters the upstream boundary condition of the energetic population. The resulting anisotropy of the energetic particle distribution several scale lengths upstream of the shock is proportional to the ratio of the streaming of the shock-accelerated population to the density of the solar flare population. This theory is then compared with the results of observed upstream anisotropy and measured particle intensities and anisotropies.

Smith, Charles W.↗
NASA NTRS1983

Ion acceleration at shocks in interplanetary space - A brief review of recent observations

An assessment is presented of recent observations providing insights into the collisionless shock ion acceleration process as it is observed near the earth's bow shock and near interplanetary shocks generated by solar activity, with emphasis on the way in which the ion acceleration process appears to be the same for both types of shocks. The observed differences in energetic particle distributions found near these shocks appear to be related to the seed populations available for acceleration, the shock's extent, radius of curvature, and the angle beween the local shock normal and the magnetic field vector, the time of field line connection to the shock, and possibly the shock Mach number.

Gosling, J. T.↗