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Published by way of the yank Geophysical Union as a part of the Geophysical Monograph Series.
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Extra resources for Collisionless Shocks in the Heliosphere: Reviews of Current Research
Great care and sophistication are certainly needed in such analyses, since complex situations may arise. For example, in a "standard" flare-associated event the type II shock and the transient are likely to start or be disrupted close to the flare flash phase; since the type II shock is usually faster than the transient [Gergely, 1984], it will soon be ahead of it and have the appearance of a piston-driven shock. Another serious source of uncertainty is due to the fact that the white light structures or the radio source positions are only seen in projection onto the plane of the sky: for instance, a type II source, although projected inside the transient loops, might well be located outside but in front of the transient.
Such an interaction should occur in a strongly azimuthally structured coronal expansion close to the sun, as low-speed, sub-Alfv•nic solar coronal outflows are expected to extend to several tens of solar radii into the interplanetary medium [Marsch and Richter, 1984a]. Besides, Hada and Kennel  have shown by numerical simulation that slow mode MHD waves can steepen into slow shocks once the total plasma fi and the ratio of the ion to electrontemperature,Ti/Ti, are small in the upstream solar wind.
Stewart, R. , Source heights of meter wavelength bursts of spectral type I and III, Sol. , 50, 437, 1976. Stewart, R. , Coronal magnetic structure near the source region of a type II radio burst, Proc. Astron. Soc. , 3, 157, 1977. Stewart, R. , Transient disturbances of the outer corona, Solar and Interplanetary Dynamics, edited by M. Dryer and E. TandbergoHanssen, $ymp. Int. Astron. Union, 91, 333, 1980a. Stewart, R. , Radio evidence for electron acceleration by transverse shock waves in herringbone type II solar bursts, Proc.