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Interplanetary stream interfacesAt l AU there is a distinct boundary (the stream interface) at the leading edge of a stream in the solar wind, characterized by an abrupt drop in density, a similar increase in temperature and a small increase in speed. It is suggested that stream interfaces form in the interplanetary medium as a consequence of the non-linear evolution of streams generated by an increase in temperature in the solar envelope. This evolution eventually leads to the formation of a reverse shock behind the interface and a forward shock ahead of it. Two instances in which both a stream interface and a reverse shock had developed at l AU are presented. Examples of flare generated shocks which passed through a stream and were observed near a stream interface are also presented. It is shown that stream interfaces are definitely not the same structures as piston boundaries. It is noted that slow shocks, like stream interfaces, always occur ahead of streams and may develop in the interplanetary medium.
Document ID
19740010374
Acquisition Source
Legacy CDMS
Document Type
Technical Memorandum (TM)
Authors
Burlaga, L. F. (NASA Goddard Space Flight Center Greenbelt, MD, United States)
Date Acquired
September 3, 2013
Publication Date
February 1, 1974
Subject Category
Space Sciences
Report/Patent Number
NASA-TM-X-70601
X-692-74-46
Accession Number
74N18487
Distribution Limits
Public
Copyright
Work of the US Gov. Public Use Permitted.

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