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The relationship between proton temperature and momentum flux density in the solar wind
Author(s) -
Lopez R. E.,
Freeman J. W.,
Roelof E. C.
Publication year - 1986
Publication title -
geophysical research letters
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.007
H-Index - 273
eISSN - 1944-8007
pISSN - 0094-8276
DOI - 10.1029/gl013i007p00640
Subject(s) - solar wind , physics , momentum (technical analysis) , context (archaeology) , flux (metallurgy) , interplanetary spaceflight , proton , plasma , astrophysics , atmospheric sciences , interplanetary medium , atomic physics , nuclear physics , chemistry , geology , paleontology , organic chemistry , finance , economics
The relationship between proton temperature and momentum flux density per unit mass at 1 AU is examined using Helios 1 solar wind data from 1974 to 1980. In high‐speed plasma ( V > 500 km s −1 ) T p increases with increasing n 0 V ², where n 0 and T p are the density and proton temperature at 1 AU and V is the flow speed. In low‐speed plasma ( V < 500 km s −1 ), T p does not increase with increasing n 0 V ², and perhaps tends to decrease slightly. These basic relationships between T p and n 0 V ² are not significantly affected by stream interactions. A qualitative explanation of these results is offered in the context of a solar wind model that includes deposition of momentum and energy extending well outward into the interplanetary medium.