Solar wind flow associated with stream-free sector boundaries at 1 AU

• Published in: Solar physics 1987-01, Vol.111 (2), p.429-437
• Main Author: HANUMATH SASTRI, J
• Format: Article
• Language: English
• Subjects: Astronomy; Earth, ocean, space; Exact sciences and technology; Interplanetary space; Solar system
• ISSN: 0038-0938; 1573-093X
• DOI: 10.1007/BF00148530

The correlations between the plasma characteristics of the solar wind flow in the vicinity ( plus or minus 12 hr) of stream-free sector boundaries near Earth are examined by using the composite data base of interplanetary plasma for the period 1965-1980. The result of Lopez et al. (1986) of an inverse relationship of the proton temperature (T sub(p) ) with the momentum flux density (NV super(2) ) in the low-speed wind at 1 AU is confirmed. The coefficients of lines of best fit to the T sub(p) vs. NV super(2) (as well as T sub(p) vs. V) distribution in the sampler are, however, significantly different from those of the undifferentiated sample of low-speed wind considered by Lopez et al. in that T sub(p) is, in general, lower than expected. Further more, it is found that the proton number density (N) varies as the inverse cube of the flow speed (V), indicating an invariance of the kinetic energy flux density (NV super(3) ) relative to velocity structure in the plasma flow around stream-free boundaries. These average relationships, which are unaffected by interplanetary dynamical processes, are suggested to be due to subsonic addition of momentum and energy to the solar wind flow from the source structures, i.e., coronal streamers.