Premium
Energies of backstreaming protons in the foreshock
Author(s) -
Greenstadt E. W.
Publication year - 1976
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/gl003i009p00553
Subject(s) - ecliptic , physics , foreshock , solar wind , bow shock (aerodynamics) , proton , geophysics , upstream (networking) , boundary (topology) , magnetosheath , bow wave , geology , computational physics , astrophysics , shock wave , geodesy , seismology , nuclear physics , magnetopause , mechanics , aftershock , plasma , computer network , mathematical analysis , mathematics , computer science
A predicted pattern of energy vs detector location in the cislunar region is displayed for proton guiding‐centers traveling upstream away from the quasi‐parallel bow shock. The pattern is implied by upstream wave boundary properties deduced by Diodato et al . (1976). In the solar ecliptic, protons are estimated to have a minimum of 1.1 times the solar wind bulk energy E SW when the wave boundary is in the early morning sector and a maximum of 8.2 E SW when the boundary is near the predawn flank.