skip to main content
OSTI.GOV title logo U.S. Department of Energy
Office of Scientific and Technical Information

Title: Entry of solar wind particles into Earth's magnetosphere

Abstract

Entry of solar wind particles into Earth's magnetosphere is studied. Particles can move directly across an open'' magnetopause layer, where the magnetic field has a nonzero normal component ({ital B}{sub {ital n}}{ne}0). Under the assumption that the Walen relation holds near the open magnetopause, the solar wind particle influx can be expressed as {ital F}{sub {ital n}}={ital {bar n}}{sup 1/2}{psi}{sub {ital B}}/({mu}{sub 0}{ital m{sub i}}){sup 1/2}, where {ital {bar n}} is the average particle number density, {psi}{sub {ital B}} is the open magnetic flux at the magnetopause, {mu}{sub 0} is the permeability of free space, and {ital m}{sub {ital i}} is the ion mass. The total particle flux from the solar wind to the entire magnetosphere for a moderate negative value of IMF {ital B}{sub {ital z}} is estimated to be {similar to}7.0{times}10{sup 28} s{sup {minus}1}, although most of the particles leave from the antisolar end of the tail without being trapped. The peak flux through the dayside magnetopause is {similar to}1.1{times}10{sup 27} s{sup {minus}1}, while the peak flux through the near-Earth tail magnetopause ({vert bar} {ital x} {vert bar}{le}30{ital R}{sub {ital E}}) is {similar to}3.0{times}10{sup 27} s{sup {minus}1}. The average particle flux through the dayside and tail magnetopause inmore » the region with {vert bar} {ital x} {vert bar}{le}200{ital R}{sub {ital E}} is found to be {similar to}7.9{times}10{sup 27} s{sup {minus}1}, which is comparable to the tailward particle flux ({similar to}7.1{times}10{sup 27} s{sup {minus}1}) observed at {vert bar} {ital x} {vert bar}{approx equal}200--220{ital R}{sub {ital E}} in the distance tail.« less

Authors:
;  [1]
  1. Geophysical Institute and Department of Physics, University of Alaska-Fairbanks (US)
Publication Date:
OSTI Identifier:
5219741
Resource Type:
Journal Article
Journal Name:
Journal of Geophysical Research; (USA)
Additional Journal Information:
Journal Volume: 94:A9; Journal ID: ISSN 0148-0227
Country of Publication:
United States
Language:
English
Subject:
71 CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS; EARTH MAGNETOSPHERE; SOLAR PARTICLES; CHARGED PARTICLES; MAGNETOPAUSE; EARTH ATMOSPHERE; RADIATIONS; SOLAR RADIATION; STELLAR RADIATION; 640201* - Atmospheric Physics- Auroral, Ionospheric, & Magetospheric Phenomena

Citation Formats

Lee, L C, and Akasofu, S. Entry of solar wind particles into Earth's magnetosphere. United States: N. p., 1989. Web. doi:10.1029/JA094iA09p12015.
Lee, L C, & Akasofu, S. Entry of solar wind particles into Earth's magnetosphere. United States. doi:10.1029/JA094iA09p12015.
Lee, L C, and Akasofu, S. Fri . "Entry of solar wind particles into Earth's magnetosphere". United States. doi:10.1029/JA094iA09p12015.
@article{osti_5219741,
title = {Entry of solar wind particles into Earth's magnetosphere},
author = {Lee, L C and Akasofu, S},
abstractNote = {Entry of solar wind particles into Earth's magnetosphere is studied. Particles can move directly across an open'' magnetopause layer, where the magnetic field has a nonzero normal component ({ital B}{sub {ital n}}{ne}0). Under the assumption that the Walen relation holds near the open magnetopause, the solar wind particle influx can be expressed as {ital F}{sub {ital n}}={ital {bar n}}{sup 1/2}{psi}{sub {ital B}}/({mu}{sub 0}{ital m{sub i}}){sup 1/2}, where {ital {bar n}} is the average particle number density, {psi}{sub {ital B}} is the open magnetic flux at the magnetopause, {mu}{sub 0} is the permeability of free space, and {ital m}{sub {ital i}} is the ion mass. The total particle flux from the solar wind to the entire magnetosphere for a moderate negative value of IMF {ital B}{sub {ital z}} is estimated to be {similar to}7.0{times}10{sup 28} s{sup {minus}1}, although most of the particles leave from the antisolar end of the tail without being trapped. The peak flux through the dayside magnetopause is {similar to}1.1{times}10{sup 27} s{sup {minus}1}, while the peak flux through the near-Earth tail magnetopause ({vert bar} {ital x} {vert bar}{le}30{ital R}{sub {ital E}}) is {similar to}3.0{times}10{sup 27} s{sup {minus}1}. The average particle flux through the dayside and tail magnetopause in the region with {vert bar} {ital x} {vert bar}{le}200{ital R}{sub {ital E}} is found to be {similar to}7.9{times}10{sup 27} s{sup {minus}1}, which is comparable to the tailward particle flux ({similar to}7.1{times}10{sup 27} s{sup {minus}1}) observed at {vert bar} {ital x} {vert bar}{approx equal}200--220{ital R}{sub {ital E}} in the distance tail.},
doi = {10.1029/JA094iA09p12015},
journal = {Journal of Geophysical Research; (USA)},
issn = {0148-0227},
number = ,
volume = 94:A9,
place = {United States},
year = {1989},
month = {9}
}