Thin sheets of energetic electrons upstream from the Earth's bow shock
ISEE spacecraft observations show that energetic, ≥ 16 keV electrons are injected into the region upstream from the Earth’s bow shock in a thin sheet which lies just behind the sheet of interplanetary magnetic field lines that are tangent to the shock surface. Lower energy electrons leave the shock...
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| Veröffentlicht in: | Geophys. Res. Lett.; (United States) 1979-05, Vol.6 (5), p.401-404 |
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| container_title | Geophys. Res. Lett.; (United States) |
| container_volume | 6 |
| creator | Anderson, K. A. Lin, R. P. Martel, F. Lin, C. S. Parks, G. K. Rème, H. |
| description | ISEE spacecraft observations show that energetic, ≥ 16 keV electrons are injected into the region upstream from the Earth’s bow shock in a thin sheet which lies just behind the sheet of interplanetary magnetic field lines that are tangent to the shock surface. Lower energy electrons leave the shock over a much broader region. Although the energetic electron intensity varies, the sheet is nearly always present and may be a quasi‐steady state feature of the bow shock. The electron velocity distribution in the thin sheet is strongly peaked and is responsible for excitation of electron plasma waves. |
| doi_str_mv | 10.1029/GL006i005p00401 |
| format | Article |
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A. ; Lin, R. P. ; Martel, F. ; Lin, C. S. ; Parks, G. K. ; Rème, H.</creator><creatorcontrib>Anderson, K. A. ; Lin, R. P. ; Martel, F. ; Lin, C. S. ; Parks, G. K. ; Rème, H. ; Space Sciences Laboratory, University of California, Berkeley, CA 94720</creatorcontrib><description>ISEE spacecraft observations show that energetic, ≥ 16 keV electrons are injected into the region upstream from the Earth’s bow shock in a thin sheet which lies just behind the sheet of interplanetary magnetic field lines that are tangent to the shock surface. Lower energy electrons leave the shock over a much broader region. Although the energetic electron intensity varies, the sheet is nearly always present and may be a quasi‐steady state feature of the bow shock. The electron velocity distribution in the thin sheet is strongly peaked and is responsible for excitation of electron plasma waves.</description><identifier>ISSN: 0094-8276</identifier><identifier>EISSN: 1944-8007</identifier><identifier>DOI: 10.1029/GL006i005p00401</identifier><language>eng</language><publisher>United States: Blackwell Publishing Ltd</publisher><subject>640203 - Atmospheric Physics- Magnetospheric Phenomena- (-1987) ; CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS ; DISTRIBUTION FUNCTIONS ; Earth ; EARTH ATMOSPHERE ; ELECTRON DENSITY ; Electron plasma ; ELECTRONS ; ELEMENTARY PARTICLES ; ENERGY RANGE ; FERMIONS ; Geophysics ; INCLINATION ; INTERPLANETARY MAGNETIC FIELDS ; KEV RANGE ; LEPTONS ; MAGNETIC FIELDS ; MAGNETOSPHERE ; PLASMA WAVES ; Quasi-steady states ; SOLAR ACTIVITY ; SOLAR WIND ; Spacecraft ; Tangents ; Upstream</subject><ispartof>Geophys. Res. 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A.</creatorcontrib><creatorcontrib>Lin, R. P.</creatorcontrib><creatorcontrib>Martel, F.</creatorcontrib><creatorcontrib>Lin, C. S.</creatorcontrib><creatorcontrib>Parks, G. K.</creatorcontrib><creatorcontrib>Rème, H.</creatorcontrib><creatorcontrib>Space Sciences Laboratory, University of California, Berkeley, CA 94720</creatorcontrib><title>Thin sheets of energetic electrons upstream from the Earth's bow shock</title><title>Geophys. Res. Lett.; (United States)</title><addtitle>Geophys. Res. Lett</addtitle><description>ISEE spacecraft observations show that energetic, ≥ 16 keV electrons are injected into the region upstream from the Earth’s bow shock in a thin sheet which lies just behind the sheet of interplanetary magnetic field lines that are tangent to the shock surface. Lower energy electrons leave the shock over a much broader region. Although the energetic electron intensity varies, the sheet is nearly always present and may be a quasi‐steady state feature of the bow shock. 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A.</creatorcontrib><creatorcontrib>Lin, R. P.</creatorcontrib><creatorcontrib>Martel, F.</creatorcontrib><creatorcontrib>Lin, C. S.</creatorcontrib><creatorcontrib>Parks, G. K.</creatorcontrib><creatorcontrib>Rème, H.</creatorcontrib><creatorcontrib>Space Sciences Laboratory, University of California, Berkeley, CA 94720</creatorcontrib><collection>Istex</collection><collection>CrossRef</collection><collection>Environmental Engineering Abstracts</collection><collection>Technology Research Database</collection><collection>Environmental Sciences and Pollution Management</collection><collection>Engineering Research Database</collection><collection>Aerospace Database</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>Mechanical & Transportation Engineering Abstracts</collection><collection>OSTI.GOV</collection><jtitle>Geophys. Res. Lett.; (United States)</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Anderson, K. A.</au><au>Lin, R. P.</au><au>Martel, F.</au><au>Lin, C. S.</au><au>Parks, G. K.</au><au>Rème, H.</au><aucorp>Space Sciences Laboratory, University of California, Berkeley, CA 94720</aucorp><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Thin sheets of energetic electrons upstream from the Earth's bow shock</atitle><jtitle>Geophys. Res. Lett.; (United States)</jtitle><addtitle>Geophys. Res. Lett</addtitle><date>1979-05</date><risdate>1979</risdate><volume>6</volume><issue>5</issue><spage>401</spage><epage>404</epage><pages>401-404</pages><issn>0094-8276</issn><eissn>1944-8007</eissn><abstract>ISEE spacecraft observations show that energetic, ≥ 16 keV electrons are injected into the region upstream from the Earth’s bow shock in a thin sheet which lies just behind the sheet of interplanetary magnetic field lines that are tangent to the shock surface. Lower energy electrons leave the shock over a much broader region. Although the energetic electron intensity varies, the sheet is nearly always present and may be a quasi‐steady state feature of the bow shock. The electron velocity distribution in the thin sheet is strongly peaked and is responsible for excitation of electron plasma waves.</abstract><cop>United States</cop><pub>Blackwell Publishing Ltd</pub><doi>10.1029/GL006i005p00401</doi><tpages>4</tpages></addata></record> |
| fulltext | fulltext |
| identifier | ISSN: 0094-8276 |
| ispartof | Geophys. Res. Lett.; (United States), 1979-05, Vol.6 (5), p.401-404 |
| issn | 0094-8276 1944-8007 |
| language | eng |
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| source | Wiley Online Library Journals Frontfile Complete |
| subjects | 640203 - Atmospheric Physics- Magnetospheric Phenomena- (-1987) CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS DISTRIBUTION FUNCTIONS Earth EARTH ATMOSPHERE ELECTRON DENSITY Electron plasma ELECTRONS ELEMENTARY PARTICLES ENERGY RANGE FERMIONS Geophysics INCLINATION INTERPLANETARY MAGNETIC FIELDS KEV RANGE LEPTONS MAGNETIC FIELDS MAGNETOSPHERE PLASMA WAVES Quasi-steady states SOLAR ACTIVITY SOLAR WIND Spacecraft Tangents Upstream |
| title | Thin sheets of energetic electrons upstream from the Earth's bow shock |
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