Polar cap electric field structures with a northward interplanetary magnetic field
Polar cap electric fields patterns are presented from times when the S3‐2 Satellite was near the dawn‐dusk meridian and IMF data were available. With Bz ≥ 0.7 γ, two characteristic types of electric field patterns were measured in the polar cap. In the sunlit polar cap the convection pattern usually...
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| Veröffentlicht in: | Geophys. Res. Lett.; (United States) 1979-01, Vol.6 (1), p.21-24 |
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| container_title | Geophys. Res. Lett.; (United States) |
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| creator | Burke, W. J. Kelley, M. C. Sagalyn, R. C. Smiddy, M. Lai, S. T. |
| description | Polar cap electric fields patterns are presented from times when the S3‐2 Satellite was near the dawn‐dusk meridian and IMF data were available. With Bz ≥ 0.7 γ, two characteristic types of electric field patterns were measured in the polar cap. In the sunlit polar cap the convection pattern usually consisted of four cells. Two of the cells were confined to the polar cap with sunward convection in the central portion of the cap. The other pair of cells were marked by anti‐sunward flow along the flanks of the polar cap and by sunward flow in the auroral oval. These observations are interpreted in terms of a model for magnetic merging at the poleward wall of the dayside polar cusp. The sunward flow in the auroral zone is not predicted by the magnetic model and may be due to a viscous interaction between the solar wind and magnetosphere. The second type, which was observed in some of the summer hemisphere passes and all of the winter ones, was characterized by an electric field pattern which was very turbulent, and may be related to inhomogeneous merging. |
| doi_str_mv | 10.1029/GL006i001p00021 |
| format | Article |
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J. ; Kelley, M. C. ; Sagalyn, R. C. ; Smiddy, M. ; Lai, S. T.</creator><creatorcontrib>Burke, W. J. ; Kelley, M. C. ; Sagalyn, R. C. ; Smiddy, M. ; Lai, S. T. ; Research Center, Regis College, Weston, MA 02193</creatorcontrib><description>Polar cap electric fields patterns are presented from times when the S3‐2 Satellite was near the dawn‐dusk meridian and IMF data were available. With Bz ≥ 0.7 γ, two characteristic types of electric field patterns were measured in the polar cap. In the sunlit polar cap the convection pattern usually consisted of four cells. Two of the cells were confined to the polar cap with sunward convection in the central portion of the cap. The other pair of cells were marked by anti‐sunward flow along the flanks of the polar cap and by sunward flow in the auroral oval. These observations are interpreted in terms of a model for magnetic merging at the poleward wall of the dayside polar cusp. The sunward flow in the auroral zone is not predicted by the magnetic model and may be due to a viscous interaction between the solar wind and magnetosphere. The second type, which was observed in some of the summer hemisphere passes and all of the winter ones, was characterized by an electric field pattern which was very turbulent, and may be related to inhomogeneous merging.</description><identifier>ISSN: 0094-8276</identifier><identifier>EISSN: 1944-8007</identifier><identifier>DOI: 10.1029/GL006i001p00021</identifier><language>eng</language><publisher>United States: Blackwell Publishing Ltd</publisher><subject>640203 - Atmospheric Physics- Magnetospheric Phenomena- (-1987) ; AURORAE ; AURORAL OVAL ; CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS ; Convection ; EARTH ATMOSPHERE ; ELECTRIC FIELDS ; Hemispheres ; INTERPLANETARY MAGNETIC FIELDS ; MAGNETIC FIELD CONFIGURATIONS ; MAGNETIC FIELDS ; MAGNETOSPHERE ; Mathematical models ; Merging ; POLAR REGIONS ; POLAR-CAP AURORAE ; SOLAR ACTIVITY ; SOLAR WIND ; Turbulence ; Walls ; Winter</subject><ispartof>Geophys. Res. 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J.</creatorcontrib><creatorcontrib>Kelley, M. C.</creatorcontrib><creatorcontrib>Sagalyn, R. C.</creatorcontrib><creatorcontrib>Smiddy, M.</creatorcontrib><creatorcontrib>Lai, S. T.</creatorcontrib><creatorcontrib>Research Center, Regis College, Weston, MA 02193</creatorcontrib><title>Polar cap electric field structures with a northward interplanetary magnetic field</title><title>Geophys. Res. Lett.; (United States)</title><addtitle>Geophys. Res. Lett</addtitle><description>Polar cap electric fields patterns are presented from times when the S3‐2 Satellite was near the dawn‐dusk meridian and IMF data were available. With Bz ≥ 0.7 γ, two characteristic types of electric field patterns were measured in the polar cap. In the sunlit polar cap the convection pattern usually consisted of four cells. Two of the cells were confined to the polar cap with sunward convection in the central portion of the cap. The other pair of cells were marked by anti‐sunward flow along the flanks of the polar cap and by sunward flow in the auroral oval. These observations are interpreted in terms of a model for magnetic merging at the poleward wall of the dayside polar cusp. The sunward flow in the auroral zone is not predicted by the magnetic model and may be due to a viscous interaction between the solar wind and magnetosphere. The second type, which was observed in some of the summer hemisphere passes and all of the winter ones, was characterized by an electric field pattern which was very turbulent, and may be related to inhomogeneous merging.</description><subject>640203 - Atmospheric Physics- Magnetospheric Phenomena- (-1987)</subject><subject>AURORAE</subject><subject>AURORAL OVAL</subject><subject>CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS</subject><subject>Convection</subject><subject>EARTH ATMOSPHERE</subject><subject>ELECTRIC FIELDS</subject><subject>Hemispheres</subject><subject>INTERPLANETARY MAGNETIC FIELDS</subject><subject>MAGNETIC FIELD CONFIGURATIONS</subject><subject>MAGNETIC FIELDS</subject><subject>MAGNETOSPHERE</subject><subject>Mathematical models</subject><subject>Merging</subject><subject>POLAR REGIONS</subject><subject>POLAR-CAP AURORAE</subject><subject>SOLAR ACTIVITY</subject><subject>SOLAR WIND</subject><subject>Turbulence</subject><subject>Walls</subject><subject>Winter</subject><issn>0094-8276</issn><issn>1944-8007</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>1979</creationdate><recordtype>article</recordtype><recordid>eNqFkT2PEzEQhi3ESYRATWtRIJrl_LX-KFHgAiIc6HQopTVxbGLY7C62o9z9exwtUFBcqpnieUYz8yL0gpI3lDBzuVwRIiMhdCSEMPoIzagRotGEqMdoRoipPVPyCXqa84-KcMLpDN18HTpI2MGIfeddSdHhEH23xbmkgyuH5DM-xrLDgPshld0R0hbHvvg0dtD7Auke7-F77f6az9BFgC7753_qHH27en-7-NCsviw_Lt6uGscNNY0S2jndAucCHEjpBQlcbTz4jdFCBg3UGVDMUNgoshWB-GCCVNoAA7MNfI5eTnOHXKLNLhbvdm7o-3qGlUJqI2WFXk3QmIZfB5-L3cfsfHfafThky3jL5ekX50CqBW0ZVxV8_TAoFW0N1VyfR1tmTMtOYczR5YS6NOScfLBjivv6XEuJPeVr_8u3GnwyjrHz9-dwu7xZGWaq1UxWzMXf_bMg_bRScdXa9fXSvluw20-f12t7zX8DaGi2kQ</recordid><startdate>197901</startdate><enddate>197901</enddate><creator>Burke, W. 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T.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c3919-748cc85a334aca66e40f37beaeb9846f8a1c9a7291ab70d4f0ef9f6789a2a9df3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>1979</creationdate><topic>640203 - Atmospheric Physics- Magnetospheric Phenomena- (-1987)</topic><topic>AURORAE</topic><topic>AURORAL OVAL</topic><topic>CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS</topic><topic>Convection</topic><topic>EARTH ATMOSPHERE</topic><topic>ELECTRIC FIELDS</topic><topic>Hemispheres</topic><topic>INTERPLANETARY MAGNETIC FIELDS</topic><topic>MAGNETIC FIELD CONFIGURATIONS</topic><topic>MAGNETIC FIELDS</topic><topic>MAGNETOSPHERE</topic><topic>Mathematical models</topic><topic>Merging</topic><topic>POLAR REGIONS</topic><topic>POLAR-CAP AURORAE</topic><topic>SOLAR ACTIVITY</topic><topic>SOLAR WIND</topic><topic>Turbulence</topic><topic>Walls</topic><topic>Winter</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Burke, W. J.</creatorcontrib><creatorcontrib>Kelley, M. C.</creatorcontrib><creatorcontrib>Sagalyn, R. C.</creatorcontrib><creatorcontrib>Smiddy, M.</creatorcontrib><creatorcontrib>Lai, S. T.</creatorcontrib><creatorcontrib>Research Center, Regis College, Weston, MA 02193</creatorcontrib><collection>Istex</collection><collection>CrossRef</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Mechanical & Transportation Engineering Abstracts</collection><collection>Engineering Research Database</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>Burke, W. J.</au><au>Kelley, M. C.</au><au>Sagalyn, R. C.</au><au>Smiddy, M.</au><au>Lai, S. T.</au><aucorp>Research Center, Regis College, Weston, MA 02193</aucorp><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Polar cap electric field structures with a northward interplanetary magnetic field</atitle><jtitle>Geophys. Res. Lett.; (United States)</jtitle><addtitle>Geophys. Res. Lett</addtitle><date>1979-01</date><risdate>1979</risdate><volume>6</volume><issue>1</issue><spage>21</spage><epage>24</epage><pages>21-24</pages><issn>0094-8276</issn><eissn>1944-8007</eissn><abstract>Polar cap electric fields patterns are presented from times when the S3‐2 Satellite was near the dawn‐dusk meridian and IMF data were available. With Bz ≥ 0.7 γ, two characteristic types of electric field patterns were measured in the polar cap. In the sunlit polar cap the convection pattern usually consisted of four cells. Two of the cells were confined to the polar cap with sunward convection in the central portion of the cap. The other pair of cells were marked by anti‐sunward flow along the flanks of the polar cap and by sunward flow in the auroral oval. These observations are interpreted in terms of a model for magnetic merging at the poleward wall of the dayside polar cusp. The sunward flow in the auroral zone is not predicted by the magnetic model and may be due to a viscous interaction between the solar wind and magnetosphere. The second type, which was observed in some of the summer hemisphere passes and all of the winter ones, was characterized by an electric field pattern which was very turbulent, and may be related to inhomogeneous merging.</abstract><cop>United States</cop><pub>Blackwell Publishing Ltd</pub><doi>10.1029/GL006i001p00021</doi><tpages>4</tpages></addata></record> |
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| source | Wiley Online Library Journals Frontfile Complete |
| subjects | 640203 - Atmospheric Physics- Magnetospheric Phenomena- (-1987) AURORAE AURORAL OVAL CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS Convection EARTH ATMOSPHERE ELECTRIC FIELDS Hemispheres INTERPLANETARY MAGNETIC FIELDS MAGNETIC FIELD CONFIGURATIONS MAGNETIC FIELDS MAGNETOSPHERE Mathematical models Merging POLAR REGIONS POLAR-CAP AURORAE SOLAR ACTIVITY SOLAR WIND Turbulence Walls Winter |
| title | Polar cap electric field structures with a northward interplanetary magnetic field |
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