EUV flux variation during end of solar cycle 20 and beginning cycle 21, observed from AE-C satellite

Minimum levels of solar EUV fluxes appear to have occurred about 14 months before July 1976, the month designated as the start of Cycle 21 (minimum of monthly mean value of sunspot number, RZ). The EUV minimum, observed by the EUVS experiment on AE‐C, occurred around 20 April 1975 under conditions o...

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Veröffentlicht in:	Geophys. Res. Lett.; (United States) 1977-06, Vol.4 (6), p.231-234
1. Verfasser:	Hinteregger, H. E.
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Sprache:	eng
Schlagworte:	640104 - Astrophysics & Cosmology- Solar Phenomena CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS Disks ELECTROMAGNETIC RADIATION EXTREME ULTRAVIOLET RADIATION Flux Fluxes Geophysics Iron RADIATIONS Satellites SOLAR ACTIVITY Solar cycles SOLAR FLUX SOLAR RADIATION SUNSPOTS ULTRAVIOLET RADIATION VARIATIONS
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container_title	Geophys. Res. Lett.; (United States)
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creator	Hinteregger, H. E.
description	Minimum levels of solar EUV fluxes appear to have occurred about 14 months before July 1976, the month designated as the start of Cycle 21 (minimum of monthly mean value of sunspot number, RZ). The EUV minimum, observed by the EUVS experiment on AE‐C, occurred around 20 April 1975 under conditions of a spotless disk and of a simultaneous minimum in F10.7. Another rise of quiet‐disk EUV, observed a few months before July 1976, was found in the low‐excitation lines such as 584 Å He I and 1026 Å H Ly‐β. The transition‐region lines of Fe X at 174.5 and 177.2 Å showed a substantial gradual rise later, toward the end of 1976 and mainly in early 1977, when periods of spotless disk with simultaneously minimal F10.730 with F10.7>80) on different sides of the sunspot minimum show drastically different relations to F10.7.
doi_str_mv	10.1029/GL004i006p00231
format	Article
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E.</creator><creatorcontrib>Hinteregger, H. E. ; Air Force Geophysics Laboratory, Hanscom AFB, Bedford, Massachusetts 01731</creatorcontrib><description>Minimum levels of solar EUV fluxes appear to have occurred about 14 months before July 1976, the month designated as the start of Cycle 21 (minimum of monthly mean value of sunspot number, RZ). The EUV minimum, observed by the EUVS experiment on AE‐C, occurred around 20 April 1975 under conditions of a spotless disk and of a simultaneous minimum in F10.7. Another rise of quiet‐disk EUV, observed a few months before July 1976, was found in the low‐excitation lines such as 584 Å He I and 1026 Å H Ly‐β. The transition‐region lines of Fe X at 174.5 and 177.2 Å showed a substantial gradual rise later, toward the end of 1976 and mainly in early 1977, when periods of spotless disk with simultaneously minimal F10.7<70 no longer existed. EUV fluxes for days of "high" activity (RZ>30 with F10.7>80) on different sides of the sunspot minimum show drastically different relations to F10.7.</description><identifier>ISSN: 0094-8276</identifier><identifier>EISSN: 1944-8007</identifier><identifier>DOI: 10.1029/GL004i006p00231</identifier><language>eng</language><publisher>United States: Blackwell Publishing Ltd</publisher><subject>640104 - Astrophysics & Cosmology- Solar Phenomena ; CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS ; Disks ; ELECTROMAGNETIC RADIATION ; EXTREME ULTRAVIOLET RADIATION ; Flux ; Fluxes ; Geophysics ; Iron ; RADIATIONS ; Satellites ; SOLAR ACTIVITY ; Solar cycles ; SOLAR FLUX ; SOLAR RADIATION ; SUNSPOTS ; ULTRAVIOLET RADIATION ; VARIATIONS</subject><ispartof>Geophys. Res. 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E.</creatorcontrib><creatorcontrib>Air Force Geophysics Laboratory, Hanscom AFB, Bedford, Massachusetts 01731</creatorcontrib><title>EUV flux variation during end of solar cycle 20 and beginning cycle 21, observed from AE-C satellite</title><title>Geophys. Res. Lett.; (United States)</title><addtitle>Geophys. Res. Lett</addtitle><description>Minimum levels of solar EUV fluxes appear to have occurred about 14 months before July 1976, the month designated as the start of Cycle 21 (minimum of monthly mean value of sunspot number, RZ). The EUV minimum, observed by the EUVS experiment on AE‐C, occurred around 20 April 1975 under conditions of a spotless disk and of a simultaneous minimum in F10.7. Another rise of quiet‐disk EUV, observed a few months before July 1976, was found in the low‐excitation lines such as 584 Å He I and 1026 Å H Ly‐β. The transition‐region lines of Fe X at 174.5 and 177.2 Å showed a substantial gradual rise later, toward the end of 1976 and mainly in early 1977, when periods of spotless disk with simultaneously minimal F10.7<70 no longer existed. EUV fluxes for days of "high" activity (RZ>30 with F10.7>80) on different sides of the sunspot minimum show drastically different relations to F10.7.</description><subject>640104 - Astrophysics & Cosmology- Solar Phenomena</subject><subject>CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS</subject><subject>Disks</subject><subject>ELECTROMAGNETIC RADIATION</subject><subject>EXTREME ULTRAVIOLET RADIATION</subject><subject>Flux</subject><subject>Fluxes</subject><subject>Geophysics</subject><subject>Iron</subject><subject>RADIATIONS</subject><subject>Satellites</subject><subject>SOLAR ACTIVITY</subject><subject>Solar cycles</subject><subject>SOLAR FLUX</subject><subject>SOLAR RADIATION</subject><subject>SUNSPOTS</subject><subject>ULTRAVIOLET RADIATION</subject><subject>VARIATIONS</subject><issn>0094-8276</issn><issn>1944-8007</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>1977</creationdate><recordtype>article</recordtype><recordid>eNqFkU1v1DAQhiMEEkvhzNXigDiQdmzHdnysVktASouEKEhcLMeZFEM2Xuxs6f57vErFgQN7mtHoeeedj6J4SeGcAtMXTQtQeQC5A2CcPipWVFdVWQOox8UKQOecKfm0eJbSDwDgwOmq6Dc3X8gw7u_JnY3ezj5MpN9HP90SnHoSBpLCaCNxBzciYUBsrnZ466fpyDyU6VsSuoTxDnsyxLAll5tyTZKdcRz9jM-LJ4MdE754iGfFzbvN5_X7sv3YfFhftqWrlGSl6KiSg62xHlive0p7lFbWvBtEjmJgVDmtuRsYdhbRUsuchqoHdOhYz_hZ8WrpG9LsTXLZ2n13YZrQzUZxCrISGXq9QLsYfu0xzWbrk8uD2gnDPhnGtBZK6ZMgrSuu60pm8M3_QamoqEEwOI2K7A5CwnGZiwV1MaQUcTC76Lc2HgwFc_y4-efjWcEXxW8_4uEUbppPreBHn3JR-TTj_V-VjT-NVFwJ8_W6MYJdtc01_Zav-AeTmrp6</recordid><startdate>197706</startdate><enddate>197706</enddate><creator>Hinteregger, H. E.</creator><general>Blackwell Publishing Ltd</general><scope>BSCLL</scope><scope>AAYXX</scope><scope>CITATION</scope><scope>8FD</scope><scope>H8D</scope><scope>L7M</scope><scope>7TG</scope><scope>KL.</scope><scope>OTOTI</scope></search><sort><creationdate>197706</creationdate><title>EUV flux variation during end of solar cycle 20 and beginning cycle 21, observed from AE-C satellite</title><author>Hinteregger, H. E.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c4762-5b176fa8e8f2d9d11de6a683bf56a65f217c993cf2ebaeea1a2c904d0ecec2d23</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>1977</creationdate><topic>640104 - Astrophysics & Cosmology- Solar Phenomena</topic><topic>CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS</topic><topic>Disks</topic><topic>ELECTROMAGNETIC RADIATION</topic><topic>EXTREME ULTRAVIOLET RADIATION</topic><topic>Flux</topic><topic>Fluxes</topic><topic>Geophysics</topic><topic>Iron</topic><topic>RADIATIONS</topic><topic>Satellites</topic><topic>SOLAR ACTIVITY</topic><topic>Solar cycles</topic><topic>SOLAR FLUX</topic><topic>SOLAR RADIATION</topic><topic>SUNSPOTS</topic><topic>ULTRAVIOLET RADIATION</topic><topic>VARIATIONS</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Hinteregger, H. E.</creatorcontrib><creatorcontrib>Air Force Geophysics Laboratory, Hanscom AFB, Bedford, Massachusetts 01731</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>OSTI.GOV</collection><jtitle>Geophys. Res. Lett.; (United States)</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Hinteregger, H. E.</au><aucorp>Air Force Geophysics Laboratory, Hanscom AFB, Bedford, Massachusetts 01731</aucorp><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>EUV flux variation during end of solar cycle 20 and beginning cycle 21, observed from AE-C satellite</atitle><jtitle>Geophys. Res. Lett.; (United States)</jtitle><addtitle>Geophys. Res. Lett</addtitle><date>1977-06</date><risdate>1977</risdate><volume>4</volume><issue>6</issue><spage>231</spage><epage>234</epage><pages>231-234</pages><issn>0094-8276</issn><eissn>1944-8007</eissn><abstract>Minimum levels of solar EUV fluxes appear to have occurred about 14 months before July 1976, the month designated as the start of Cycle 21 (minimum of monthly mean value of sunspot number, RZ). The EUV minimum, observed by the EUVS experiment on AE‐C, occurred around 20 April 1975 under conditions of a spotless disk and of a simultaneous minimum in F10.7. Another rise of quiet‐disk EUV, observed a few months before July 1976, was found in the low‐excitation lines such as 584 Å He I and 1026 Å H Ly‐β. The transition‐region lines of Fe X at 174.5 and 177.2 Å showed a substantial gradual rise later, toward the end of 1976 and mainly in early 1977, when periods of spotless disk with simultaneously minimal F10.7<70 no longer existed. EUV fluxes for days of "high" activity (RZ>30 with F10.7>80) on different sides of the sunspot minimum show drastically different relations to F10.7.</abstract><cop>United States</cop><pub>Blackwell Publishing Ltd</pub><doi>10.1029/GL004i006p00231</doi><tpages>4</tpages></addata></record>
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subjects	640104 - Astrophysics & Cosmology- Solar Phenomena CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS Disks ELECTROMAGNETIC RADIATION EXTREME ULTRAVIOLET RADIATION Flux Fluxes Geophysics Iron RADIATIONS Satellites SOLAR ACTIVITY Solar cycles SOLAR FLUX SOLAR RADIATION SUNSPOTS ULTRAVIOLET RADIATION VARIATIONS
title	EUV flux variation during end of solar cycle 20 and beginning cycle 21, observed from AE-C satellite
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