The EUV Unresolved Corona

The EUV Unresolved Corona

The unresolved corona for three active regions (ARs) above the solar limb is investigated. Intensities measured for ions formed above 1 MK are presented as a function of height above the solar surface. The observed decrease in intensity with altitude is found to be best fit by an exponential. Furthe...

Ausführliche Beschreibung

Gespeichert in:
Bibliographische Detailangaben
Veröffentlicht in:Solar physics 2006-05, Vol.235 (1-2), p.295-316
Hauptverfasser: Cirtain, Jonathan, Martens, PCH, Acton, L W, Weber, Mark
Format: Artikel
Sprache:eng
Schlagworte:
Corona
Solar physics
Studies
Online-Zugang:Volltext
Tags: Tag hinzufügen
Keine Tags, Fügen Sie den ersten Tag hinzu!
container_end_page 316
container_issue 1-2
container_start_page 295
container_title Solar physics
container_volume 235
creator Cirtain, Jonathan
Martens, PCH
Acton, L W
Weber, Mark
description The unresolved corona for three active regions (ARs) above the solar limb is investigated. Intensities measured for ions formed above 1 MK are presented as a function of height above the solar surface. The observed decrease in intensity with altitude is found to be best fit by an exponential. Furthermore, this exponential decrease is approximately the decrease in emission expected for a hydrostatic planar geometry atmosphere, where the scale height temperature is dependent on the dynamics of the AR. For two of the ARs analyzed, we have found that the best-fit temperature derived from the exponential fits is consistent with an isothermal hydrostatic unresolved corona.
doi_str_mv 10.1007/s11207-006-0035-3
format Article
fullrecord <record><control><sourceid>proquest_cross</sourceid><recordid>TN_cdi_proquest_miscellaneous_954521310</recordid><sourceformat>XML</sourceformat><sourcesystem>PC</sourcesystem><sourcerecordid>954521310</sourcerecordid><originalsourceid>FETCH-LOGICAL-c367t-aa3d3314f8798ea2d7d78a5e5e418bba6b179f940a2fa6423e6d668f17e9af3e3</originalsourceid><addsrcrecordid>eNqFkEtLAzEQgIMoWB8_oLfiQU-rM5lkkxyl1AcUvLTiLaTdBFu2m5q0gv_eLPXkQQ_DDMM3w8zH2BDhFgHUXUbkoCqAugTJio7YAKWiCgy9HbNBaeq-1qfsLOc1QD8lB2w4e_ejyfx1NO-Sz7H99M1oHFPs3AU7Ca7N_vInn7P5w2Q2fqqmL4_P4_tptaRa7SrnqCFCEbQy2jveqEZpJ730AvVi4eoFKhOMAMeDqwUnXzd1rQMqb1wgT-fs5rB3m-LH3ued3azy0ret63zcZ2ukkBwJ4V9SCQJlgHghr_8k0ZSTucACXv0C13GfuvKvVSSUUIbrAuEBWqaYc_LBbtNq49KXRbC9R3uwb4t929u3RN8CcHQF</addsrcrecordid><sourcetype>Aggregation Database</sourcetype><iscdi>true</iscdi><recordtype>article</recordtype><pqid>734747928</pqid></control><display><type>article</type><title>The EUV Unresolved Corona</title><source>SpringerLink Journals - AutoHoldings</source><creator>Cirtain, Jonathan ; Martens, PCH ; Acton, L W ; Weber, Mark</creator><creatorcontrib>Cirtain, Jonathan ; Martens, PCH ; Acton, L W ; Weber, Mark</creatorcontrib><description>The unresolved corona for three active regions (ARs) above the solar limb is investigated. Intensities measured for ions formed above 1 MK are presented as a function of height above the solar surface. The observed decrease in intensity with altitude is found to be best fit by an exponential. Furthermore, this exponential decrease is approximately the decrease in emission expected for a hydrostatic planar geometry atmosphere, where the scale height temperature is dependent on the dynamics of the AR. For two of the ARs analyzed, we have found that the best-fit temperature derived from the exponential fits is consistent with an isothermal hydrostatic unresolved corona.</description><identifier>ISSN: 0038-0938</identifier><identifier>EISSN: 1573-093X</identifier><identifier>DOI: 10.1007/s11207-006-0035-3</identifier><language>eng</language><publisher>Dordrecht: Springer Nature B.V</publisher><subject>Corona ; Solar physics ; Studies</subject><ispartof>Solar physics, 2006-05, Vol.235 (1-2), p.295-316</ispartof><rights>Springer Science + Business Media, Inc. 2006</rights><lds50>peer_reviewed</lds50><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c367t-aa3d3314f8798ea2d7d78a5e5e418bba6b179f940a2fa6423e6d668f17e9af3e3</citedby><cites>FETCH-LOGICAL-c367t-aa3d3314f8798ea2d7d78a5e5e418bba6b179f940a2fa6423e6d668f17e9af3e3</cites></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>314,780,784,27924,27925</link.rule.ids></links><search><creatorcontrib>Cirtain, Jonathan</creatorcontrib><creatorcontrib>Martens, PCH</creatorcontrib><creatorcontrib>Acton, L W</creatorcontrib><creatorcontrib>Weber, Mark</creatorcontrib><title>The EUV Unresolved Corona</title><title>Solar physics</title><description>The unresolved corona for three active regions (ARs) above the solar limb is investigated. Intensities measured for ions formed above 1 MK are presented as a function of height above the solar surface. The observed decrease in intensity with altitude is found to be best fit by an exponential. Furthermore, this exponential decrease is approximately the decrease in emission expected for a hydrostatic planar geometry atmosphere, where the scale height temperature is dependent on the dynamics of the AR. For two of the ARs analyzed, we have found that the best-fit temperature derived from the exponential fits is consistent with an isothermal hydrostatic unresolved corona.</description><subject>Corona</subject><subject>Solar physics</subject><subject>Studies</subject><issn>0038-0938</issn><issn>1573-093X</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2006</creationdate><recordtype>article</recordtype><sourceid>ABUWG</sourceid><sourceid>AFKRA</sourceid><sourceid>AZQEC</sourceid><sourceid>BENPR</sourceid><sourceid>CCPQU</sourceid><sourceid>DWQXO</sourceid><sourceid>GNUQQ</sourceid><recordid>eNqFkEtLAzEQgIMoWB8_oLfiQU-rM5lkkxyl1AcUvLTiLaTdBFu2m5q0gv_eLPXkQQ_DDMM3w8zH2BDhFgHUXUbkoCqAugTJio7YAKWiCgy9HbNBaeq-1qfsLOc1QD8lB2w4e_ejyfx1NO-Sz7H99M1oHFPs3AU7Ca7N_vInn7P5w2Q2fqqmL4_P4_tptaRa7SrnqCFCEbQy2jveqEZpJ730AvVi4eoFKhOMAMeDqwUnXzd1rQMqb1wgT-fs5rB3m-LH3ued3azy0ret63zcZ2ukkBwJ4V9SCQJlgHghr_8k0ZSTucACXv0C13GfuvKvVSSUUIbrAuEBWqaYc_LBbtNq49KXRbC9R3uwb4t929u3RN8CcHQF</recordid><startdate>20060501</startdate><enddate>20060501</enddate><creator>Cirtain, Jonathan</creator><creator>Martens, PCH</creator><creator>Acton, L W</creator><creator>Weber, Mark</creator><general>Springer Nature B.V</general><scope>AAYXX</scope><scope>CITATION</scope><scope>3V.</scope><scope>7TG</scope><scope>7XB</scope><scope>88I</scope><scope>8FD</scope><scope>8FE</scope><scope>8FG</scope><scope>8FK</scope><scope>ABUWG</scope><scope>AFKRA</scope><scope>ARAPS</scope><scope>AZQEC</scope><scope>BENPR</scope><scope>BGLVJ</scope><scope>CCPQU</scope><scope>DWQXO</scope><scope>GNUQQ</scope><scope>H8D</scope><scope>HCIFZ</scope><scope>KL.</scope><scope>L7M</scope><scope>M2P</scope><scope>P5Z</scope><scope>P62</scope><scope>PQEST</scope><scope>PQQKQ</scope><scope>PQUKI</scope><scope>Q9U</scope></search><sort><creationdate>20060501</creationdate><title>The EUV Unresolved Corona</title><author>Cirtain, Jonathan ; Martens, PCH ; Acton, L W ; Weber, Mark</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c367t-aa3d3314f8798ea2d7d78a5e5e418bba6b179f940a2fa6423e6d668f17e9af3e3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2006</creationdate><topic>Corona</topic><topic>Solar physics</topic><topic>Studies</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Cirtain, Jonathan</creatorcontrib><creatorcontrib>Martens, PCH</creatorcontrib><creatorcontrib>Acton, L W</creatorcontrib><creatorcontrib>Weber, Mark</creatorcontrib><collection>CrossRef</collection><collection>ProQuest Central (Corporate)</collection><collection>Meteorological &amp; Geoastrophysical Abstracts</collection><collection>ProQuest Central (purchase pre-March 2016)</collection><collection>Science Database (Alumni Edition)</collection><collection>Technology Research Database</collection><collection>ProQuest SciTech Collection</collection><collection>ProQuest Technology Collection</collection><collection>ProQuest Central (Alumni) (purchase pre-March 2016)</collection><collection>ProQuest Central (Alumni Edition)</collection><collection>ProQuest Central UK/Ireland</collection><collection>Advanced Technologies &amp; Aerospace Collection</collection><collection>ProQuest Central Essentials</collection><collection>ProQuest Central</collection><collection>Technology Collection</collection><collection>ProQuest One Community College</collection><collection>ProQuest Central Korea</collection><collection>ProQuest Central Student</collection><collection>Aerospace Database</collection><collection>SciTech Premium Collection</collection><collection>Meteorological &amp; Geoastrophysical Abstracts - Academic</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>Science Database</collection><collection>Advanced Technologies &amp; Aerospace Database</collection><collection>ProQuest Advanced Technologies &amp; Aerospace Collection</collection><collection>ProQuest One Academic Eastern Edition (DO NOT USE)</collection><collection>ProQuest One Academic</collection><collection>ProQuest One Academic UKI Edition</collection><collection>ProQuest Central Basic</collection><jtitle>Solar physics</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Cirtain, Jonathan</au><au>Martens, PCH</au><au>Acton, L W</au><au>Weber, Mark</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>The EUV Unresolved Corona</atitle><jtitle>Solar physics</jtitle><date>2006-05-01</date><risdate>2006</risdate><volume>235</volume><issue>1-2</issue><spage>295</spage><epage>316</epage><pages>295-316</pages><issn>0038-0938</issn><eissn>1573-093X</eissn><abstract>The unresolved corona for three active regions (ARs) above the solar limb is investigated. Intensities measured for ions formed above 1 MK are presented as a function of height above the solar surface. The observed decrease in intensity with altitude is found to be best fit by an exponential. Furthermore, this exponential decrease is approximately the decrease in emission expected for a hydrostatic planar geometry atmosphere, where the scale height temperature is dependent on the dynamics of the AR. For two of the ARs analyzed, we have found that the best-fit temperature derived from the exponential fits is consistent with an isothermal hydrostatic unresolved corona.</abstract><cop>Dordrecht</cop><pub>Springer Nature B.V</pub><doi>10.1007/s11207-006-0035-3</doi><tpages>22</tpages></addata></record>
fulltext fulltext
identifier ISSN: 0038-0938
ispartof Solar physics, 2006-05, Vol.235 (1-2), p.295-316
issn 0038-0938
1573-093X
language eng
recordid cdi_proquest_miscellaneous_954521310
source SpringerLink Journals - AutoHoldings
subjects Corona
Solar physics
Studies
title The EUV Unresolved Corona
url https://sfx.bib-bvb.de/sfx_tum?ctx_ver=Z39.88-2004&ctx_enc=info:ofi/enc:UTF-8&ctx_tim=2024-12-29T15%3A09%3A26IST&url_ver=Z39.88-2004&url_ctx_fmt=infofi/fmt:kev:mtx:ctx&rfr_id=info:sid/primo.exlibrisgroup.com:primo3-Article-proquest_cross&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.genre=article&rft.atitle=The%20EUV%20Unresolved%20Corona&rft.jtitle=Solar%20physics&rft.au=Cirtain,%20Jonathan&rft.date=2006-05-01&rft.volume=235&rft.issue=1-2&rft.spage=295&rft.epage=316&rft.pages=295-316&rft.issn=0038-0938&rft.eissn=1573-093X&rft_id=info:doi/10.1007/s11207-006-0035-3&rft_dat=%3Cproquest_cross%3E954521310%3C/proquest_cross%3E%3Curl%3E%3C/url%3E&disable_directlink=true&sfx.directlink=off&sfx.report_link=0&rft_id=info:oai/&rft_pqid=734747928&rft_id=info:pmid/&rfr_iscdi=true