Helium Emissions Observed in Ground-Based Spectra of Solar Prominences
The only prominent line of singly ionized helium in the visible spectral range, He ii 4686 Å, is observed together with the He i 5015 Å singlet and the He i 4471 Å triplet line in solar prominences. The Na D 2 emission is used as a tracer for He ii emissions which are sufficiently bright to e...
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| Veröffentlicht in: | Solar physics 2012-12, Vol.281 (2), p.697-706 |
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| creator | Ramelli, R. Stellmacher, G. Wiehr, E. Bianda, M. |
| description | The only prominent line of singly ionized helium in the visible spectral range, He
ii
4686 Å, is observed together with the He
i
5015 Å singlet and the He
i
4471 Å triplet line in solar prominences. The Na D
2
emission is used as a tracer for He
ii
emissions which are sufficiently bright to exceed the noise level near 10
−6
of the disk-center intensity. The prominences thus selected are characterized by small non-thermal line broadening and almost absent velocity shifts, yielding narrow line profiles without wiggles. The reduced widths [Δ
λ
D
/
λ
] of He
ii
4686 Å are 1.5 times broader than those of the He
i
4471 Å triplet and 1.65 times broader than those of the He
i
5015 Å singlet. This indicates that the He lines originate in a prominence–corona transition region with outwards increasing temperature. |
| doi_str_mv | 10.1007/s11207-012-0118-2 |
| format | Article |
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ii
4686 Å, is observed together with the He
i
5015 Å singlet and the He
i
4471 Å triplet line in solar prominences. The Na D
2
emission is used as a tracer for He
ii
emissions which are sufficiently bright to exceed the noise level near 10
−6
of the disk-center intensity. The prominences thus selected are characterized by small non-thermal line broadening and almost absent velocity shifts, yielding narrow line profiles without wiggles. The reduced widths [Δ
λ
D
/
λ
] of He
ii
4686 Å are 1.5 times broader than those of the He
i
4471 Å triplet and 1.65 times broader than those of the He
i
5015 Å singlet. This indicates that the He lines originate in a prominence–corona transition region with outwards increasing temperature.</description><identifier>ISSN: 0038-0938</identifier><identifier>EISSN: 1573-093X</identifier><identifier>DOI: 10.1007/s11207-012-0118-2</identifier><language>eng</language><publisher>Dordrecht: Springer Netherlands</publisher><subject>Astrophysics and Astroparticles ; Atmospheric Sciences ; Emission ; Emissions ; Helium ; Line broadening ; Noise levels ; Physics ; Physics and Astronomy ; Solar physics ; Solar prominences ; Space Exploration and Astronautics ; Space Sciences (including Extraterrestrial Physics ; Spectral emissivity ; Spectrum analysis ; Sun ; Tracers</subject><ispartof>Solar physics, 2012-12, Vol.281 (2), p.697-706</ispartof><rights>The Author(s) 2012</rights><rights>Springer Science+Business Media Dordrecht 2012</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><cites>FETCH-LOGICAL-p222t-38e0a7c2f131974220450417d53fa3b49348ce37d4e3891e42ddd849bdfdd1993</cites></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://link.springer.com/content/pdf/10.1007/s11207-012-0118-2$$EPDF$$P50$$Gspringer$$Hfree_for_read</linktopdf><linktohtml>$$Uhttps://link.springer.com/10.1007/s11207-012-0118-2$$EHTML$$P50$$Gspringer$$Hfree_for_read</linktohtml><link.rule.ids>314,780,784,27924,27925,41488,42557,51319</link.rule.ids></links><search><creatorcontrib>Ramelli, R.</creatorcontrib><creatorcontrib>Stellmacher, G.</creatorcontrib><creatorcontrib>Wiehr, E.</creatorcontrib><creatorcontrib>Bianda, M.</creatorcontrib><title>Helium Emissions Observed in Ground-Based Spectra of Solar Prominences</title><title>Solar physics</title><addtitle>Sol Phys</addtitle><description>The only prominent line of singly ionized helium in the visible spectral range, He
ii
4686 Å, is observed together with the He
i
5015 Å singlet and the He
i
4471 Å triplet line in solar prominences. The Na D
2
emission is used as a tracer for He
ii
emissions which are sufficiently bright to exceed the noise level near 10
−6
of the disk-center intensity. The prominences thus selected are characterized by small non-thermal line broadening and almost absent velocity shifts, yielding narrow line profiles without wiggles. The reduced widths [Δ
λ
D
/
λ
] of He
ii
4686 Å are 1.5 times broader than those of the He
i
4471 Å triplet and 1.65 times broader than those of the He
i
5015 Å singlet. This indicates that the He lines originate in a prominence–corona transition region with outwards increasing temperature.</description><subject>Astrophysics and Astroparticles</subject><subject>Atmospheric Sciences</subject><subject>Emission</subject><subject>Emissions</subject><subject>Helium</subject><subject>Line broadening</subject><subject>Noise levels</subject><subject>Physics</subject><subject>Physics and Astronomy</subject><subject>Solar physics</subject><subject>Solar prominences</subject><subject>Space Exploration and Astronautics</subject><subject>Space Sciences (including Extraterrestrial Physics</subject><subject>Spectral emissivity</subject><subject>Spectrum analysis</subject><subject>Sun</subject><subject>Tracers</subject><issn>0038-0938</issn><issn>1573-093X</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2012</creationdate><recordtype>article</recordtype><sourceid>C6C</sourceid><sourceid>ABUWG</sourceid><sourceid>AFKRA</sourceid><sourceid>AZQEC</sourceid><sourceid>BENPR</sourceid><sourceid>CCPQU</sourceid><sourceid>DWQXO</sourceid><sourceid>GNUQQ</sourceid><recordid>eNqFkcFKw0AQhhdRsFYfwFvAi5fozOwmu3vUYluhUKEK3pY0u5GUdBN3G5_fhHoQLx6GmYFvhn_mZ-wa4Q4B5H1EJJApIA2BKqUTNsFM8hQ0fz9lEwCuxlqds4sYdwDjVDZh86Vr6n6fPO3rGOvWx2S9jS58OZvUPlmEtvc2fSzi0G86Vx5CkbRVsmmbIiQvod3X3vnSxUt2VhVNdFc_ecre5k-vs2W6Wi-eZw-rtCOiQ8qVg0KWVCFHLQURiAwESpvxquBboblQpePSCseVRifIWquE3trKWtSaT9ntcW8X2s_exYMZdJeuaQrv2j4azCUKmWeQ_Y9SJmWeA_EBvfmD7to--OEQgyi01lIRDRQdqdiF2n-48IsCM_7THF0wgwtmdMEQ_wbCNXfc</recordid><startdate>20121201</startdate><enddate>20121201</enddate><creator>Ramelli, R.</creator><creator>Stellmacher, G.</creator><creator>Wiehr, E.</creator><creator>Bianda, M.</creator><general>Springer Netherlands</general><general>Springer Nature B.V</general><scope>C6C</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><scope>7TV</scope><scope>C1K</scope></search><sort><creationdate>20121201</creationdate><title>Helium Emissions Observed in Ground-Based Spectra of Solar Prominences</title><author>Ramelli, R. ; Stellmacher, G. ; Wiehr, E. ; Bianda, M.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-p222t-38e0a7c2f131974220450417d53fa3b49348ce37d4e3891e42ddd849bdfdd1993</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2012</creationdate><topic>Astrophysics and Astroparticles</topic><topic>Atmospheric Sciences</topic><topic>Emission</topic><topic>Emissions</topic><topic>Helium</topic><topic>Line broadening</topic><topic>Noise levels</topic><topic>Physics</topic><topic>Physics and Astronomy</topic><topic>Solar physics</topic><topic>Solar prominences</topic><topic>Space Exploration and Astronautics</topic><topic>Space Sciences (including Extraterrestrial Physics</topic><topic>Spectral emissivity</topic><topic>Spectrum analysis</topic><topic>Sun</topic><topic>Tracers</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Ramelli, R.</creatorcontrib><creatorcontrib>Stellmacher, G.</creatorcontrib><creatorcontrib>Wiehr, E.</creatorcontrib><creatorcontrib>Bianda, M.</creatorcontrib><collection>Springer Nature OA/Free Journals</collection><collection>ProQuest Central (Corporate)</collection><collection>Meteorological & 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 & 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 & Geoastrophysical Abstracts - Academic</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>Science Database</collection><collection>Advanced Technologies & Aerospace Database</collection><collection>ProQuest Advanced Technologies & 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><collection>Pollution Abstracts</collection><collection>Environmental Sciences and Pollution Management</collection><jtitle>Solar physics</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Ramelli, R.</au><au>Stellmacher, G.</au><au>Wiehr, E.</au><au>Bianda, M.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Helium Emissions Observed in Ground-Based Spectra of Solar Prominences</atitle><jtitle>Solar physics</jtitle><stitle>Sol Phys</stitle><date>2012-12-01</date><risdate>2012</risdate><volume>281</volume><issue>2</issue><spage>697</spage><epage>706</epage><pages>697-706</pages><issn>0038-0938</issn><eissn>1573-093X</eissn><abstract>The only prominent line of singly ionized helium in the visible spectral range, He
ii
4686 Å, is observed together with the He
i
5015 Å singlet and the He
i
4471 Å triplet line in solar prominences. The Na D
2
emission is used as a tracer for He
ii
emissions which are sufficiently bright to exceed the noise level near 10
−6
of the disk-center intensity. The prominences thus selected are characterized by small non-thermal line broadening and almost absent velocity shifts, yielding narrow line profiles without wiggles. The reduced widths [Δ
λ
D
/
λ
] of He
ii
4686 Å are 1.5 times broader than those of the He
i
4471 Å triplet and 1.65 times broader than those of the He
i
5015 Å singlet. This indicates that the He lines originate in a prominence–corona transition region with outwards increasing temperature.</abstract><cop>Dordrecht</cop><pub>Springer Netherlands</pub><doi>10.1007/s11207-012-0118-2</doi><tpages>10</tpages><oa>free_for_read</oa></addata></record> |
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| language | eng |
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| subjects | Astrophysics and Astroparticles Atmospheric Sciences Emission Emissions Helium Line broadening Noise levels Physics Physics and Astronomy Solar physics Solar prominences Space Exploration and Astronautics Space Sciences (including Extraterrestrial Physics Spectral emissivity Spectrum analysis Sun Tracers |
| title | Helium Emissions Observed in Ground-Based Spectra of Solar Prominences |
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