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FIP effect for minor heavy solar wind ions as seen with SOHO/CELIAS/MTOF
A recent paper [Shearer et al., 2014] reported that during solar maximum Ne showed a surprisingly low abundance. This leads to the question whether other elements show the same behavior. The good mass resolution of Mass-Time-Of-Flight (MTOF) as part of the Charge ELement and Isotope Analysis System...
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description | A recent paper [Shearer et al., 2014] reported that during solar maximum Ne showed a surprisingly low abundance. This leads to the question whether other elements show the same behavior. The good mass resolution of Mass-Time-Of-Flight (MTOF) as part of the Charge ELement and Isotope Analysis System (CELIAS) on the Solar Helioshperic Observatory (SOHO) allows to investigate the composition of heavy minor elements in different types of solar wind. We restrict this study to slow solar wind, where the characterisation of slow solar wind is taken from Xu and Borovsky, 2014. This classification scheme requires magnet field information. Since SOHO does not carry a magnetometer, we use the Magnetometer (MAG) of the Advanced Composition Explorer (ACE) instead. The Solar Wind Ion Composition Spectrometer (ACE/SWICS) also provides composition data for cross-calibration and charge-state distributions as input for the transmission function of MTOF whenever the two spacecraft can be expected to observe the same type of wind. We illustrate the MTOF’s capability to determine the solar wind abundance compared to the photospheric abundance (called the FIP ratio in the following) for rare elements like Ti or Cr on long-time scales as a proof of concept for our analysis. And in this brief study, measurements with both ACE/SWICS indicate that the observed elements exhibit a (weak) dependence on the solar cycle, whereas the MTOF measurements are inconclusive. |
doi_str_mv | 10.1063/1.4943815 |
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This leads to the question whether other elements show the same behavior. The good mass resolution of Mass-Time-Of-Flight (MTOF) as part of the Charge ELement and Isotope Analysis System (CELIAS) on the Solar Helioshperic Observatory (SOHO) allows to investigate the composition of heavy minor elements in different types of solar wind. We restrict this study to slow solar wind, where the characterisation of slow solar wind is taken from Xu and Borovsky, 2014. This classification scheme requires magnet field information. Since SOHO does not carry a magnetometer, we use the Magnetometer (MAG) of the Advanced Composition Explorer (ACE) instead. The Solar Wind Ion Composition Spectrometer (ACE/SWICS) also provides composition data for cross-calibration and charge-state distributions as input for the transmission function of MTOF whenever the two spacecraft can be expected to observe the same type of wind. We illustrate the MTOF’s capability to determine the solar wind abundance compared to the photospheric abundance (called the FIP ratio in the following) for rare elements like Ti or Cr on long-time scales as a proof of concept for our analysis. And in this brief study, measurements with both ACE/SWICS indicate that the observed elements exhibit a (weak) dependence on the solar cycle, whereas the MTOF measurements are inconclusive.</description><identifier>ISSN: 0094-243X</identifier><identifier>EISSN: 1551-7616</identifier><identifier>DOI: 10.1063/1.4943815</identifier><identifier>CODEN: APCPCS</identifier><language>eng</language><publisher>Melville: American Institute of Physics</publisher><subject>Abundance ; Advanced Composition Explorer ; ASTROPHYSICS ; CALIBRATION ; Charge distribution ; CHARGE STATES ; CHROMIUM ; CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS ; COMPARATIVE EVALUATIONS ; Composition ; Dependence ; INSTRUMENTATION RELATED TO NUCLEAR SCIENCE AND TECHNOLOGY ; MAGNETIC SPECTROMETERS ; MAGNETOMETERS ; MASS ; MASS RESOLUTION ; PHOTOSPHERE ; SOLAR CYCLE ; Solar maximum ; SOLAR WIND ; SPACE VEHICLES ; TIME-OF-FLIGHT METHOD</subject><ispartof>AIP Conference Proceedings, 2016, Vol.1720 (1)</ispartof><rights>AIP Publishing LLC</rights><rights>2016 AIP Publishing LLC.</rights><lds50>peer_reviewed</lds50><woscitedreferencessubscribed>false</woscitedreferencessubscribed></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>230,310,311,315,786,790,795,796,891,23958,23959,25170,27957,27958</link.rule.ids><backlink>$$Uhttps://www.osti.gov/biblio/22590905$$D View this record in Osti.gov$$Hfree_for_read</backlink></links><search><contributor>Möbius, Eberhard</contributor><contributor>Wang, Linghua</contributor><contributor>Bruno, Roberto</contributor><contributor>Zank, Gary</contributor><contributor>Vourlidas, Angelos</contributor><creatorcontrib>Heidrich-Meisner, Verena</creatorcontrib><creatorcontrib>Berger, Lars</creatorcontrib><creatorcontrib>Wimmer-Schweingruber, Robert F.</creatorcontrib><creatorcontrib>Wurz, Peter</creatorcontrib><creatorcontrib>Bochsler, Peter</creatorcontrib><creatorcontrib>Ipavich, Fred M.</creatorcontrib><creatorcontrib>Paquette, John A.</creatorcontrib><creatorcontrib>Klecker, Bernd</creatorcontrib><title>FIP effect for minor heavy solar wind ions as seen with SOHO/CELIAS/MTOF</title><title>AIP Conference Proceedings</title><description>A recent paper [Shearer et al., 2014] reported that during solar maximum Ne showed a surprisingly low abundance. This leads to the question whether other elements show the same behavior. The good mass resolution of Mass-Time-Of-Flight (MTOF) as part of the Charge ELement and Isotope Analysis System (CELIAS) on the Solar Helioshperic Observatory (SOHO) allows to investigate the composition of heavy minor elements in different types of solar wind. We restrict this study to slow solar wind, where the characterisation of slow solar wind is taken from Xu and Borovsky, 2014. This classification scheme requires magnet field information. Since SOHO does not carry a magnetometer, we use the Magnetometer (MAG) of the Advanced Composition Explorer (ACE) instead. The Solar Wind Ion Composition Spectrometer (ACE/SWICS) also provides composition data for cross-calibration and charge-state distributions as input for the transmission function of MTOF whenever the two spacecraft can be expected to observe the same type of wind. We illustrate the MTOF’s capability to determine the solar wind abundance compared to the photospheric abundance (called the FIP ratio in the following) for rare elements like Ti or Cr on long-time scales as a proof of concept for our analysis. And in this brief study, measurements with both ACE/SWICS indicate that the observed elements exhibit a (weak) dependence on the solar cycle, whereas the MTOF measurements are inconclusive.</description><subject>Abundance</subject><subject>Advanced Composition Explorer</subject><subject>ASTROPHYSICS</subject><subject>CALIBRATION</subject><subject>Charge distribution</subject><subject>CHARGE STATES</subject><subject>CHROMIUM</subject><subject>CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS</subject><subject>COMPARATIVE EVALUATIONS</subject><subject>Composition</subject><subject>Dependence</subject><subject>INSTRUMENTATION RELATED TO NUCLEAR SCIENCE AND TECHNOLOGY</subject><subject>MAGNETIC SPECTROMETERS</subject><subject>MAGNETOMETERS</subject><subject>MASS</subject><subject>MASS RESOLUTION</subject><subject>PHOTOSPHERE</subject><subject>SOLAR CYCLE</subject><subject>Solar maximum</subject><subject>SOLAR WIND</subject><subject>SPACE VEHICLES</subject><subject>TIME-OF-FLIGHT METHOD</subject><issn>0094-243X</issn><issn>1551-7616</issn><fulltext>true</fulltext><rsrctype>conference_proceeding</rsrctype><creationdate>2016</creationdate><recordtype>conference_proceeding</recordtype><recordid>eNqFkE1rAjEQhkNpodb20H8Q6K2wmsnHZnMU0SpYtqCF3kJ2k-CKbuxmrfjvu6LQYy8zMDzMO_Mg9AxkACRlQxhwxVkG4gb1QAhIZArpLeoRonhCOfu6Rw8xbgihSsqsh2bT-Qd23ruyxT40eFfVXV0783PCMWxNg49VbXEV6ohNxNG5upu0a7zMZ_lwPFnMR8vh-yqfPqI7b7bRPV17H31OJ6vxLFnkb_PxaJEEKnmbeKoKSpgqjLGMS-kYzZgnVmSegE1taZVIwaXEcu-FkbwQBQOwjnGjnJWsj14ue0NsKx3LqnXlugx13X2gKRWKKCL-qH0Tvg8utnoTDk3dHaYpUMhEqjj_l2Iyy86JrxfqHGbaToXeN9XONCcNRJ-ta9BX6-wX-sxvtw</recordid><startdate>20160325</startdate><enddate>20160325</enddate><creator>Heidrich-Meisner, Verena</creator><creator>Berger, Lars</creator><creator>Wimmer-Schweingruber, Robert F.</creator><creator>Wurz, Peter</creator><creator>Bochsler, Peter</creator><creator>Ipavich, Fred M.</creator><creator>Paquette, John A.</creator><creator>Klecker, Bernd</creator><general>American Institute of Physics</general><scope>8FD</scope><scope>H8D</scope><scope>L7M</scope><scope>OTOTI</scope></search><sort><creationdate>20160325</creationdate><title>FIP effect for minor heavy solar wind ions as seen with SOHO/CELIAS/MTOF</title><author>Heidrich-Meisner, Verena ; Berger, Lars ; Wimmer-Schweingruber, Robert F. ; Wurz, Peter ; Bochsler, Peter ; Ipavich, Fred M. ; Paquette, John A. ; Klecker, Bernd</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-o274t-f29b2039baad3477e3283f0d58f01d6dcd9561e60d4ff5a74b5b311de34a9ed73</frbrgroupid><rsrctype>conference_proceedings</rsrctype><prefilter>conference_proceedings</prefilter><language>eng</language><creationdate>2016</creationdate><topic>Abundance</topic><topic>Advanced Composition Explorer</topic><topic>ASTROPHYSICS</topic><topic>CALIBRATION</topic><topic>Charge distribution</topic><topic>CHARGE STATES</topic><topic>CHROMIUM</topic><topic>CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS</topic><topic>COMPARATIVE EVALUATIONS</topic><topic>Composition</topic><topic>Dependence</topic><topic>INSTRUMENTATION RELATED TO NUCLEAR SCIENCE AND TECHNOLOGY</topic><topic>MAGNETIC SPECTROMETERS</topic><topic>MAGNETOMETERS</topic><topic>MASS</topic><topic>MASS RESOLUTION</topic><topic>PHOTOSPHERE</topic><topic>SOLAR CYCLE</topic><topic>Solar maximum</topic><topic>SOLAR WIND</topic><topic>SPACE VEHICLES</topic><topic>TIME-OF-FLIGHT METHOD</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Heidrich-Meisner, Verena</creatorcontrib><creatorcontrib>Berger, Lars</creatorcontrib><creatorcontrib>Wimmer-Schweingruber, Robert F.</creatorcontrib><creatorcontrib>Wurz, Peter</creatorcontrib><creatorcontrib>Bochsler, Peter</creatorcontrib><creatorcontrib>Ipavich, Fred M.</creatorcontrib><creatorcontrib>Paquette, John A.</creatorcontrib><creatorcontrib>Klecker, Bernd</creatorcontrib><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>OSTI.GOV</collection></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Heidrich-Meisner, Verena</au><au>Berger, Lars</au><au>Wimmer-Schweingruber, Robert F.</au><au>Wurz, Peter</au><au>Bochsler, Peter</au><au>Ipavich, Fred M.</au><au>Paquette, John A.</au><au>Klecker, Bernd</au><format>book</format><genre>proceeding</genre><ristype>CONF</ristype><atitle>FIP effect for minor heavy solar wind ions as seen with SOHO/CELIAS/MTOF</atitle><btitle>AIP Conference Proceedings</btitle><date>2016-03-25</date><risdate>2016</risdate><volume>1720</volume><issue>1</issue><issn>0094-243X</issn><eissn>1551-7616</eissn><coden>APCPCS</coden><abstract>A recent paper [Shearer et al., 2014] reported that during solar maximum Ne showed a surprisingly low abundance. This leads to the question whether other elements show the same behavior. The good mass resolution of Mass-Time-Of-Flight (MTOF) as part of the Charge ELement and Isotope Analysis System (CELIAS) on the Solar Helioshperic Observatory (SOHO) allows to investigate the composition of heavy minor elements in different types of solar wind. We restrict this study to slow solar wind, where the characterisation of slow solar wind is taken from Xu and Borovsky, 2014. This classification scheme requires magnet field information. Since SOHO does not carry a magnetometer, we use the Magnetometer (MAG) of the Advanced Composition Explorer (ACE) instead. The Solar Wind Ion Composition Spectrometer (ACE/SWICS) also provides composition data for cross-calibration and charge-state distributions as input for the transmission function of MTOF whenever the two spacecraft can be expected to observe the same type of wind. We illustrate the MTOF’s capability to determine the solar wind abundance compared to the photospheric abundance (called the FIP ratio in the following) for rare elements like Ti or Cr on long-time scales as a proof of concept for our analysis. And in this brief study, measurements with both ACE/SWICS indicate that the observed elements exhibit a (weak) dependence on the solar cycle, whereas the MTOF measurements are inconclusive.</abstract><cop>Melville</cop><pub>American Institute of Physics</pub><doi>10.1063/1.4943815</doi><tpages>4</tpages></addata></record> |
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subjects | Abundance Advanced Composition Explorer ASTROPHYSICS CALIBRATION Charge distribution CHARGE STATES CHROMIUM CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS COMPARATIVE EVALUATIONS Composition Dependence INSTRUMENTATION RELATED TO NUCLEAR SCIENCE AND TECHNOLOGY MAGNETIC SPECTROMETERS MAGNETOMETERS MASS MASS RESOLUTION PHOTOSPHERE SOLAR CYCLE Solar maximum SOLAR WIND SPACE VEHICLES TIME-OF-FLIGHT METHOD |
title | FIP effect for minor heavy solar wind ions as seen with SOHO/CELIAS/MTOF |
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