HIGH-ACCURACY MR-MP PERTURBATION THEORY ENERGY AND RADIATIVE RATES CALCULATIONS FOR CORE-EXCITED TRANSITIONS IN Fe XVI
Accurate theoretical energy level, lifetime, and transition probability calculations of core-excited Fe XVI were performed employing the relativistic Multireference Moller-Plesset perturbation theory. In these computations the term energies of the highly excited n [< or =, slant] 5 states arising...
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description | Accurate theoretical energy level, lifetime, and transition probability calculations of core-excited Fe XVI were performed employing the relativistic Multireference Moller-Plesset perturbation theory. In these computations the term energies of the highly excited n [< or =, slant] 5 states arising from the configuration 1s super(2)2s super(k)2p super(m)3l super(p)nl super('q ), where k + m + p + q = 9, l [< or =, slant] 3 and p + q [< or =, slant] 2 are considered, including those of the autoionizing levels with a hole-state in the L-shell. All even and odd parity states of sodium-like iron ion were included for a total of 1784 levels. Comparison of the calculated L-shell transition wavelengths with those from laboratory measurements shows excellent agreement. Therefore, our calculation may be used to predict the wavelengths of as of yet unobserved Fe XVI, such as the second strongest 2p-3d Fe XVI line, which has not been directly observed in the laboratory and which blends with one of the prominent Fe XVII lines. |
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In these computations the term energies of the highly excited n [< or =, slant] 5 states arising from the configuration 1s super(2)2s super(k)2p super(m)3l super(p)nl super('q ), where k + m + p + q = 9, l [< or =, slant] 3 and p + q [< or =, slant] 2 are considered, including those of the autoionizing levels with a hole-state in the L-shell. All even and odd parity states of sodium-like iron ion were included for a total of 1784 levels. Comparison of the calculated L-shell transition wavelengths with those from laboratory measurements shows excellent agreement. Therefore, our calculation may be used to predict the wavelengths of as of yet unobserved Fe XVI, such as the second strongest 2p-3d Fe XVI line, which has not been directly observed in the laboratory and which blends with one of the prominent Fe XVII lines.</description><identifier>ISSN: 0067-0049</identifier><identifier>EISSN: 1538-4365</identifier><identifier>DOI: 10.1088/0067-0049/207/1/11</identifier><language>eng</language><publisher>United States</publisher><subject>ACCURACY ; ASTROPHYSICS ; ASTROPHYSICS, COSMOLOGY AND ASTRONOMY ; ATOMIC AND MOLECULAR PHYSICS ; Blends ; CALCULATION METHODS ; COMPARATIVE EVALUATIONS ; ENERGY LEVELS ; ENERGY-LEVEL TRANSITIONS ; GAMMA RADIATION ; HOLES ; Iron ; IRON IONS ; L SHELL ; LIFETIME ; Mathematical analysis ; MULTICHARGED IONS ; PARITY ; PERTURBATION THEORY ; Polymer blends ; PROBABILITY ; RELATIVISTIC RANGE ; SODIUM ; STELLAR CORONAE ; Wavelengths ; X RADIATION</subject><ispartof>The Astrophysical journal. 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Supplement series</title><description>Accurate theoretical energy level, lifetime, and transition probability calculations of core-excited Fe XVI were performed employing the relativistic Multireference Moller-Plesset perturbation theory. In these computations the term energies of the highly excited n [< or =, slant] 5 states arising from the configuration 1s super(2)2s super(k)2p super(m)3l super(p)nl super('q ), where k + m + p + q = 9, l [< or =, slant] 3 and p + q [< or =, slant] 2 are considered, including those of the autoionizing levels with a hole-state in the L-shell. All even and odd parity states of sodium-like iron ion were included for a total of 1784 levels. Comparison of the calculated L-shell transition wavelengths with those from laboratory measurements shows excellent agreement. Therefore, our calculation may be used to predict the wavelengths of as of yet unobserved Fe XVI, such as the second strongest 2p-3d Fe XVI line, which has not been directly observed in the laboratory and which blends with one of the prominent Fe XVII lines.</description><subject>ACCURACY</subject><subject>ASTROPHYSICS</subject><subject>ASTROPHYSICS, COSMOLOGY AND ASTRONOMY</subject><subject>ATOMIC AND MOLECULAR PHYSICS</subject><subject>Blends</subject><subject>CALCULATION METHODS</subject><subject>COMPARATIVE EVALUATIONS</subject><subject>ENERGY LEVELS</subject><subject>ENERGY-LEVEL TRANSITIONS</subject><subject>GAMMA RADIATION</subject><subject>HOLES</subject><subject>Iron</subject><subject>IRON IONS</subject><subject>L SHELL</subject><subject>LIFETIME</subject><subject>Mathematical analysis</subject><subject>MULTICHARGED IONS</subject><subject>PARITY</subject><subject>PERTURBATION THEORY</subject><subject>Polymer blends</subject><subject>PROBABILITY</subject><subject>RELATIVISTIC RANGE</subject><subject>SODIUM</subject><subject>STELLAR CORONAE</subject><subject>Wavelengths</subject><subject>X RADIATION</subject><issn>0067-0049</issn><issn>1538-4365</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2013</creationdate><recordtype>article</recordtype><recordid>eNqFkcFO4zAQhi20SHSBF-BkicteQj1xbMfHbOq2kUqC3BTRk1VcRxSVBuIUibfHpYgrpxlpPv2amQ-hKyA3QNJ0SAgXESGJHMZEDGEIcIIGwGgaJZSzP2jwA5yhv94_E0IEo3KA3qfFZBpleb7QWb7Etzq6vcN3StcL_T-ri6rE9VRVeolVqfRkibNyhHU2KsLsXoWuVnOcZ7N8Mfui53hcaZxXWkXqIS9qNcK1zsp5cRwWJR47_HBfXKDTZrX17vK7nqPFWNX5NJpVkyLkRZYC6yNOOdCVi1OaJExK0jzG1iaioSDlWjomYJ2QtWxEYjl3INM4XNUwxxPuGGNreo6uj7mt7zfG203v7JNtdztnexPHACkXJFD_jtRr177tne_Ny8Zbt92udq7dewNcCBm4sMfvKE9jfnhuQOMjarvW-8415rXbvKy6DwPEHKyZgxRzkGKCNQMGgH4CyXV95w</recordid><startdate>20130701</startdate><enddate>20130701</enddate><creator>Diaz, F</creator><creator>VILKAS, M J</creator><creator>Ishikawa, Y</creator><creator>Beiersdorfer, P</creator><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>KL.</scope><scope>8FD</scope><scope>H8D</scope><scope>L7M</scope><scope>OTOTI</scope></search><sort><creationdate>20130701</creationdate><title>HIGH-ACCURACY MR-MP PERTURBATION THEORY ENERGY AND RADIATIVE RATES CALCULATIONS FOR CORE-EXCITED TRANSITIONS IN Fe XVI</title><author>Diaz, F ; VILKAS, M J ; Ishikawa, Y ; Beiersdorfer, P</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c315t-63613ae283445990fb2cc47f3199d9e571d40d9f74c66e1982753f5e646e555d3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2013</creationdate><topic>ACCURACY</topic><topic>ASTROPHYSICS</topic><topic>ASTROPHYSICS, COSMOLOGY AND ASTRONOMY</topic><topic>ATOMIC AND MOLECULAR PHYSICS</topic><topic>Blends</topic><topic>CALCULATION METHODS</topic><topic>COMPARATIVE EVALUATIONS</topic><topic>ENERGY LEVELS</topic><topic>ENERGY-LEVEL TRANSITIONS</topic><topic>GAMMA RADIATION</topic><topic>HOLES</topic><topic>Iron</topic><topic>IRON IONS</topic><topic>L SHELL</topic><topic>LIFETIME</topic><topic>Mathematical analysis</topic><topic>MULTICHARGED IONS</topic><topic>PARITY</topic><topic>PERTURBATION THEORY</topic><topic>Polymer blends</topic><topic>PROBABILITY</topic><topic>RELATIVISTIC RANGE</topic><topic>SODIUM</topic><topic>STELLAR CORONAE</topic><topic>Wavelengths</topic><topic>X RADIATION</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Diaz, F</creatorcontrib><creatorcontrib>VILKAS, M J</creatorcontrib><creatorcontrib>Ishikawa, Y</creatorcontrib><creatorcontrib>Beiersdorfer, P</creatorcontrib><collection>CrossRef</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>OSTI.GOV</collection><jtitle>The Astrophysical journal. Supplement series</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Diaz, F</au><au>VILKAS, M J</au><au>Ishikawa, Y</au><au>Beiersdorfer, P</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>HIGH-ACCURACY MR-MP PERTURBATION THEORY ENERGY AND RADIATIVE RATES CALCULATIONS FOR CORE-EXCITED TRANSITIONS IN Fe XVI</atitle><jtitle>The Astrophysical journal. Supplement series</jtitle><date>2013-07-01</date><risdate>2013</risdate><volume>207</volume><issue>1</issue><spage>1</spage><epage>10</epage><pages>1-10</pages><issn>0067-0049</issn><eissn>1538-4365</eissn><abstract>Accurate theoretical energy level, lifetime, and transition probability calculations of core-excited Fe XVI were performed employing the relativistic Multireference Moller-Plesset perturbation theory. In these computations the term energies of the highly excited n [< or =, slant] 5 states arising from the configuration 1s super(2)2s super(k)2p super(m)3l super(p)nl super('q ), where k + m + p + q = 9, l [< or =, slant] 3 and p + q [< or =, slant] 2 are considered, including those of the autoionizing levels with a hole-state in the L-shell. All even and odd parity states of sodium-like iron ion were included for a total of 1784 levels. Comparison of the calculated L-shell transition wavelengths with those from laboratory measurements shows excellent agreement. Therefore, our calculation may be used to predict the wavelengths of as of yet unobserved Fe XVI, such as the second strongest 2p-3d Fe XVI line, which has not been directly observed in the laboratory and which blends with one of the prominent Fe XVII lines.</abstract><cop>United States</cop><doi>10.1088/0067-0049/207/1/11</doi><tpages>10</tpages><oa>free_for_read</oa></addata></record> |
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subjects | ACCURACY ASTROPHYSICS ASTROPHYSICS, COSMOLOGY AND ASTRONOMY ATOMIC AND MOLECULAR PHYSICS Blends CALCULATION METHODS COMPARATIVE EVALUATIONS ENERGY LEVELS ENERGY-LEVEL TRANSITIONS GAMMA RADIATION HOLES Iron IRON IONS L SHELL LIFETIME Mathematical analysis MULTICHARGED IONS PARITY PERTURBATION THEORY Polymer blends PROBABILITY RELATIVISTIC RANGE SODIUM STELLAR CORONAE Wavelengths X RADIATION |
title | HIGH-ACCURACY MR-MP PERTURBATION THEORY ENERGY AND RADIATIVE RATES CALCULATIONS FOR CORE-EXCITED TRANSITIONS IN Fe XVI |
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