MEASUREMENT OF THE Fe VIII-Fe XVI 3-3 EMISSION IN THE EXTREME ULTRAVIOLET AND COMPARISON WITH CHIANTI

Beiersdorfer, P; Lepson, J K

doi:10.1088/0067-0049/201/2/28

Title: MEASUREMENT OF THE Fe VIII-Fe XVI 3-3 EMISSION IN THE EXTREME ULTRAVIOLET AND COMPARISON WITH CHIANTI

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Abstract

Laboratory measurements of the n = 3 to n = 3 emission from M-shell iron ions are presented and compared to synthetic spectra from the CHIANTI spectral model. The measurements cover the range 170-290 Angstrom-Sign and are made at an electron density of about 10{sup 11} cm{sup -3}. Emission from Fe VIII through Fe XVI has been identified. Excellent agreement with CHIANTI predictions is found for most lines. Twenty weaker features are noted in the laboratory data that are either absent in CHIANTI or have recently been added and correspond to lines that have not been verified by experimental measurements. A few of these lines may have already been observed (but not yet identified) in the Sun. The features are attributed to emission from various charge states of iron, notably Fe IX and Fe XIII, and two features have been identified as transitions in Fe VIII, i.e., the 3p{sup 6}3d {sup 2}D{sub 5/2}-3p {sup 5}3d{sup 2} {sup 2}P{sub 3/2} and the 3p {sup 6}3d {sup 2}D{sub 3/2}-3p {sup 5}3d{sup 2} {sup 2}P{sub 1/2} transitions at 225.25 {+-} 0.12 and 226.35 {+-} 0.10 Angstrom-Sign , respectively. Seven lines in Fe XI, Fe XII, and Fe XIII between 200 and 205 Angstrom-Signmore »« less

Authors:

Beiersdorfer, P; Lepson, J K ^[1]

Space Sciences Laboratory, University of California, Berkeley, CA 96720 (United States)

Publication Date:: Wed Aug 01 00:00:00 EDT 2012

OSTI Identifier:: 22047611

Resource Type:: Journal Article

Journal Name:: Astrophysical Journal, Supplement Series

Additional Journal Information:: Journal Volume: 201; Journal Issue: 2; Other Information: Country of input: International Atomic Energy Agency (IAEA); Journal ID: ISSN 0067-0049

Country of Publication:: United States

Language:: English

Subject:: 74 ATOMIC AND MOLECULAR PHYSICS; 79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; C CODES; CHARGE STATES; COMPARATIVE EVALUATIONS; COMPUTERIZED SIMULATION; ELECTRON DENSITY; EMISSION SPECTRA; ENERGY-LEVEL TRANSITIONS; EXTREME ULTRAVIOLET RADIATION; GAMMA RADIATION; IRON IONS; M SHELL; MULTICHARGED IONS; SUN; WAVELENGTHS; X RADIATION

Citation Formats


                    Beiersdorfer, P, and Lepson, J K. MEASUREMENT OF THE Fe VIII-Fe XVI 3-3 EMISSION IN THE EXTREME ULTRAVIOLET AND COMPARISON WITH CHIANTI.  United States: N. p., 2012. 
        Web.  doi:10.1088/0067-0049/201/2/28.

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                    Beiersdorfer, P, & Lepson, J K. MEASUREMENT OF THE Fe VIII-Fe XVI 3-3 EMISSION IN THE EXTREME ULTRAVIOLET AND COMPARISON WITH CHIANTI.  United States.  https://doi.org/10.1088/0067-0049/201/2/28

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                    Beiersdorfer, P, and Lepson, J K. 2012.  
        "MEASUREMENT OF THE Fe VIII-Fe XVI 3-3 EMISSION IN THE EXTREME ULTRAVIOLET AND COMPARISON WITH CHIANTI".  United States.  https://doi.org/10.1088/0067-0049/201/2/28.

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@article{osti_22047611,

  title        = {MEASUREMENT OF THE Fe VIII-Fe XVI 3-3 EMISSION IN THE EXTREME ULTRAVIOLET AND COMPARISON WITH CHIANTI},

  author       = {Beiersdorfer, P and Lepson, J K},

  abstractNote = {Laboratory measurements of the n = 3 to n = 3 emission from M-shell iron ions are presented and compared to synthetic spectra from the CHIANTI spectral model. The measurements cover the range 170-290 Angstrom-Sign and are made at an electron density of about 10{sup 11} cm{sup -3}. Emission from Fe VIII through Fe XVI has been identified. Excellent agreement with CHIANTI predictions is found for most lines. Twenty weaker features are noted in the laboratory data that are either absent in CHIANTI or have recently been added and correspond to lines that have not been verified by experimental measurements. A few of these lines may have already been observed (but not yet identified) in the Sun. The features are attributed to emission from various charge states of iron, notably Fe IX and Fe XIII, and two features have been identified as transitions in Fe VIII, i.e., the 3p{sup 6}3d {sup 2}D{sub 5/2}-3p {sup 5}3d{sup 2} {sup 2}P{sub 3/2} and the 3p {sup 6}3d {sup 2}D{sub 3/2}-3p {sup 5}3d{sup 2} {sup 2}P{sub 1/2} transitions at 225.25 {+-} 0.12 and 226.35 {+-} 0.10 Angstrom-Sign , respectively. Seven lines in Fe XI, Fe XII, and Fe XIII between 200 and 205 Angstrom-Sign are noted for which the wavelengths in the CHIANTI database disagree with those in the current database of the National Institute of Standards and Technology. Our measurements of five of these lines appear to agree with the assignments used in CHIANTI.},

  doi          = {10.1088/0067-0049/201/2/28},

  url          = {https://www.osti.gov/biblio/22047611},
  journal      = {Astrophysical Journal, Supplement Series},

  issn         = {0067-0049},

  number       = 2,

  volume       = 201,

  place        = {United States},

  year         = {Wed Aug 01 00:00:00 EDT 2012},

  month        = {Wed Aug 01 00:00:00 EDT 2012}

}

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