Advanced

HYPERFINE-DEPENDENT gf -VALUES OF Mn i LINES IN THE 1.49–1.80 μm H BAND

Andersson, Martin LU ; Grumer, Jon LU ; Ryde, Nils LU ; Blackwell-Whitehead, Richard LU ; Hutton, R; Zou, Y.; Jönsson, Per and Brage, Tomas LU (2015) In The Astrophysical Journal Supplement Series 216(1).
Abstract
The three Mn I lines at 17325, 17339, and 17349 angstrom are among the 25 strongest lines (log(gf) > 0.5) in the H band. They are all heavily broadened due to hyperfine structure, and the profiles of these lines have so far not been understood. Earlier studies of these lines even suggested that they were blended. In this work, the profiles of these three infrared (IR) lines have been studied theoretically and compared to experimental spectra to assist in the complete understanding of the solar spectrum in the IR. It is shown that the structure of these lines cannot be described in the conventional way using the diagonal A and B hyperfine interaction constants. The off-diagonal hyperfine interaction not only has a large impact on the... (More)
The three Mn I lines at 17325, 17339, and 17349 angstrom are among the 25 strongest lines (log(gf) > 0.5) in the H band. They are all heavily broadened due to hyperfine structure, and the profiles of these lines have so far not been understood. Earlier studies of these lines even suggested that they were blended. In this work, the profiles of these three infrared (IR) lines have been studied theoretically and compared to experimental spectra to assist in the complete understanding of the solar spectrum in the IR. It is shown that the structure of these lines cannot be described in the conventional way using the diagonal A and B hyperfine interaction constants. The off-diagonal hyperfine interaction not only has a large impact on the energies of the hyperfine levels, but also introduces a large intensity redistribution among the hyperfine lines, changing the line profiles dramatically. By performing large-scale calculations of the diagonal and off-diagonal hyperfine interaction and the gf-values between the upper and lower hyperfine levels and using a semi-empirical fitting procedure, we achieved agreement between our synthetic and experimental spectra. Furthermore, we compare our results with observations of stellar spectra. The spectra of the Sun and the K1.5 III red giant star Arcturus were modeled in the relevant region, 1.73-1.74 mu m, using our theoretically predicted gf-values and energies for each individual hyperfine line. Satisfactory fits were obtained and clear improvements were found using our new data compared with the old available Mn I data. A complete list of energies and gf-values for all the 3d(5)4s(S-7)4d e(6)D - 3d(5)4s(S-7)4f w(6)F hyperfine lines are available as supporting material, whereas only the stronger lines are presented and discussed in detail in this paper. (Less)
Please use this url to cite or link to this publication:
author
organization
alternative title
HYPERFINE-DEPENDENT gf -VALUES OF Mn i LINES IN THE 1.49–1.80 μm H BAND
publishing date
type
Contribution to journal
publication status
published
subject
keywords
atomic data, infrared: stars, line: identification, methods: laboratory:, atomic, methods: numerical, stars: abundances
in
The Astrophysical Journal Supplement Series
volume
216
issue
1
pages
9 pages
publisher
University of Chicago Press
external identifiers
  • wos:000348129600002
  • scopus:84921351140
ISSN
0067-0049
DOI
10.1088/0067-0049/216/1/2http://dx.doi.org/10.1088/0067-0049/216/1/2
language
English
LU publication?
yes
id
316c1a50-2573-497f-8cdd-bca81d962409 (old id 5063097)
date added to LUP
2015-02-24 11:57:25
date last changed
2017-04-19 15:16:33
@article{316c1a50-2573-497f-8cdd-bca81d962409,
  abstract     = {The three Mn I lines at 17325, 17339, and 17349 angstrom are among the 25 strongest lines (log(gf) > 0.5) in the H band. They are all heavily broadened due to hyperfine structure, and the profiles of these lines have so far not been understood. Earlier studies of these lines even suggested that they were blended. In this work, the profiles of these three infrared (IR) lines have been studied theoretically and compared to experimental spectra to assist in the complete understanding of the solar spectrum in the IR. It is shown that the structure of these lines cannot be described in the conventional way using the diagonal A and B hyperfine interaction constants. The off-diagonal hyperfine interaction not only has a large impact on the energies of the hyperfine levels, but also introduces a large intensity redistribution among the hyperfine lines, changing the line profiles dramatically. By performing large-scale calculations of the diagonal and off-diagonal hyperfine interaction and the gf-values between the upper and lower hyperfine levels and using a semi-empirical fitting procedure, we achieved agreement between our synthetic and experimental spectra. Furthermore, we compare our results with observations of stellar spectra. The spectra of the Sun and the K1.5 III red giant star Arcturus were modeled in the relevant region, 1.73-1.74 mu m, using our theoretically predicted gf-values and energies for each individual hyperfine line. Satisfactory fits were obtained and clear improvements were found using our new data compared with the old available Mn I data. A complete list of energies and gf-values for all the 3d(5)4s(S-7)4d e(6)D - 3d(5)4s(S-7)4f w(6)F hyperfine lines are available as supporting material, whereas only the stronger lines are presented and discussed in detail in this paper.},
  articleno    = {2},
  author       = {Andersson, Martin and Grumer, Jon and Ryde, Nils and Blackwell-Whitehead, Richard and Hutton, R and Zou, Y. and Jönsson, Per and Brage, Tomas},
  issn         = {0067-0049},
  keyword      = {atomic data,infrared: stars,line: identification,methods: laboratory:,atomic,methods: numerical,stars: abundances},
  language     = {eng},
  month        = {01},
  number       = {1},
  pages        = {9},
  publisher    = {University of Chicago Press},
  series       = {The Astrophysical Journal Supplement Series},
  title        = {HYPERFINE-DEPENDENT gf -VALUES OF Mn i LINES IN THE 1.49–1.80 μm H BAND},
  url          = {http://dx.doi.org/10.1088/0067-0049/216/1/2http://dx.doi.org/10.1088/0067-0049/216/1/2},
  volume       = {216},
  year         = {2015},
}