IInterpretation of Anomalous Ultraviolet Transitions of Fe II Observed in Laboratory Fourier Transform Spectra and Stellar HST and IUE Spectra
(1995) In Astrophysical Journal 446(1). p.361-370- Abstract
- We discuss LS-forbidden Delta S = 2 transitions of Fe Pi that appear as strong lines in ultraviolet stellar and laboratory spectra. The lines occur because of indirect lever mixing-two close energy levels, w(2)P(3/2) and x(6)P(3/2), are mixed through a third level acting as a catalyst. In transition multiplets, that involve either the w(2)P(3/2) or the x(6)P(3/2) level the normal component is accompanied by a close, parasite component. These components are well resolved in laboratory Fourier transform spectra, from which accurate intensity ratios can be measured. Spectra of the HgMn star chi Lupi, recorded with the Hubble Space Telescope, show the normal and the parasite components resolved for the first time in stellar spectra. These have... (More)
- We discuss LS-forbidden Delta S = 2 transitions of Fe Pi that appear as strong lines in ultraviolet stellar and laboratory spectra. The lines occur because of indirect lever mixing-two close energy levels, w(2)P(3/2) and x(6)P(3/2), are mixed through a third level acting as a catalyst. In transition multiplets, that involve either the w(2)P(3/2) or the x(6)P(3/2) level the normal component is accompanied by a close, parasite component. These components are well resolved in laboratory Fourier transform spectra, from which accurate intensity ratios can be measured. Spectra of the HgMn star chi Lupi, recorded with the Hubble Space Telescope, show the normal and the parasite components resolved for the first time in stellar spectra. These have been used together with laboratory spectra to derive oscillator strengths for four multiplets and the mixing coefficients for the two interacting energy levels. We also provide improved spectroscopic data for all Fe Pi multiplets that include the w(2)P(3/2) and x(6)P(3/2) levels. The level mixing involves the UV 191 multiplet of Fe Pi around 1780 Angstrom, which is shown to have one parasite component. This multiplet is known to be a prominent emission feature in spectra of various objects, e.g., cool star chromospheres and symbiotic stars. As an example, we show IUE spectra of the eclipsing binary 32 Cyg, which provides perfect conditions for fluorescence experiments, and discuss possible excitation mechanisms of UV 191. Based on second-order perturbation theory and multiconfiguration Hartree-Fock calculations, an atomic three-level model is constructed. This model explains the contradiction found when applying first-order perturbation theory, viz., two close energy levels perturbing each other without causing a repulsion. (Less)
Please use this url to cite or link to this publication:
https://lup.lub.lu.se/record/3918956
- author
- Johansson, Sveneric LU ; Brage, Tomas LU ; Leckrone, DS ; Nave, G and Wahlgren, Glenn LU
- publishing date
- 1995
- type
- Contribution to journal
- publication status
- published
- subject
- keywords
- LABORATORY STARS, METHODS, ATOMIC PROCESSES, IDENTIFICATION, LINE, INDIVIDUAL (CHI LUPI, 32 CYGNI), ULTRAVIOLET, STARS
- in
- Astrophysical Journal
- volume
- 446
- issue
- 1
- pages
- 361 - 370
- publisher
- American Astronomical Society
- external identifiers
-
- wos:A1995RF81000035
- scopus:11944264387
- ISSN
- 0004-637X
- DOI
- 10.1086/175795
- language
- English
- LU publication?
- no
- id
- e8e9bac8-4d00-4345-9d1d-e20bf854ae3f (old id 3918956)
- date added to LUP
- 2016-04-01 15:45:09
- date last changed
- 2021-01-03 07:50:59
@article{e8e9bac8-4d00-4345-9d1d-e20bf854ae3f,
abstract = {{We discuss LS-forbidden Delta S = 2 transitions of Fe Pi that appear as strong lines in ultraviolet stellar and laboratory spectra. The lines occur because of indirect lever mixing-two close energy levels, w(2)P(3/2) and x(6)P(3/2), are mixed through a third level acting as a catalyst. In transition multiplets, that involve either the w(2)P(3/2) or the x(6)P(3/2) level the normal component is accompanied by a close, parasite component. These components are well resolved in laboratory Fourier transform spectra, from which accurate intensity ratios can be measured. Spectra of the HgMn star chi Lupi, recorded with the Hubble Space Telescope, show the normal and the parasite components resolved for the first time in stellar spectra. These have been used together with laboratory spectra to derive oscillator strengths for four multiplets and the mixing coefficients for the two interacting energy levels. We also provide improved spectroscopic data for all Fe Pi multiplets that include the w(2)P(3/2) and x(6)P(3/2) levels. The level mixing involves the UV 191 multiplet of Fe Pi around 1780 Angstrom, which is shown to have one parasite component. This multiplet is known to be a prominent emission feature in spectra of various objects, e.g., cool star chromospheres and symbiotic stars. As an example, we show IUE spectra of the eclipsing binary 32 Cyg, which provides perfect conditions for fluorescence experiments, and discuss possible excitation mechanisms of UV 191. Based on second-order perturbation theory and multiconfiguration Hartree-Fock calculations, an atomic three-level model is constructed. This model explains the contradiction found when applying first-order perturbation theory, viz., two close energy levels perturbing each other without causing a repulsion.}},
author = {{Johansson, Sveneric and Brage, Tomas and Leckrone, DS and Nave, G and Wahlgren, Glenn}},
issn = {{0004-637X}},
keywords = {{LABORATORY STARS; METHODS; ATOMIC PROCESSES; IDENTIFICATION; LINE; INDIVIDUAL (CHI LUPI; 32 CYGNI); ULTRAVIOLET; STARS}},
language = {{eng}},
number = {{1}},
pages = {{361--370}},
publisher = {{American Astronomical Society}},
series = {{Astrophysical Journal}},
title = {{IInterpretation of Anomalous Ultraviolet Transitions of Fe II Observed in Laboratory Fourier Transform Spectra and Stellar HST and IUE Spectra}},
url = {{http://dx.doi.org/10.1086/175795}},
doi = {{10.1086/175795}},
volume = {{446}},
year = {{1995}},
}