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Mg I emission lines at 12 and 18 mu m in K giants

Sundqvist, J. O.; Ryde, Nils LU ; Harper, G. M.; Kruger, A. and Richter, M. J. (2008) In Astronomy & Astrophysics 486(3). p.985-993
Abstract
Context. The solar mid-infrared metallic emission lines have already been observed and analyzed well, and the formation scenario of the Mg I 12 mu m lines has been known for more than a decade. Detections of stellar emission at 12 mu m have, however, been limited to Mg I in very few objects. Previous modeling attempts have been made only for Procyon and two cool evolved stars, with unsatisfactory results for the latter. This prevents the lines' long predicted usage as probes of stellar magnetic fields. Aims. We want to explain our observed Mg I emission lines at 12 mu m in the K giants Pollux, Arcturus, and Aldebaran and at 18 mu m in Pollux and Arcturus. We discuss our modeling of these lines and particularly how various aspects of the... (More)
Context. The solar mid-infrared metallic emission lines have already been observed and analyzed well, and the formation scenario of the Mg I 12 mu m lines has been known for more than a decade. Detections of stellar emission at 12 mu m have, however, been limited to Mg I in very few objects. Previous modeling attempts have been made only for Procyon and two cool evolved stars, with unsatisfactory results for the latter. This prevents the lines' long predicted usage as probes of stellar magnetic fields. Aims. We want to explain our observed Mg I emission lines at 12 mu m in the K giants Pollux, Arcturus, and Aldebaran and at 18 mu m in Pollux and Arcturus. We discuss our modeling of these lines and particularly how various aspects of the model atom affect the emergent line profiles. Methods. High-resolution observational spectra were obtained using TEXES at Gemini North and the IRTF. To produce synthetic line spectra, we employed standard one-dimensional, plane-parallel, non-LTE modeling for trace elements in cool stellar atmospheres. We computed model atmospheres with the MARCS code, applied a comprehensive magnesium model atom, and used the radiative transfer code MULTI to solve for the magnesium occupation numbers in statistical equilibrium. Results. The Mg I emission lines at 12 mu m in the K giants are stronger than in the dwarfs observed so far. We present the first observed stellar emission lines from Mg I at 18 mu m and from Al I, Si I, and presumably Ca I at 12 mu m. We successfully reproduce the observed Mg I emission lines simultaneously in the giants and in the Sun, but show how the computed line profiles depend critically on atomic data input and how the inclusion of energy levels with n >= 10 and collisions with neutral hydrogen are necessary to obtain reasonable fits. (Less)
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author
organization
publishing date
type
Contribution to journal
publication status
published
subject
keywords
stars : individual :, Arcturus, stars : individual : Aldebaran, formation, stars : late-type, line :, stars : atmospheres, stars : individual : Pollux
in
Astronomy & Astrophysics
volume
486
issue
3
pages
985 - 993
publisher
EDP Sciences
external identifiers
  • wos:000258326500039
  • scopus:47749104525
ISSN
0004-6361
DOI
10.1051/0004-6361:200809778
language
English
LU publication?
yes
id
55f53e19-37e8-4b0d-b9f2-12703f17da19 (old id 1252948)
date added to LUP
2008-10-31 09:33:24
date last changed
2017-10-08 04:08:44
@article{55f53e19-37e8-4b0d-b9f2-12703f17da19,
  abstract     = {Context. The solar mid-infrared metallic emission lines have already been observed and analyzed well, and the formation scenario of the Mg I 12 mu m lines has been known for more than a decade. Detections of stellar emission at 12 mu m have, however, been limited to Mg I in very few objects. Previous modeling attempts have been made only for Procyon and two cool evolved stars, with unsatisfactory results for the latter. This prevents the lines' long predicted usage as probes of stellar magnetic fields. Aims. We want to explain our observed Mg I emission lines at 12 mu m in the K giants Pollux, Arcturus, and Aldebaran and at 18 mu m in Pollux and Arcturus. We discuss our modeling of these lines and particularly how various aspects of the model atom affect the emergent line profiles. Methods. High-resolution observational spectra were obtained using TEXES at Gemini North and the IRTF. To produce synthetic line spectra, we employed standard one-dimensional, plane-parallel, non-LTE modeling for trace elements in cool stellar atmospheres. We computed model atmospheres with the MARCS code, applied a comprehensive magnesium model atom, and used the radiative transfer code MULTI to solve for the magnesium occupation numbers in statistical equilibrium. Results. The Mg I emission lines at 12 mu m in the K giants are stronger than in the dwarfs observed so far. We present the first observed stellar emission lines from Mg I at 18 mu m and from Al I, Si I, and presumably Ca I at 12 mu m. We successfully reproduce the observed Mg I emission lines simultaneously in the giants and in the Sun, but show how the computed line profiles depend critically on atomic data input and how the inclusion of energy levels with n >= 10 and collisions with neutral hydrogen are necessary to obtain reasonable fits.},
  author       = {Sundqvist, J. O. and Ryde, Nils and Harper, G. M. and Kruger, A. and Richter, M. J.},
  issn         = {0004-6361},
  keyword      = {stars : individual :,Arcturus,stars : individual : Aldebaran,formation,stars : late-type,line :,stars : atmospheres,stars : individual : Pollux},
  language     = {eng},
  number       = {3},
  pages        = {985--993},
  publisher    = {EDP Sciences},
  series       = {Astronomy & Astrophysics},
  title        = {Mg I emission lines at 12 and 18 mu m in K giants},
  url          = {http://dx.doi.org/10.1051/0004-6361:200809778},
  volume       = {486},
  year         = {2008},
}