uu.seUppsala University Publications
Change search
CiteExportLink to record
Permanent link

Direct link
Cite
Citation style
  • apa
  • ieee
  • modern-language-association
  • vancouver
  • Other style
More styles
Language
  • de-DE
  • en-GB
  • en-US
  • fi-FI
  • nn-NO
  • nn-NB
  • sv-SE
  • Other locale
More languages
Output format
  • html
  • text
  • asciidoc
  • rtf
Water Vapor on Supergiants: The 12 μm TEXES Spectra of μ Cephei
Uppsala University, Disciplinary Domain of Science and Technology, Physics, Department of Astronomy and Space Physics. Uppsala University, Disciplinary Domain of Science and Technology, Physics, Astronomical observatory.
Uppsala University, Disciplinary Domain of Science and Technology, Physics, Department of Astronomy and Space Physics. Uppsala University, Disciplinary Domain of Science and Technology, Physics, Astronomical observatory.
Show others and affiliations
2006 (English)In: Astrophysical Journal, ISSN 0004-637X, E-ISSN 1538-4357, Vol. 645, no 1, 652-658 p.Article in journal (Refereed) Published
Abstract [en]

Several recent papers have argued for warm, semidetached, molecular layers surrounding red giant and supergiant stars, a concept known as a MOLsphere. Spectroscopic and interferometric analyses have often corroborated this general picture. Here we present high-resolution spectroscopic data of pure rotational lines of water vapor at 12 mu m for the supergiant mu Cep. This star has often been used to test the concept of molecular layers around supergiants. Given the prediction of an isothermal, optically thick water vapor layer in local thermodynamic equilibrium around the star ( MOLsphere), we expected the 12 mu m lines to be in emission or at least in absorption but filled in by emission from the molecular layer around the star. Our data, however, show the contrary; we find definite absorption. Thus, our data do not easily fit into the suggested isothermal MOLsphere scenario. The 12 mu m lines, therefore, put new, strong constraints on the MOLsphere concept and on the nature of water seen in signatures across the spectra of early M supergiants. We also find that the absorption is even stronger than that calculated from a standard, spherically symmetric model photosphere without any surrounding layers. A cool model photosphere, representing cool outer layers, is, however, able to reproduce the lines, but this model does not account for water vapor emission at 6 mu m. Thus, a unified model for water vapor on mu Cep appears to be lacking. It does seem necessary to model the underlying photospheres of these supergiants in their whole complexity. The strong water vapor lines clearly reveal inadequacies of classical model atmospheres.

Place, publisher, year, edition, pages
2006. Vol. 645, no 1, 652-658 p.
Keyword [en]
infrared : stars; stars : atmospheres; stars : individual (mu Cephei)
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
URN: urn:nbn:se:uu:diva-22077DOI: 10.1086/504287ISI: 000238832900053OAI: oai:DiVA.org:uu-22077DiVA: diva2:49850
Available from: 2007-01-10 Created: 2007-01-10 Last updated: 2017-12-07Bibliographically approved

Open Access in DiVA

No full text

Other links

Publisher's full text

Authority records BETA

Ryde, NilsEriksson, Kjell

Search in DiVA

By author/editor
Ryde, NilsEriksson, Kjell
By organisation
Department of Astronomy and Space PhysicsAstronomical observatory
In the same journal
Astrophysical Journal
Astronomy, Astrophysics and Cosmology

Search outside of DiVA

GoogleGoogle Scholar

doi
urn-nbn

Altmetric score

doi
urn-nbn
Total: 357 hits
CiteExportLink to record
Permanent link

Direct link
Cite
Citation style
  • apa
  • ieee
  • modern-language-association
  • vancouver
  • Other style
More styles
Language
  • de-DE
  • en-GB
  • en-US
  • fi-FI
  • nn-NO
  • nn-NB
  • sv-SE
  • Other locale
More languages
Output format
  • html
  • text
  • asciidoc
  • rtf