Water in Betelgeuse and Antares

Absorption lines of hot water have been identified in the infrared spectra of Betelgeuse (α Orionis) and Antares (α Scorpii) near 12.3 micrometers (811 to 819 wavenumbers). The water lines originate in the atmospheres of the stars, not in their circumstellar material. The spectra are similar in stru...

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Bibliographic Details
Published in:Science (American Association for the Advancement of Science) 1998-02, Vol.279 (5352), p.844-847
Main Authors: Jennings, Donald E., Sada, Pedro V.
Format: Article
Language:English
Subjects:
Absorption spectra
Abundances, chemical composition
Astronomical Phenomena
Astronomy
Climate
Earth, ocean, space
Exact sciences and technology
Extraterrestrial Environment
Laboratories
Life Sciences (General)
Line spectra
Molecules
Normal stars (by class): general or individual
Scientific Concepts
Solar observatories
Space life sciences
Spectrophotometry, Infrared
Stars
Stars & galaxies
Stellar characteristics and properties
Stellar spectra
Stellar spectral lines
Sunspots
Supergiant stars
Telluric lines
Water
Water - analysis
Water temperature
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Summary:Absorption lines of hot water have been identified in the infrared spectra of Betelgeuse (α Orionis) and Antares (α Scorpii) near 12.3 micrometers (811 to 819 wavenumbers). The water lines originate in the atmospheres of the stars, not in their circumstellar material. The spectra are similar in structure to umbral sunspot spectra. Pure rotation water lines of this type will occur throughout the spectra of cool stars at wavelengths greater than 10 micrometers. From the water spectra, the upper limit for the temperature in the line formation region in both stars is 2800 kelvin. The water column density in both stars is (3 ± 2) × 10$^{18}$ molecules per square centimeter, yielding an abundance relative to atomic hydrogen of n(H$_2$O)/n(H) ≈ 10$^{-7}$.
ISSN:0036-8075
1095-9203
DOI:10.1126/science.279.5352.844