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Detection of Water Vapor in the Photosphere of Arcturus
We report detections of pure rotation lines of OH and H2O in the K1.5 III red-giant star Arcturus (α Bootis) using high-resolution, infrared spectra covering the regions 806 −822cm −1 (12.2 −12.4 µm)Expand
Texes Observations of M Supergiants: Dynamics and Thermodynamics of Wind Acceleration
We have detected [Fe II] 17.94 μm and 24.52 μm emission from a sample of M supergiants (μ Cep, α Sco, α Ori, CE Tau, AD Per, and α Her) using the Texas Echelon Cross Echelle Spectrograph on NASA'sExpand
Mg I emission lines at 12 and 18 mu m in K giants
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.Expand
FLUORINE IN THE SOLAR NEIGHBORHOOD: IS IT ALL PRODUCED IN ASYMPTOTIC GIANT BRANCH STARS?
The origin of cosmic fluorine is uncertain, but there are three proposed production sites/mechanisms for the origin: asymptotic giant branch (AGB) stars, ν nucleosynthesis in Type II supernovae,Expand
[S IV] IN THE NGC 5253 SUPERNEBULA: IONIZED GAS KINEMATICS AT HIGH RESOLUTION
The nearby dwarf starburst galaxy NGC 5253 hosts a deeply embedded radio-infrared supernebula excited by thousands of O stars. We have observed this source in the 10.5 {mu}m line of S{sup +3} at 3.8Expand
Water Vapor on Betelgeuse as Revealed by TEXES
The outer atmosphere of the M supergiant Betelgeuse is puzzling. Published observations of different kinds have shed light on different aspects of the atmosphere, but no unified picture has emerged.Expand
SOFIA-EXES Mid-IR Observations of [Fe II] Emission from the Extended Atmosphere of Betelgeuse
We present a NASA-DLR SOFIA-Echelon Cross Echelle Spectrograph (EXES) and NASA Infrared Telescope Facility-Texas Echelon Cross Echelle Spectrograph (TEXES) mid-IR R ≃ 50,000 spectral study ofExpand
Nonthermal Mg I Emission at 12 Micron from Procyon
We report on stellar Mg I emission at 12 μm from α CMi (Procyon), a star slightly hotter than the Sun. Solar Mg I emission is well known, and its formation was successfully explained in detail byExpand
Water vapor on supergiants : The 12 μm texes spectra of μ cephei
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 haveExpand
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