A potential new method for determining the temperature of cool stars
arXiv:0805.3297 · doi:10.1111/j.1365-2966.2008.13489.x
Abstract
We present high resolution (R = 90,000) mid-infrared spectra of M dwarfs. The mid infrared region of the spectra of cool low mass stars contain pure rotational water vapour transitions that may provide us with a new methodology in the determination of the effective temperatures for low mass stars. We identify and assign water transitions in these spectra and determine how sensitive each pure rotational water transition is to small (25 K) changes in effective temperature. We find that, of the 36 confirmed and assigned pure rotational water transitions, at least 10 should be sensitive enough to be used as temperature indicators.
accepted by MNRAS
References in corpus (9)
- A high accuracy computed water line list
- An Infrared Spectroscopic Sequence of M, L and T Dwarfs
- Infrared Spectra and Spectral Energy Distributions of Late-M- and L-Dwarfs
- TEXES: A Sensitive High-Resolution Grating Spectrograph for the Mid-Infrared
- Spectral Energy Distributions for Disk and Halo M--Dwarfs
- TiO and HO absorption lines in cool stellar atmospheres
- Spectral analysis of water vapour in cool stars
- Carbon Monoxide in low-mass dwarf stars
- Water vapor on supergiants. The 12 micron TEXES spectra of mu Cephei