Exploring the stellar properties of M dwarfs with high-resolution spectroscopy from the optical to the near-infrared

@article{Rajpurohit2018ExploringTS,
  title={Exploring the stellar properties of M dwarfs with high-resolution spectroscopy from the optical to the near-infrared},
  author={Arvind Singh Rajpurohit and France Allard and Sangeeta Rajpurohit and R Sharma and Guilherme Teixeira and Olivier Mousis and Kamlesh Rajpurohit},
  journal={Astronomy \& Astrophysics},
  year={2018}
}
Context. Being the most numerous and oldest stars in the galaxy, M dwarfs are objects of great interest for exoplanet searches. The presence of molecules in their atmosphere complicates our understanding of their atmospheric properties. But great advances have recently been made in the modeling of M dwarfs due to the revision of solar abundances. Aims. We aim to determine stellar parameters of M dwarfs using high resolution spectra (R ∼ 90 000) simultaneously in the visible and the near… 
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References

SHOWING 1-10 OF 61 REFERENCES
Photospheric properties and fundamental parameters of M dwarfs
M dwarfs are an important source of information when studying and probing the lower end of the Hertzsprung-Russell (HR) diagram, down to the hydrogen-burning limit. Being the most numerous and oldest
The effective temperature scale of M dwarfs
Context. Despite their large number in the Galaxy, M dwarfs remain elusive objects and the modeling of their photospheres has long remained a challenge (molecular opacities, dust cloud formation).
Spectral energy distribution of M-subdwarfs: A study of their atmospheric properties
Context. M-type subdwarfs are metal-poor low-mass stars and probe for the old populations in our Galaxy. Accurate knowledge of their atmospheric parameters and especially the composition is essential
MODEL ATMOSPHERES OF VERY LOW MASS STARS AND BROWN DWARFS
▪ Abstract As progressively cooler stellar and substellar objects are discovered, the presence first of molecules and then of condensed particulates greatly complicates the understanding of their
The CARMENES search for exoplanets around M dwarfs
Context. The new CARMENES instrument comprises two high-resolution and high-stability spectrographs that are used to search for habitable planets around M dwarfs in the visible and near-infrared
PROSPECTING IN ULTRACOOL DWARFS: MEASURING THE METALLICITIES OF MID- AND LATE-M DWARFS
Metallicity is a fundamental parameter that contributes to the physical characteristics of a star. The low temperatures and complex molecules present in M dwarf atmospheres make it difficult to
High-resolution spectroscopic atlas of M subdwarfs. Effective temperature and metallicity
Context. M subdwarfs are metal poor and cool stars. They are important probes of the old galactic populations. However, they remain elusive due to their low luminosity. Observational and modeling
Fundamental M-dwarf parameters from high-resolution spectra using PHOENIX ACES models: I. Parameter accuracy and benchmark stars
M-dwarf stars are the most numerous stars in the Universe; they span a wide range in mass and are in the focus of ongoing and planned exoplanet surveys. To investigate and understand their physical
High-resolution spectra of very low-mass stars
We present the results of high-resolution (1–0.4 A) optical spectroscopy of a sample of very low-mass stars. These data are used to examine the kinematics of the stars at the bottom of the
M dwarfs: effective temperatures, radii and metallicities
We empirically determine effective temperatures and bolometric luminosities for a large sample of nearby M dwarfs, for which high accuracy optical and infrared photometry is available. We introduce a
...
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4
5
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