Spatially resolved spectroscopy across stellar surfaces

@article{Dravins2018SpatiallyRS,
  title={Spatially resolved spectroscopy across stellar surfaces},
  author={Dainis Dravins and Hans-G. Ludwig and Bernd Freytag},
  journal={Astronomy \& Astrophysics},
  year={2018},
  volume={649},
  pages={A16}
}
Context. High-precision stellar analyses require hydrodynamic 3D modeling. Such models predict changes across stellar disks of spectral line shapes, asymmetries, and wavelength shifts. For testing models in stars other than the Sun, spatially resolved observations are feasible from differential spectroscopy during exoplanet transits, retrieving spectra of those stellar surface segments that successively become hidden behind the transiting planet, as demonstrated in Papers I, II, and III. Aims… 

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References

SHOWING 1-10 OF 213 REFERENCES

Spatially resolved spectroscopy across stellar surfaces : I. Using exoplanet transits to analyze 3D stellar atmospheres

Context. High-precision stellar analyses require hydrodynamic modeling to interpret chemical abundances or oscillation modes. Exoplanet atmosphere studies require stellar background spectra to be

Spatially resolved spectroscopy across stellar surfaces: II. High-resolution spectra across HD 209458 (G0 V)

Context. High-resolution spectroscopy across spatially resolved stellar surfaces aims at obtaining spectral-line profiles that are free from rotational broadening; the gradual changes of these

The Stagger-grid: A grid of 3D stellar atmosphere models V. Synthetic stellar spectra and broad-band photometry

Context. The surface structures and dynamics of cool stars are characterized by the presence of convective motions and turbulent flows which shape the emergent spectrum. Aims. We used realistic

Planet and star synergy at high-spectral resolution. A rationale for the characterization of exoplanet atmospheres

Context. Spectroscopy of exoplanet atmospheres at high-resolving powers is rapidly gaining popularity for measuring the presence of atomic and molecular species. While this technique is particularly

Granulation in K-type dwarf stars I. Spectroscopic observations

Aims. We seek to detect and quantify the effects of surface convection (granulation) on the line spectra of K-dwarfs as a first step towards a rigorous testing of hydrodynamic models for their

Precise Radial Velocities of Cool Low-mass Stars with iSHELL

The coolest dwarf stars are intrinsically faint at visible wavelengths and exhibit rotationally modulated stellar activity from spots and plages. It is advantageous to observe these stars at

New light on stellar abundance analyses: Departures from LTE and homogeneity.

▪ Abstract The information on the chemical compositions of stars encoded in their spectra plays a central role in contemporary astrophysics. Stellar element abundances are, however, not observed: to

Testing the Solar Activity Paradigm in the Context of Exoplanet Transits

Transits of exoplanets across cool stars contain blended information about structures on the stellar surface and about the planetary body and atmosphere. To advance understanding of how this

Granulation in K-type dwarf stars II. Hydrodynamic simulations and 3D spectrum synthesis

Aims. To explore the impact of surface inhomogeneities on stellar spectra, granulation models need to be computed. Ideally, the most fundamental characteristics of these models should be carefully

Stellar granulation as seen in disk-integrated intensity I. Simplified theoretical modeling

Context. Solar granulation has been known for a long time to be a surface manifestation of convection. The space-borne missions CoRoT and Kepler enable us to observe the signature of this phenomena
...