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 atmospheres. Methods. Very high-resolution (R similar or equal to 160 000-210 000), high signal-to-noise ratio (S/N greater than or similar to 300) spectra of nine bright K-dwarfs were obtained with the 2dcoude spectrograph on the 2.7m telescope at McDonald Observatory to determine wavelength shifts and asymmetries of Fe I lines. Spectra of the same stars acquired with the High Resolution Spectrograph (R similar or equal to 120, 000) on the 9.2m Hobby Eberly Telescope were used as radial velocity templates to calibrate the wavelength scale of the 2dco...
Context. Solar granulation has been known for a long time to be a surface manifestation of convectio...
Context. Stellar granulation generates fluctuations in photometric and spectroscopic data whose prop...
Context. Spectroscopy across spatially resolved stellar surfaces reveals spectral line profiles free...
Aims. We seek to detect and quantify the effects of surface convection (granulation) on the line spe...
Aims. We seek to detect and quantify the effects of surface convection (granulation) on the line spe...
Aims. To explore the impact of surface inhomogeneities on stellar spectra, granulation models need t...
textThe presence of surface convection in K-type dwarfs is revealed in very high quality spectra (R...
A very high resolution (R = lambda/Delta lambda = 200,000), high signal-to-noise ratio (S/N similar ...
Granulation in the atmospheres of cool stars introduce changes to the shapes of absorption lines dis...
Stars are not smooth. Their photosphere is covered by a granulation pattern associated with the heat...
Cool, low mass stars with a convective envelope have bubbles of hot, bright plasma rising to the sur...
Manifestations of stellar activity (such as star-spots, plage/faculae, and convective flows) are wel...
. Wavelength positions of photospheric absorption lines may be affected by surface convection (stell...
International audienceContext. Stellar activity and convection-related surface structures might caus...
Context. Solar granulation has been known for a long time to be a surface manifestation of convectio...
Context. Stellar granulation generates fluctuations in photometric and spectroscopic data whose prop...
Context. Spectroscopy across spatially resolved stellar surfaces reveals spectral line profiles free...
Aims. We seek to detect and quantify the effects of surface convection (granulation) on the line spe...
Aims. We seek to detect and quantify the effects of surface convection (granulation) on the line spe...
Aims. To explore the impact of surface inhomogeneities on stellar spectra, granulation models need t...
textThe presence of surface convection in K-type dwarfs is revealed in very high quality spectra (R...
A very high resolution (R = lambda/Delta lambda = 200,000), high signal-to-noise ratio (S/N similar ...
Granulation in the atmospheres of cool stars introduce changes to the shapes of absorption lines dis...
Stars are not smooth. Their photosphere is covered by a granulation pattern associated with the heat...
Cool, low mass stars with a convective envelope have bubbles of hot, bright plasma rising to the sur...
Manifestations of stellar activity (such as star-spots, plage/faculae, and convective flows) are wel...
. Wavelength positions of photospheric absorption lines may be affected by surface convection (stell...
International audienceContext. Stellar activity and convection-related surface structures might caus...
Context. Solar granulation has been known for a long time to be a surface manifestation of convectio...
Context. Stellar granulation generates fluctuations in photometric and spectroscopic data whose prop...
Context. Spectroscopy across spatially resolved stellar surfaces reveals spectral line profiles free...