Volume 550, February 2013
|Number of page(s)||13|
|Published online||04 February 2013|
Instituto de Astrofísica de Canarias, 38205
La Laguna, Tenerife,
2 Departamento de Astrofísica, Universidad de La Laguna, 38206, La Laguna, Tenerife, Spain
3 Texas Advanced Computing Center, University of Texas, Austin, TX 78759, USA
4 Zentrum für Astronomie der Universität Heidelberg, Landessternwarte, Königstuhl 12, 69117 Heidelberg, Germany
e-mail: H.Ludwig@lsw.uni-heidelberg.de; E.Caffau@lsw.uni-heidelberg.de
5 Centre de Recherche Astrophysique de Lyon, UMR 5574, CNRS, Université de Lyon, École Normale Supérieure de Lyon, 46 allée d’Italie, 69364 Lyon Cedex 07, France
Received: 20 July 2012
Accepted: 26 November 2012
Context. To derive space velocities of stars along the line of sight from wavelength shifts in stellar spectra requires accounting for a number of second-order effects. For most stars, gravitational redshifts, convective blueshifts, and transverse stellar motion are the dominant contributors.
Aims. We provide theoretical corrections for the net velocity shifts due to convection expected for the measurements from the Gaia Radial Velocity Spectrometer (RVS).
Methods. We used a set of three-dimensional time-dependent simulations of stellar surface convection computed with CO5BOLD to calculate spectra of late-type stars in the Gaia RVS range and to infer the net velocity offset that convective motions will induce in radial velocities derived by cross-correlation.
Results. The net velocity shifts derived by cross-correlation depend both on the wavelength range and spectral resolution of the observations. Convective shifts for Gaia RVS observations are less than 0.1 km s-1 for late-K-type stars, and they increase with stellar mass, reaching about 0.3 km s-1 or more for early F-type dwarfs. This tendency is the result of an increase with effective temperature in both temperature and velocity fluctuations in the line-forming region. Our simulations also indicate that the net RVS convective shifts can be positive (i.e. redshifts) in some cases. Overall, the blueshifts weaken slightly with increasing surface gravity, and are enhanced at low metallicity. Gravitational redshifts amount to 0.7 km s-1 and dominate convective blueshifts for dwarfs, but become much weaker for giants.
Key words: stars: atmospheres / line: formation / convection / techniques: radial velocities / stars: solar-type / stars: late-type
Appendix A is available in electronic form at http://www.aanda.org
Model spectra from the 1D and 3D calculations are only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr184.108.40.206 or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/550/A103
© ESO, 2013
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