Volume 403, Number 3, June I 2003
|Page(s)||1077 - 1087|
|Section||Stellar structure and evolution|
|Published online||23 May 2003|
The low-level radial velocity variability in Barnard's star (= GJ 699)*
Secular acceleration, indications for convective redshift, and planet mass limits
Thüringer Landessternwarte Tautenburg, Sternwarte 5, 07778 Tautenburg, Germany e-mail: firstname.lastname@example.org; email@example.com
2 McDonald Observatory, The University of Texas at Austin, Austin, TX 78712-1083, USA e-mail: firstname.lastname@example.org; email@example.com
3 Université de Paris-Sud, bâtiment 470, 91405 Orsay Cedex, France e-mail: firstname.lastname@example.org
4 The Isaac Newton Group of Telescopes, Apartado 321, 38700 Santa Cruz de La Palma, Canary Islands, Spain e-mail: email@example.com
5 European Southern Observatory, Casilla 19001, Vitacura, Santiago 19, Chile e-mail: firstname.lastname@example.org; email@example.com
6 Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA e-mail: firstname.lastname@example.org
Corresponding author: M. Kürster, email@example.com
Accepted: 11 March 2003
We report results from of high precision radial velocity monitoring of Barnard's star. The high RV measurement precision of the VLT-UT2+UVES of made the following findings possible. (1) The first detection of the change in the RV of a star caused by its space motion (RV secular acceleration). (2) An anti-correlation of the measured RV with the strength of the filling-in of the line by emission. (3) Very stringent mass upper limits to planetary companions. Using only data from the first 2 years, we obtain a best-fit value for the RV secular acceleration of . This agrees within with the predicted value of based on the Hipparcos proper motion and parallax combined with the known absolute radial velocity of the star. When the RV data of the last half-year are added the best-fit slope is strongly reduced to ( away from the predicted value), clearly suggesting the presence of additional RV variability in the star. Part of it can be attributed to stellar activity as we demonstrate by correlating the residual RVs with an index that describes the filling-in of the H line by emission. A correlation coefficient of -0.50 indicates that the appearance of active regions causes a blueshift of photospheric absorption lines. Assuming that active regions basically inhibit convection we discuss the possibility that the fundamental (inactive) convection pattern in this M4V star produces a convective redshift which would indicate that the majority of the absorption lines relevant for our RV measurements is formed in a region of convective overshoot. This interpretation could possibly extend a trend indicated in the behaviour of earlier spectral types that exhibit convective blueshift, but with decreasing line asymmetries and blueshifts as one goes from G to K dwarfs. Based on this assumption, we estimate that the variation of the visible plage coverage is about 20%. We also determine upper limits to the projected mass and to the true mass m of hypothetical planetary companions in circular orbits. For the separation range we exclude any planet with and . Throughout the habitable zone around Barnard's star, i.e. , we exclude planets with and .
Key words: techniques: radial velocities / stars: kinematics / stars: planetary systems / stars: activity
© ESO, 2003
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