The low-level radial velocity variability in Barnard's star (= GJ 699) - Secular acceleration, indications for convective redshift, and planet mass limits

We report results from 2 1=2 yr of high precision radial velocity (RV) monitoring of Barnard's star. The high RV measurement precision of the VLT-UT2+UVES of 2:65 m s 1 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 H 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 5:15 0:89 m s 1 yr 1 .T his agrees within 0:95 with the predicted value of 4:50 m s 1 yr 1 based on the Hipparcos proper motionand 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 2:97 0:51 m s 1 yr 1 (3:0 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 coecient of 0:50 indicates that the appearance of active regions causes a blueshiftof 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 blueshiftsas 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 m sin i and to the true massm of hypothetical planetary companions in circular orbits. For the separation range 0:017 0:98 AU we exclude any planet with m sin i> 0:12 MJupiter and m> 0:86 MJupiter. Throughout the habitable zone around Barnard's star, i.e. 0:034 0:082 AU, we exclude planets with m sin i> 7:5 MEarth and m> 3:1 MNeptune.