| Abstract: | The radial velocity of the binary star β CrB was reinvestigated to look for the hypothetical third body, suggested by NEUBAUERS results. Under the assumption that a systematic difference of 1.4 km/sec between NEUBAUERS results from 1931–43 and ours from 1971–83 is of instrumental origin, the radial velocities of both epochs can be well represented with the same orbital elements: thus the probability for the existence of a third component in the system is reduced. The eccentricity and the angle of periastron passage of the visual orbit, derived from published speckle interferometric measurements, agree very well with the corresponding elements of the spectroscopic orbit. For the masses of the components those of giant resp. subgiant stars of type A8 and F5 are found. The geometry of the binary β CrB with a magnetic star as the primary component is demonstrated. |
