| Abstract: | The determination of the radial velocity and the effective magnetic field strength for the peculiar A-type stars 53 Cam and γ Equ lad to the following results 53 Cam: The radial velocity shows a dependence on the excitation, resp. ionization potential in the way that evidently lines with higher excitation potential have higher radial velocity. We cannot explain this result with the rotator model without an essential modification of that. The amount and the time variation of the effective magnetic field agrees only approximately with that determined by BABCOCK. A secular variation may be indicated, but needs further confirmation. The effective magnetic field strength determined from the SiII-line λ = 4130.884 Å shows an essential smaller value than that by the other lines. The investigation of γ Equ yielded the following results: The best way to represent both the radial velocity and the effective magnetic field strength is a period of 1786 days given by STEINITZ and PYPER. We did not find a difference of the radial velocities derived from different lines and no line intensity variations. However, there seems to be observational evidence that short and obvious accidental variations of the radial velocity and effective magnetic field exist. |
