  The results from a spectro-polarimetric study of the planet-hosting Sun-like
star, HD 147513 (G5V), are presented here. Robust detections of Zeeman
signatures at all observed epochs indicate a surface magnetic field, with
longitudinal magnetic field strengths varying between 1.0-3.2 G. Radial
velocity variations from night to night modulate on a similar timescale to the
longitudinal magnetic field measurements. These variations are therefore likely
due to the rotational modulation of stellar active regions rather than the much
longer timescale of the planetary orbit (Porb=528 d). Both the longitudinal
magnetic field measurements and radial velocity variations are consistent with
a rotation period of 10 +/- 2 days, which are also consistent with the measured
chromospheric activity level of the star (log R'(HK)=-4.64). Together, these
quantities indicate a low inclination angle, i~18 degrees. We present
preliminary magnetic field maps of the star based on the above period and find
a simple poloidal large-scale field. Chemical analyses of the star have
revealed that it is likely to have undergone a barium-enrichment phase in its
evolution because of a higher mass companion. Despite this, our study reveals
that the star has a fairly typical activity level for its rotation period and
spectral type. Future studies will enable us to explore the long-term evolution
of the field, as well as to measure the stellar rotation period, with greater
accuracy.
