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 ( P _ { orb } = 528 d ) .
Both the longitudinal magnetic field measurements and radial velocity variations are consistent with a rotation period of 10 \pm 2 days , which are also consistent with the measured chromospheric activity level of the star ( ^ { \prime } logR ^ { \prime } _ { HK } = -4.64 ) .
Together , these quantities indicate a low inclination angle , i \sim 18 ^ { \circ } .
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 .