The stars 55 Cnc , 51 Peg , 47 UMa , 70 Vir , and HD 114762 have recently been proposed to harbor planetary mass companions .
Using spectroscopic methods we find that 55 Cnc and 51 Peg are super metal-rich , 47 UMa and 70 Vir have roughly solar metallicities , and HD 114762 is metal-poor .
Otherwise , the abundance patterns , expressed as [ X/Fe ] , are approximately solar .
The ages of 47 UMa and 51 Peg are similar to that of the Sun ; 70 Vir is slightly older , and 55 Cnc and HD 114762 are at least 10 Gyrs old .
Our estimates of v \sin i for the parent stars are 1.4 \pm 0.5 , 1.8 \pm 0.4 , 2.0 \pm 0.3 , < 1 , and < 1.5 km s ^ { -1 } for 55 Cnc , 51 Peg , 47 UMa , 70 Vir , and HD 114762 , respectively .
Using these data and estimates for the rotation periods and radii , the corresponding masses of the companions are : > 0.6 , 0.51 ^ { +0.22 } _ { -0.03 } , 4.6 \pm 1.0 , > 20 , and > 8.5 M _ { J } .
The systems appear to fall into three groups : roughly Jupiter mass companions with small circular orbits with metal-rich parent stars ( 55 Cnc and 51 Peg ) , larger companions with larger circular orbits ( 47 UMa ) , and much more massive companions with large eccentric orbits orbiting moderately metal-poor parent stars ( 70 Vir and HD 114762 ) .

Our findings are consistent with a recently proposed mechanism whereby a gas giant migrates to within a few hundredths of an AU of its parent star during the formative epoch of the planetary system .
During this process the material between the giant planet and the star is accreted onto the latter .
If the accreted material is depleted in H and He , then the photospheric composition of the parent star might be altered significantly .