This work presents a homogeneous determination of lithium abundances in a large sample of giant-planet hosting stars ( N=117 ) , and a control sample of disk stars without detected planets ( N=145 ) .
The lithium abundances were derived using a detailed profile fitting of the Li i doublet at \lambda 6708 Å in LTE .
The planet hosting and comparison stars were chosen to have significant overlap in their respective physical properties , including effective temperatures , luminosities , masses , metallicities and ages .
The combination of uniform data and homogeneous analysis with well selected samples , makes this study well-suited to probe for possible differences in the lithium abundances found in planet hosting stars .
An overall comparison between the two samples reveals no obvious differences between stars with and without planets .
Closer examination of the behavior of the Li abundances over a narrow range of effective temperature ( 5700 K \leq T _ { eff } \leq 5850 K ) indicates subtle differences between the two stellar samples ; this temperature range is particularly sensitive to various physical processes that can deplete lithium .
In this T _ { eff } range planet hosting stars have lower Li abundances ( by \sim 0.26 dex on average ) than the comparison stars , although this segregation may be influenced by combining stars from a range of ages , metallicities and masses .
When stars with very restricted ranges in metallicity ( [ Fe/H ] = 0.00 to +0.20 dex ) and mass ( M \sim 1.05 – 1.15 M _ { \sun } ) are compared , however , both stars with and without planets exhibit similar behaviors in the lithium abundance with stellar age , suggesting that there are no differences in the lithium abundances between stars with planets and stars not known to have planets .