The Hyades open cluster presents a unique laboratory for planet formation and stellar pollution studies because all of the stars have essentially the same age and were born from the same cloud of gas .
Furthermore , with an age of \sim 650 Myr most of the intermediate and low mass stars are on the main sequence .
Given these assumptions , the accretion of metal rich material onto the surface of a star during and shortly after the formation of planetary systems should be evident via the enhanced metallicity of the star .
Building on previous work , stellar evolution models which include the effects of stellar pollution are applied to the Hyades .
The results of several Monte Carlo simulations , in which the amount of accreted material is drawn at random from a Gaussian distribution with standard deviation equal to half the mean , are presented .
An effective temperature– [ Fe/H ] relation is produced and compared to recent observations .
The theoretical predictions presented in this letter will be useful in future searches for evidence of stellar pollution due to planet formation .
It is concluded that stellar pollution effects at the mean level of \geq 2 \mathrm { M _ { \oplus } } of iron are ruled out by the current observational data ( ) .