By following the evolution of several observed exoplanetary systems we show that by lowering the mass loss rate of single solar-like stars during their two giant branches , these stars will swallow their planets at the tip of their asymptotic giant branch ( AGB ) phase .
This will most likely lead the stars to form elliptical planetary nebulae ( PNe ) .
Under the traditional mass loss rate these stars will hardly form observable PNe .
Stars with a lower mass loss rate as we propose , about 15 per cent of the traditional mass loss rate of single stars , leave the AGB with much higher luminosities than what traditional evolution produces .
Hence , the assumed lower mass loss rate might also account for the presence of bright PNe in old stellar populations .
We present the evolution of four exoplanetary systems that represent stellar masses in the range of 0.9 - 1.3 M _ { \odot } .
The justification for this low mass loss rate is our assumption that the stellar samples that were used to derive the traditional average single-star mass loss rate were contaminated by stars that suffer binary interaction .