LoTr 5 is a planetary nebula with an unusual long-period binary central star .
As far as we know , the pair consists of a rapidly rotating G-type star and a hot star , which is responsible for the ionization of the nebula .
The rotation period of the G-type star is 5.95 days and the orbital period of the binary is now known to be \sim 2700 days , one of the longest in central star of planetary nebulae .
The spectrum of the G central star shows a complex H \alpha double-peaked profile which varies with very short time scales , also reported in other central stars of planetary nebulae and whose origin is still unknown .
We present new radial velocity observations of the central star which allow us to confirm the orbital period for the long-period binary and discuss the possibility of a third component in the system at \sim 129 days to the G star .
This is complemented with the analysis of archival light curves from SuperWASP , ASAS and OMC .
From the spectral fitting of the G-type star , we obtain a effective temperature of T _ { eff } = 5410 \pm 250 K and surface gravity of \log g = 2.7 \pm 0.5 , consistent with both giant and subgiant stars .
We also present a detailed analysis of the H \alpha double-peaked profile and conclude that it does not present correlation with the rotation period and that the presence of an accretion disk via Roche lobe overflow is unlikely .