  This paper is written as a follow-up observations to reinterpret the radial
velocity (RV) of HD 36384, where the existence of planetary systems is known to
be ambiguous. In giants, it is, in general, difficult to distinguish the
signals of planetary companions from those of stellar activities. Thus, known
exoplanetary giant hosts are relatively rare. We, for many years, have obtained
RV data in evolved stars using the high-resolution, fiber-fed Bohyunsan
Observatory Echelle Spectrograph (BOES) at the Bohyunsan Optical Astronomy
Observatory (BOAO). Here, we report the results of RV variations in the M giant
HD 36384. We have found two significant periods of 586d and 490d. Considering
the orbital stability, it is impossible to have two planets at so close orbits.
To determine the nature of the RV variability variations, we analyze the
HIPPARCOS photometric data, some indicators of stellar activities, and line
profiles. A significant period of 580d was revealed in the HIPPARCOS
photometry. H{\alpha} EW variations also show a meaningful period of 582d.
Thus, the period of 586d may be closely related to the rotational modulations
and/or stellar pulsations. On the other hand, the other significant period of
490d is interpreted as the result of the orbiting companion. Our orbital fit
suggests that the companion was a planetary mass of 6.6 MJ and is located at
1.3 AU from the host.
