V346 Ori is a Herbig Ae star of Spectral type A7. It has already been observed from during 2 single nights separated by 1 year (see Pinheiro et al. 2003, A&A, 399, 271). It has been found to be variable on short time scales and its light curve of the star has been interpreted as the superposition of at least two periodic signals that result from delta Scuti-type stellar oscillations. The computation of linear non-adiabatic radial pulsation models for PMS stars reproduces these periods for a 1.55 Msun star with Teff = 7410 K and log L/Lsun = 0.74 pulsating in the fundamental and in the second overtone. If the assumption of radial oscillations is indeed correct, the star's location on the HR diagram places it at a distance significantly smaller than that of the Orion star forming region, hence raising questions regarding the evolutionary status of V346 Ori. Observations with better time sampling and spanning a longer period of time are needed if the latter question is to be addressed fully.