Context : The study of pulsation in Pre–Main–Sequence intermediate-mass stars represents an important tool for deriving information on fundamental stellar parameters and internal structure , as well as for testing current theoretical models .
Interest in this class of variable stars has significantly increased during the last decade and about 30 members are presently known in the literature .

Aims : We have constructed the frequency spectrum of the oscillations in V346 Ori .
We apply asteroseismic tools to these data to estimate the intrinsic parameters ( mass , luminosity , effective temperature ) of V346 Ori and to obtain information on its internal structure .

Methods : CCD time series photometry in the Johnson V filter has been obtained for a total of 145.7 h of observations distributed over 36 nights .
The resulting light curves have been subjected to a detailed frequency analysis using updated numerical techniques .
Photometric and spectroscopic data have also been acquired to determine reliable estimates of the stellar properties .

Results : We have identified 13 oscillation frequencies , 6 of which with higher significance .
These have been compared with the predictions of non-radial adiabatic models .
The resulting best fit model has a mass of 2.1 \pm 0.2 M _ { \odot } , luminosity \log { L / L _ { \odot } } = 1.37 ^ { +0.11 } _ { -0.13 } , and effective temperature 7300 \pm 200 K. These values are marginally consistent with the association of V346 Ori to Orion OB1a .
Alternatively , V346 Ori could be placed at a slightly larger distance than previously estimated .

Conclusions :