We present the results on period search and modeling of the cool DAV star KUV 02464+3239 .
Our observations resolved the multiperiodic pulsational behaviour of the star .
In agreement with its position near the red edge of the DAV instability strip , it shows large amplitude , long period pulsation modes , and has a strongly non-sinusoidal light curve .
We determined 6 frequencies as normal modes and revealed remarkable short-term amplitude variations .
A rigorous test was performed for the possible source of amplitude variation : beating of modes , effect of noise , unresolved frequencies or rotational triplets .
Among the best-fit models resulting from a grid search , we selected 3 that gave l = 1 solutions for the largest amplitude modes .
These models had masses of 0.645 , 0.650 and 0.680 M _ { \sun } .
The 3 ‘ favoured ’ models have M _ { \mathrm { H } } between 2.5 \mathrm { x } 10 ^ { -5 } -6.3 \mathrm { x } 10 ^ { -6 } M _ { * } and give 14.2 – 14.8 mas seismological parallax .
The 0.645 M _ { \sun } ( 11 400 K ) model also matches the spectroscopic \mathrm { log } g and T _ { \mathrm { eff } } within 1 \sigma .
We investigated the possibility of mode trapping and concluded that while it can explain high amplitude modes , it is not required .