Context : Super giant fast X-ray transient ( SFXT ) is a new class of the high mass X-ray binary that shows short X-ray flares . The physical mechanism of SFXT short flares is still open for discussion . The accretion process of dense clumps in stellar wind onto neutron star ( NS ) has been proposed as the origin of such short flares . Aims : In order to examine the applicability of the clumpy wind scenario , we focus on the accretion mode that depends on orbital parameters . Our goal is to impose restrictions on the orbital parameters of SFXT . Methods : Assuming a simple analytic model of clumpy wind , we investigate the condition where the size of accretion cylinder overcomes the clump size . Results : The allowed parameter region for SFXT is restricted in a relatively narrow window in P _ { orb } - e diagram . Conclusions : Binary systems with large eccentricities ( e \ga 0.4 ) and moderate orbital periods ( P _ { orb } \sim 10 d ) are prone to show periodic X-ray outbursts which are characteristic for SFXT . We confirm that systems with a long orbital period of more than 100 days can not produce bright X-ray flares in the simple clumpy wind scenario .