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The formation of dust gaps in protoplanetary disks is one of the mostimportant signposts of disk evolution and possibly the formation of planets. Weaim to characterize the 'flaring' disk structure around the Herbig Ae/Be starsHD 100453 and HD 34282. Their spectral energy distributions (SEDs) show anemission excess between 15-40{\mu}m, but very weak (HD 100453) and no (HD34282) signs of the 10 and 20 {\mu}m amorphous silicate features. Weinvestigate whether this implies the presence of large dust gaps. In this work,spatially resolved mid-infrared Q-band images taken with Gemini North/MICHELLEare investigated. We perform radiative transfer modeling and examine the radialdistribution of dust. We simultaneously fit the Q-band images and SEDs of HD100453 and HD 34282. Our solutions require that the inner-halos and outer-disksare likely separated by large dust gaps that are depleted wih respect to theouter disk by a factor of 1000 or more. The inner edges of the outer disks ofHD 100453 and HD 34282 have temperatures of about $160 \pm 10$ K and $60 \pm 5$K respectively. Because of the high surface brightnesses of these walls, theydominate the emission in the Q-band. Their radii are constrained at 20+2 AU and92+31 AU, respectively. We conclude that, HD 100453 and HD 34282 likely havedisk dust gaps and the upper limit on the dust mass in each gap is estimated tobe about $10^{-7}$M$_{\odot}$. We find that the locations and sizes of diskdust gaps are connected to the SED, as traced by the mid-infrared flux ratioF30/F13.5. We propose a new classification scheme for the Meeus groups (Meeuset al. 2001) based on the F30/F13.5 ratio. The absence of amorphous silicatefeatures in the observed SEDs is caused by the depletion of small (smaller than1 {\mu}m) silicate dust at temperatures above 160 K, which could be related tothe presence of a dust gap in that region of the disk.

Large dust gaps in the transitional disks of HD 100453 and HD 34282