Understanding disk dissipation is essential for studying how planets form .
Disk gaps and holes , which almost correspond to dust-free regions , are inferred from infrared observations of T Tauri stars ( TTS ) , indicating the existence of a transitional phase between thick accreting disks and debris disks .
Transition disks are usually referred to as candidates for newly formed planets .
We searched for transition disk candidates belonging to NGC 2264 .
Using stellar and disk parameters obtained in the observational multiwavelength campaign CSI2264 , we characterized accretion , disk , and stellar properties of transition disk candidates and compared them to systems with a full disk and diskless stars We modeled the spectral energy distribution ( SED ) of a sample of 401 TTS , observed with both CFHT equipped with MegaCam and IRAC instrument on the Spitzer , with Hyperion SED fitting code using photometric data from the U band ( 0.3 \mu \mathrm { m } ) to the Spitzer/MIPS 24 \mu \mathrm { m } band .
We used the SED modeling to distinguish transition disk candidates , full disk systems , and diskless stars .
We classified \sim 52 \% of the sample as full disk systems , \sim 41 \% as diskless stars , and \sim 7 \% of the systems as transition disk candidates , among which seven systems are new transition disk candidates belonging to the NGC 2264 cluster .
The sample of transition disk candidates present dust in the inner disk similar to anemic disks , according to the \alpha _ { \mathrm { IRAC } } classification , which shows that anemic disk systems can be candidate transition disks .
We show that the presence of a dust hole in the inner disk does not stop the accretion process since 82 \% of transition disk candidates accrete and show \mathrm { H } \alpha , UV excess , and mass accretion rates at the same level as full disk systems .
We estimate the inner hole sizes , ranging from 0.1 to 78 \mathrm { AU } , for the sample of transition disk candidates .
In only \sim 18 \% of the transition disk candidates , the hole size could be explained by X-ray photoevaporation from stellar radiation .