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We propose a new model for the description of ultra-short flares from TeVblazars by compact magnetized condensations (blobs), produced when red giantstars cross the jet close to the central black hole. Our study includes asimple dynamical model for the evolution of the envelope lost by the star inthe jet, and its high energy nonthermal emission through different leptonic andhadronic radiation mechanisms. We show that the fragmented envelope of the starcan be accelerated to Lorentz factors up to 100 and radiate effectively theavailable energy in gamma-rays predominantly through proton synchrotronradiation or external inverse Compton scattering of electrons. The model canreadily explain the minute-scale TeV flares on top of longer (typicaltime-scales of days) gamma-ray variability as observed from the blazar PKS2155-304. In the framework of the proposed scenario, the key parameters of thesource are robustly constrained. In the case of proton synchrotron origin ofthe emission a mass of the central black hole of $M_{\rm BH}\approx 10^8M_{\odot}$, a total jet power of $L_{\rm j} \approx 2\times 10^{47} \, \rmerg\,s^{-1}$ and a Doppler factor, of the gamma-ray emitting blobs, of$\delta\geq 40$ are required. Whilst for the external inverse Compton model,parameters of  $M_{\rm BH}\approx 10^8 M_{\odot}$, $L_{\rm j} \approx 10^{46} \, \rmerg\,s^{-1}$ and the $\delta\geq 150$ are required.

Rapid TeV variability in Blazars as result of Jet-Star Interaction