2026-07-072026-07-07http://salesiana.dossiersoluciones.com/handle/123456789/181043The emission spectra of TeV blazars extend up to tens of TeV and the emission mechanism of the TeV $γ$-rays is explained by synchrotron self-Compton scattering in leptonic models. In these models the time variabilities of X-rays and TeV $γ$-rays are correlated. However, recent observations of 1ES 1959+650 and Mrk 421 have found the ``orphan'' TeV $γ$-ray flares, i.e., TeV $γ$-ray flares without simultaneous X-ray flares. In this paper we propose a model for the ``orphan'' TeV $γ$-ray flares, employing an inhomogeneous leptonic jet model. After a primary flare that accompanies flare-up both in X-rays and TeV $γ$-rays, radiation propagates in various directions in the comoving frame of the jet. When a dense region in the jet receives the radiation, X-rays are scattered by relativistic electrons/positrons to become TeV $γ$-rays. These $γ$-ray photons are observed as an ``orphan'' TeV $γ$-ray flare. The observed delay time between the primary and ``orphan'' flares is about two weeks and this is accounted for in our model for parameters such as $Γ= 20$, $d = 4 \times 10^{17}$cm, $α= 3$, and $η= 1$, where $Γ$ is the bulk Lorentz factor of the jet, $d$ is the distance between the central black hole and the primary flare site, $α/Γ$ is the angle between the jet axis and the direction of the motion of the dense region that scatters incoming X-rays produced by the primary flare, and $η/Γ$ is the angle between the jet axis and the line of sight.12page, 6 figures, accepted by ApJAstrophysicstext