A study over several epochs and frequencies has demonstrated that the variability in CTA 102 (QSO 2230+114, z = 1.037) at λ<32 cm is mainly due to intrinsic processes (Rantakyrö et al. 1995, A&A, in press, hereafter R1995). Observations of CTA 102 with the EGRET telescope at the high-energy γ-ray waveband have shown that the source exhibits a strong γ-ray luminosity, Lγ = 5 × 1047 ergs s–1 (Nolan, P.L., et al. 1993, ApJ, 414, 82). This luminosity dominates the emission seen at all other wavebands, a common feature among BLAZARs. The common explanation for the high Lγ is that the emission is the result of a beamed jet with a high Lorentz factor.