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We present the discovery of KELT-22Ab, a hot Jupiter from the KELT-Southsurvey. KELT-22Ab transits the moderately bright ($V\sim 11.1$) Sun-like G2Vstar TYC 7518-468-1. The planet has an orbital period of $P = 1.3866529 \pm0.27 $ days, a radius of $R_{P} = 1.285_{-0.071}^{+0.12}~R_{J}$, and arelatively large mass of $M_{P} = 3.47_{-0.14}^{+0.15}~ M_{J}$. The star has$R_{\star} = 1.099_{-0.046}^{+0.079}~ R_{\odot}$, $M_{\star} =1.092_{-0.041}^{+0.045}~ M_{\odot}$, ${T_{\rm eff}\,} = 5767_{-49}^{+50}~$ K,${\log{g_\star}} = 4.393_{-0.060}^{+0.039}~$ (cgs), and [m/H] =$+0.259_{-0.083}^{+0.085}~$, and thus, other than its slightly super-solarmetallicity, appears to be a near solar twin. Surprisingly, KELT-22A exhibitskinematics and a Galactic orbit that are somewhat atypical for thin disk stars.Nevertheless, the star is rotating quite rapidly for its estimated age, showsevidence of chromospheric activity, and is somewhat metal rich. Imaging revealsa slightly fainter companion to KELT-22A that is likely bound, with a projectedseparation of 6\arcsec ($\sim$1400 AU). In addition to the orbital motioncaused by the transiting planet, we detect a possible linear trend in theradial velocity of KELT-22A suggesting the presence of another relativelynearby body that is perhaps non-stellar. KELT-22Ab is highly irradiated (as aconsequence of the small semi-major axis of $a/R_{\star} = 4.97$), and ismildly inflated. At such small separations, tidal forces become significant.The configuration of this system is optimal for measuring the rate of tidaldissipation within the host star. Our models predict that, due to tidal forces,the semi-major axis of KELT-22Ab is decreasing rapidly, and is thus predictedto spiral into the star within the next Gyr.

KELT-22Ab: A Massive Hot Jupiter Transiting a Near Solar Twin