  Hot Jupiters formed through circularization of high-eccentricity orbits
should be found at orbital separations $a$ exceeding $twice$ that of their
Roche limit $a_{\rm R}$. Nevertheless, about a dozen giant planets have now
been found well within this limit ($a_{\rm R}<a<2a_{\rm R}$), with one coming
as close as 1.2$a_{\rm R}$. In this Letter, we show that orbital decay
(starting beyond 2$a_{\rm R}$) driven by tidal dissipation in the star can
naturally explain these objects. For a few systems (WASP-4 and 19), this
explanation requires the linear reduction in convective tidal dissipation
proposed originally by Zahn (1966, 1989) and verified by recent numerical
simulations Penev et al. (2007), but rules out the quadratic prescription
proposed by Goldreich & Nicholson (1977). Additionally, we find that
WASP-19-like systems could potentially provide direct empirical constraints on
tidal dissipation, as we could soon be able to measure their orbital decay
through high precision transit timing measurements.
