Hot Jupiters orbit very close to their host stars, typically around 0.05 AU. At such a distance, a hot Jupiter can raise strong tides on its host star. These tides cause the host star to spin-up by taking angular momentum away from the planet’s orbit. The outcome is that the planet’s orbit shrinks. If the planet is massive enough, it can spin-up its host star to co-rotate with its orbit around the star (i.e. the star’s spin period become the same as the planet’s orbital period), and the planet can delay or even avoid spiralling into its star. If the planet is not massive enough, it will continue to lose angular momentum, eventually spiralling into its star and get tidally destructed.
Martin et al. (2011), “A binary merger origin for inflated hot Jupiter planets”, arXiv:1102.3336 [astro-ph.SR]