The role of atmospheric outflows in the migration of hot Jupiters

Abstract

Many of observed hot Jupiters are subject to atmospheric outflows. Numerical simulations have shown that the matter escaping from the atmosphere can accumulate outside the orbit of the planet, forming a torus. In a few 10 8 yr, the mass of the torus can become large enough to exert a significant gravitational effect on the planet. Accumulation of mass, in its own turn, is hindered by the activity of the star, which leads to the photoevaporation of the torus matter. We explore the role of these and other factors in the planet's migration in the epoch when the protoplanetary disk has already disappeared. Using HD 209458 system as an example, we show that the gravitational interaction with the torus leads to the possibility of migration of the planet to its observable position, starting from an orbit 0.3 AU.

Tidal migration of hot Jupiters: introducing the impact of gravity wave dissipation

“…The first attempt to consider both regimes of magnetic interaction within one model was made by Strugarek et al (2017). Aside from magnetic interaction, many different mechanisms responsible for planetary migration have been proposed, including planetary obliquity tides (Millholland & Spalding 2020), Kozai migration (Naoz et al 2011;Attia et al 2021), the gravitational interaction between hot Jupiter and its atmospheric outflows (Kurbatov & Bisikalo 2021), migration inside a disk cavity (Debras et al 2021), secular planet-planet interaction (Wu & Lithwick 2011;Laskar et al 2012;Bolmont et al 2015;Pu & Lai 2019;Becker et al 2020), and many others.…”