The role of atmospheric outflows in the migration of hot Jupiters. (arXiv:2101.04112v2 [astro-ph.EP] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Kurbatov_E/0/1/0/all/0/1">Evgeny P. Kurbatov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bisikalo_D/0/1/0/all/0/1">Dmitri V. Bisikalo</a>
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 HD209458 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.
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 HD209458 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.
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