This paper investigates the influence of magneto-centrifugally driven or
simply magnetic winds of rapidly-rotating, strongly-magnetized T Tauri stars in
causing the inward or outward migration of close-in giant planets. The
azimuthal ram pressure of the magnetized wind acting on the planet tends to
increase the planet's angular momentum and cause outward migration if the
star's rotation period P∗ is less than the planet's orbital period Pp. In
the opposite case, P∗>Pp, the planet migrates inward. Thus, planets
orbiting at distances larger (smaller) than 0.06AU(P∗/5d)2/3
tend to be pushed outward (inward), where P∗ is the rotation period of the
star assumed to have the mass of the sun. The magnetic winds are likely to
occur in T Tauri stars where the thermal speed of the gas close to the star is
small, where the star's magnetic field is strong, and where the star rotates
rapidly. The time-scale for appreciable radial motion of the planet is
estimated as ∼2−20 Myr. A sufficiently massive close-in planet may
cause tidal locking and once this happens the radial migration due to the
magnetic wind ceases. The magnetic winds are expected to be important for
planet migration for the case of a multipolar magnetic field rather than a
dipole field where the wind is directed away from the equatorial plane and
where a magnetospheric cavity forms. The influence of the magnetic wind in
eroding and eventually destroying the accretion disk is analyzed. A momentum
integral is derived for the turbulent wind/disk boundary layer and this is used
to estimate the disk erosion time-scale as ∼1−102 Myr, with the lower
value favored.Comment: 8 pages, 6 figure