Following the recent discovery of the first radial velocity planet in a star still possessing a protoplanetary disc (CI Tau), we examine the origin of the planet's eccentricity (e ~0.3). We show through long time-scale (105 orbits) simulations that the planetary eccentricity can be pumped by the disc, even when its local surface density is well below the threshold previously derived from short time-scale integrations. We show that the disc may be able to excite the planet's orbital eccentricity in < 1 Myr for the system parameters of CI Tau. We also perform two-planet scattering experiments and show that alternatively the observed planet may plausibly have acquired its eccentricity through dynamical scattering of amigrating lower mass planet, which has either been ejected from the system or swallowed by the central star. In the latter case the present location and eccentricity of the observed planet can be recovered if it was previously stalled within the disc's magnetospheric cavity.

The origin of the eccentricity of the hot Jupiter in CI Tau / G.P. Rosotti, R.A. Booth, C.J. Clarke, J. Teyssandier, S. Facchini, A.J. Mustill. - In: MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY. LETTERS. - ISSN 1745-3925. - 464:1(2017), pp. L114-L118. [10.1093/mnrasl/slw184]

The origin of the eccentricity of the hot Jupiter in CI Tau

G.P. Rosotti;S. Facchini;
2017

Abstract

Following the recent discovery of the first radial velocity planet in a star still possessing a protoplanetary disc (CI Tau), we examine the origin of the planet's eccentricity (e ~0.3). We show through long time-scale (105 orbits) simulations that the planetary eccentricity can be pumped by the disc, even when its local surface density is well below the threshold previously derived from short time-scale integrations. We show that the disc may be able to excite the planet's orbital eccentricity in < 1 Myr for the system parameters of CI Tau. We also perform two-planet scattering experiments and show that alternatively the observed planet may plausibly have acquired its eccentricity through dynamical scattering of amigrating lower mass planet, which has either been ejected from the system or swallowed by the central star. In the latter case the present location and eccentricity of the observed planet can be recovered if it was previously stalled within the disc's magnetospheric cavity.
Accretion; Accretion discs; Planet-disc interactions; Planets and satellites: dynamical evolution and stability; Protoplanetary discs; Stars: pre-main-sequence
Settore FIS/05 - Astronomia e Astrofisica
5-set-2016
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Utilizza questo identificativo per citare o creare un link a questo documento: http://hdl.handle.net/2434/866708
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