The orbital migrations of massive planets in the protoplanetary disks

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賴雲立(Yun-Li Lai) 查詢紙本館藏

畢業系所

天文研究所

論文名稱

(The orbital migrations of massive planets in the protoplanetary disks)

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★ Numerical Simulations of Binary Accretion Disks

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摘要(英)

The observed small orbital radii of massive extrasolar planets around
the central solar-type stars can be explained by the mechanisms of
orbital migration. The scenario is: the planet forms in the protoplanetary
disk and induces planet–disk tidal interactions resulting in the
inward migration of the planet. In this thesis, we first construct a onedimensional
disk model corresponding to the observational constraints
and then investigate the effects caused by the embedded planet, including
the regulations of the disk surface density and the planetary
orbital radius. Using numerical simulations, the evolution of the disk
as well as the changes in the planetary orbital radius are produced.
The massive planet (∼ 1MJ ) opens a gap quickly in the vicinity of its
location, and the gap would move with the migrating planet. If the
planet forms earlier in the disk, its extent of migration is larger. We
also find that the more massive planet migrates faster initially, but
the resulting change in orbital radius is not obvious (it would stop
migrating earlier).

關鍵字(中)

關鍵字(英)

★ giant planet
★ migration
★ protoplanetary disk
★ steady disk
★ gap
★ photoevaporation
★ planet

論文目次

1 Introduction 1
2 The Models 5
2.1 The Governing Equations . . . . . . . . . . . . . . . . 5
2.1.1 Viscous Accretion DiskModel . . . . . . . . . . 5
2.1.2 The Disk-Planet Interaction . . . . . . . . . . . 7
2.1.3 The PlanetaryMigrations . . . . . . . . . . . . 8
2.2 The Viscosity . . . . . . . . . . . . . . . . . . . . . . . 11
2.3 The Non-dimensionalization . . . . . . . . . . . . . . . 12
2.3.1 The Dimensionless Variables . . . . . . . . . . . 12
2.3.2 Converting to √r Space . . . . . . . . . . . . . 14
2.4 The Photoevaporation . . . . . . . . . . . . . . . . . . 15
2.5 The Steady DiskModel . . . . . . . . . . . . . . . . . . 18
3 The Numerical Methods 20
3.1 The Crank-Nicholson Scheme . . . . . . . . . . . . . . 23
3.2 The Two-Step Lax-Wendroff Scheme . . . . . . . . . . 24
4 The Comparisons with Pringle (1981) and Clarke et al.
(2001) 26
4.1 Pringle (1981): The Constant Viscosity . . . . . . . . . 26
4.2 Clarke et al. (2001): The Similarity Solution . . . . . . 28
5 The Results and Discussions 35
5.1 The Disk Parameters . . . . . . . . . . . . . . . . . . . 35
5.2 The Disk Evolution . . . . . . . . . . . . . . . . . . . . 39
5.3 The Effects of Planets . . . . . . . . . . . . . . . . . . 46
5.3.1 Different Values of Formation Time . . . . . . . 51
5.3.2 Different Values of Initial Radius . . . . . . . . 52
5.3.3 Different Values of PlanetaryMass . . . . . . . 52
5.3.4 The Results of β = 3/2Model . . . . . . . . . . 56
6 The Conclusions and Future Works 59
References 61

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指導教授

江瑛貴(Ing-Guey Jiang)

審核日期

2005-7-12

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