博碩士論文 92229014 完整後設資料紀錄

DC 欄位	值	語言
DC.contributor	天文研究所	zh_TW
DC.creator	賴雲立	zh_TW
DC.creator	Yun-Li Lai	en_US
dc.date.accessioned	2005-7-12T07:39:07Z
dc.date.available	2005-7-12T07:39:07Z
dc.date.issued	2005
dc.identifier.uri	http://ir.lib.ncu.edu.tw:88/thesis/view_etd.asp?URN=92229014
dc.contributor.department	天文研究所	zh_TW
DC.description	國立中央大學	zh_TW
DC.description	National Central University	en_US
dc.description.abstract	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).	en_US
DC.subject	giant planet	en_US
DC.subject	migration	en_US
DC.subject	protoplanetary disk	en_US
DC.subject	steady disk	en_US
DC.subject	gap	en_US
DC.subject	photoevaporation	en_US
DC.subject	planet	en_US
DC.title	The orbital migrations of massive planets in the protoplanetary disks	en_US
dc.language.iso	en_US	en_US
DC.type	博碩士論文	zh_TW
DC.type	thesis	en_US
DC.publisher	National Central University	en_US