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Conference Paper: On the Migration of the Galilean Satellites

TitleOn the Migration of the Galilean Satellites
Authors
Issue Date2013
Citation
The Protostars and Planets VI (PPVI), Heidelberg, German, 15-20 July 2013. In the Program and Abstract Book of the Protostars and Planets VI (PPVI), 2013, p. 278-279, abstract no. Poster 2K097 How to Cite?
AbstractThe migration of the Galilean satellites during formation due to interactions with the circumjovian disk is studied. In the gas-starved disk model proposed by Canup & Ward (2002, 2006), the Galilean satellites are the last generation of satellites formed in the circumjovian disk, and their migration and accretion depend on disk viscosity, opacity and material inflow rate. Relaxing the migration to non-isothermal type I regime (e.g. Paardekooper et al. 2010) allows the satellites to migrate outwards in optically-thick disk regions, and there is a position where the disk torque is zero. This contrasts with 278the results in the isothermal type I regime in which the satellites always migrate inwards. Including the effect of temperature dependence of disk opacity can produce multiple zero-torque positions in the circumjovian disk. As the disk depletes, these zero-torque positions shift towards Jupiter. Under this setting, a satellite at a range of initial locations will eventually converge to near one of these zero-torque positions, but stays at a fixed distance away (with the distance depending on satellite mass), so that it is moving inwards with the zero-torque position. However, if the satellite starts at a large-enough distance from Jupiter, it may move in a trajectory that does not converge to any of these zero-torque positions and survives to the end. The effect of satellite growth and variation of disk parameters on satellite migration will be discussed. The migration in multiple satellite system, and how these settings can possibly result in the Laplace resonance among the Galilean satellites, will be also investigated. This work is supported in part by Hong Kong RGC grant HKU 7030/11P
DescriptionPoster Presentation
Topic 67: Solar System: General
Persistent Identifierhttp://hdl.handle.net/10722/205159

 

DC FieldValueLanguage
dc.contributor.authorLi, WYen_US
dc.contributor.authorLee, MHen_US
dc.date.accessioned2014-09-20T01:44:27Z-
dc.date.available2014-09-20T01:44:27Z-
dc.date.issued2013en_US
dc.identifier.citationThe Protostars and Planets VI (PPVI), Heidelberg, German, 15-20 July 2013. In the Program and Abstract Book of the Protostars and Planets VI (PPVI), 2013, p. 278-279, abstract no. Poster 2K097en_US
dc.identifier.urihttp://hdl.handle.net/10722/205159-
dc.descriptionPoster Presentation-
dc.descriptionTopic 67: Solar System: General-
dc.description.abstractThe migration of the Galilean satellites during formation due to interactions with the circumjovian disk is studied. In the gas-starved disk model proposed by Canup & Ward (2002, 2006), the Galilean satellites are the last generation of satellites formed in the circumjovian disk, and their migration and accretion depend on disk viscosity, opacity and material inflow rate. Relaxing the migration to non-isothermal type I regime (e.g. Paardekooper et al. 2010) allows the satellites to migrate outwards in optically-thick disk regions, and there is a position where the disk torque is zero. This contrasts with 278the results in the isothermal type I regime in which the satellites always migrate inwards. Including the effect of temperature dependence of disk opacity can produce multiple zero-torque positions in the circumjovian disk. As the disk depletes, these zero-torque positions shift towards Jupiter. Under this setting, a satellite at a range of initial locations will eventually converge to near one of these zero-torque positions, but stays at a fixed distance away (with the distance depending on satellite mass), so that it is moving inwards with the zero-torque position. However, if the satellite starts at a large-enough distance from Jupiter, it may move in a trajectory that does not converge to any of these zero-torque positions and survives to the end. The effect of satellite growth and variation of disk parameters on satellite migration will be discussed. The migration in multiple satellite system, and how these settings can possibly result in the Laplace resonance among the Galilean satellites, will be also investigated. This work is supported in part by Hong Kong RGC grant HKU 7030/11P-
dc.languageengen_US
dc.relation.ispartofProtostars and Planetsen_US
dc.rightsCreative Commons: Attribution 3.0 Hong Kong License-
dc.titleOn the Migration of the Galilean Satellitesen_US
dc.typeConference_Paperen_US
dc.identifier.emailLee, MH: mhlee@hku.hken_US
dc.identifier.authorityLee, MH=rp00724en_US
dc.description.naturepublished_or_final_version-
dc.identifier.hkuros236925en_US
dc.identifier.spage278-
dc.identifier.epage279, abstract no. Poster 2K097-

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