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Conference Paper: The formation environment of the Galilean Moons

TitleThe formation environment of the Galilean Moons
Authors
KeywordsAstronomy
Issue Date2010
PublisherAmerican Astronomical Society. The Journal's web site is located at http://www.aas.org/publications/baas/baas.html
Citation
The 42nd Annual Meeting of the Division for Planetary Sciences of the American Astronomical Society, Pasadena, CA., 3-8 October 2010. In Bulletin of the American Astronomical Society, 2010, v. 42 n. 4, p. 959 How to Cite?
AbstractThe regular satellites of the gas giant planets were formed in circumplanetary disks of gas and dust, whose evolution was governed by mass and angular momentum transport of uncertain origins. Turbulence driven by the magneto-rotational instability can provide the transport if the gas is sufficiently ionised to couple to the embedded magnetic fields. We compute the ionisation states of the minimum-mass and gas-starved models of the Jovian sub-nebula, including the key effects known from Solar nebula studies: ionisation by cosmic rays and stellar X-rays, charge transfer to metal atoms, and recombination on grains. The results show that magneto-rotational turbulence develops in a region whose size depends on the absorbing mass column, the grain surface area, the gas-phase metal abundance and the strength of the turbulent mixing. The turbulence is almost entirely absent from the minimum-mass sub-nebula model over a wide range in these parameters. In contrast, turbulence occurs in the gas-starved model in the surface layers and throughout the parts furthest from the planet, provided sub-micron grains are underabundant. This work was carried out in part at the Jet Propulsion Laboratory, California Institute of Technology with support from the NASA Outer Planets Research program, and at the University of Hong Kong under RGC grant HKU 7024/08P.
DescriptionPoster - Session 24. Solar System Origin, Planet and Satellite Formation: 24.08
Persistent Identifierhttp://hdl.handle.net/10722/141321
ISSN

 

DC FieldValueLanguage
dc.contributor.authorTurner, NJen_US
dc.contributor.authorLee, MHen_US
dc.contributor.authorSano, Ten_US
dc.date.accessioned2011-09-23T06:30:38Z-
dc.date.available2011-09-23T06:30:38Z-
dc.date.issued2010en_US
dc.identifier.citationThe 42nd Annual Meeting of the Division for Planetary Sciences of the American Astronomical Society, Pasadena, CA., 3-8 October 2010. In Bulletin of the American Astronomical Society, 2010, v. 42 n. 4, p. 959en_US
dc.identifier.issn0002-7537-
dc.identifier.urihttp://hdl.handle.net/10722/141321-
dc.descriptionPoster - Session 24. Solar System Origin, Planet and Satellite Formation: 24.08-
dc.description.abstractThe regular satellites of the gas giant planets were formed in circumplanetary disks of gas and dust, whose evolution was governed by mass and angular momentum transport of uncertain origins. Turbulence driven by the magneto-rotational instability can provide the transport if the gas is sufficiently ionised to couple to the embedded magnetic fields. We compute the ionisation states of the minimum-mass and gas-starved models of the Jovian sub-nebula, including the key effects known from Solar nebula studies: ionisation by cosmic rays and stellar X-rays, charge transfer to metal atoms, and recombination on grains. The results show that magneto-rotational turbulence develops in a region whose size depends on the absorbing mass column, the grain surface area, the gas-phase metal abundance and the strength of the turbulent mixing. The turbulence is almost entirely absent from the minimum-mass sub-nebula model over a wide range in these parameters. In contrast, turbulence occurs in the gas-starved model in the surface layers and throughout the parts furthest from the planet, provided sub-micron grains are underabundant. This work was carried out in part at the Jet Propulsion Laboratory, California Institute of Technology with support from the NASA Outer Planets Research program, and at the University of Hong Kong under RGC grant HKU 7024/08P.-
dc.languageengen_US
dc.publisherAmerican Astronomical Society. The Journal's web site is located at http://www.aas.org/publications/baas/baas.html-
dc.relation.ispartofBulletin of the American Astronomical Societyen_US
dc.rightsBulletin of the American Astronomical Society. Copyright © American Astronomical Society.-
dc.subjectAstronomy-
dc.titleThe formation environment of the Galilean Moonsen_US
dc.typeConference_Paperen_US
dc.identifier.emailLee, MH: mhlee@hku.hken_US
dc.identifier.authorityLee, MH=rp00724en_US
dc.identifier.hkuros194799en_US
dc.identifier.volume42-
dc.identifier.issue4-
dc.identifier.spage959-
dc.identifier.epage959-
dc.description.otherThe 42nd Annual Meeting of the Division for Planetary Sciences of the American Astronomical Society, Pasadena, CA., 3-8 October 2010. In Bulletin of the American Astronomical Society, 2010, v. 42 n. 4, p. 959-

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