The two-fluid analysis of the Kelvin-Helmholtz instability in dusty layer of a protoplanetary disk: A possible path toward the planetesimal formation through the gravitational instability

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dc.creatorMichikoshi, Shugo
dc.creatorInutsuka, Shu-ichiro
dc.date2004-12-28
dc.date2006-04-14
dc.date.accessioned2026-07-07T06:37:06Z
dc.date.available2026-07-07T06:37:06Z
dc.descriptionWe analyze the stability of dust layer in protoplanetary disk to understand the effect of the relative motion between gas and dust. The previous analyses not including the effect of relative motion between gas and dust show that the shear-induced turbulence may prevent the dust grains from settling sufficiently to be gravitationally unstable. We determine the growth rate of Kelvin-Helmholtz instability in wide range of parameter space, and propose a possible path toward the planetesimal formation through the gravitational instability. We expect the density of dust layer becomes $ρ_\mathrm{d}/ρ_\mathrm{g} \sim 200$ if the dust grains can grow up to 5m.
dc.description43 pages, 30 figures
dc.identifierhttps://arxiv.org/abs/astro-ph/0412643
dc.identifierhttp://arxiv.org/abs/astro-ph/0412643
dc.identifierAstrophys.J. 641 (2006) 1131-1147
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/100277
dc.subjectAstrophysics
dc.titleThe two-fluid analysis of the Kelvin-Helmholtz instability in dusty layer of a protoplanetary disk: A possible path toward the planetesimal formation through the gravitational instability
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