Dust Distribution in Gas Disks. A Model for the Ring Around HR 4796A

Details Dust Distribution in Gas Disks. A Model for the Ring Around HR 4796A Dust Distribution in Gas Disks. A Model for the Ring Around HR 4796A

2000-07-27

arxiv.org/abs/astro-ph/0007422v2

Astronomy and Astrophysics

Astrophysics

proof read version, 26 pages, LaTex, 11 figures. To appear in The Astronomical Journal June 2001

Scientific paper

10.1086/321419

There have been several model analyses of the near and mid IR flux from the circumstellar ring around HR4796A. In the vicinity of a young star, the possibility that the dust ring is embedded within a residual protostellar gas disk cannot be ruled out. In a gas-rich environment, larger sizes ($>100 \mu m$) are needed for the particles to survive the radiative blow out. The total dust mass required to account for the IR flux is $< 10^{-1} M_\oplus$. The combined influence of gas and stellar radiation may also account for the observed sharp inner boundary and rapidly fading outer boundary of the ring. The pressure gradient induced by a small (10%) amplitude variation in the surface density distribution of a low-mass gaseous disk would be sufficient to modify the rotation speed of the gas.

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