Paper: astro-ph/0508452
Date: Mon, 22 Aug 2005 13:00:21 GMT (554kb)

Title: Dust distribution in protoplanetary disks - Vertical settling and radial
migration

Authors: Laure Barri\`{e}re-Fouchet (CRAL), Jean-Fran\c{c}ois Gonzalez (CRAL),
James R. Murray, Robin J. Humble (CITA), Sarah T. Maddison

Comments: Accepted for publication in Astronomy & Astrophysics. 11 pages, 6
figures
Proxy: ccsd ccsd-00008105
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We present the results of a three dimensional, locally isothermal,
non-self-gravitating SPH code which models protoplanetary disks with two
fluids: gas and dust. We ran simulations of a 1 Msun star surrounded by a 0.01
Msun disk comprising 99% gas and 1% dust in mass and extending from 0.5 to ~300
AU. The grain size ranges from 0.001 mm to 10 m for the low resolution (~25 000
SPH particles) simulations and from 0.1 mm to 10 cm for the high resolution
(~160 000 SPH particles) simulations. Dust grains are slowed down by the
sub-Keplerian gas and lose angular momentum, forcing them to migrate towards
the central star and settle to the midplane. The gas drag efficiency varies
according to the grain size, with the larger bodies being weakly influenced and
following marginally perturbed Keplerian orbits, while smaller grains are
strongly coupled to the gas. For intermediate sized grains, the drag force
decouples the dust and gas, allowing the dust to preferentially migrate
radially and efficiently settle to the midplane. The resulting dust
distributions for each grain size will indicate, when grain growth is added,
the regions when planets are likely to form.

\\ ( http://arXiv.org/abs/astro-ph/0508452 , 554kb)

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Paper: astro-ph/0504555
replaced with revised version Mon, 22 Aug 2005 17:31:13 GMT (742kb)

Title: Measurement of Spin-Orbit Alignment in an Extrasolar Planetary System

Authors: Joshua N. Winn, Robert W. Noyes, Matthew J. Holman, David Charbonneau,
Yasuhiro Ohta, Atsushi Taruya, Yasushi Suto, Norio Narita, Edwin L. Turner,
John A. Johnson, Geoffrey W. Marcy, R. Paul Butler, Steven S. Vogt

Comments: 21 pages, 6 figures. To match the version accepted by ApJ. Errors
have been corrected in Table 1. (In previous versions, some confidence limits
were mistakenly 80% rather than 90% limits.)

\\ ( http://arXiv.org/abs/astro-ph/0504555 , 742kb)