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D.R. Ardila (Johns Hopkins University), S.H. Lubow, J.E. Krist (Space Telescope Science Institute), D.A. Golimowski (Johns Hopkins University), M. Clampin (Goddard Space Flight Center), G.F. Hartig (Space Telescope Science Institute), H.C. Ford (Johns Hopkins University), J.D. Illingworth (UCO/Lick Observatory)
HD 141569A is a 5 Myr old, A0V star, 99 pc away from the sun. It is part of a triple system. The star has a circumstellar disk, and optical and near-IR images show that the disk possesses a great deal of structure: an inner hole within 100 AU of the star, almost devoid of dust, and a double ring (or perhaps a series of broken spirals) at about 300-400 AU. Recent HST-ACS images further reveal two large spiral arms. The disk is one of a small group of optically resolved debris disks, and so understanding the origin of its structure may shed light in the relevant processes sculpting in other disks. In this poster, we attempt to model the disk characteristics as due primarily to the interaction of planetesimals in the disk with the central star and the binary HD 141569B/C. We assume that the binary is unbound from HD 141569A and so the interaction is a parabolic fly-by. We model the effect of radiation pressure and the presence of gas in the small dust particles. ACS was developed under NASA contract NAS 5-32865, and this research is supported by NASA grant NAG5-7697. We are grateful for an equipment grant from the Sun Microsystems, Inc.
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Bulletin of the American Astronomical Society, 35#5
© 2003. The American Astronomical Soceity.