EDP Sciences
Free access
Issue
A&A
Volume 414, Number 3, February II 2004
Page(s) 1153 - 1164
Section Planets and planetary systems
DOI http://dx.doi.org/10.1051/0004-6361:20031622


A&A 414, 1153-1164 (2004)
DOI: 10.1051/0004-6361:20031622

Structuring the HD 141569 A circumstellar dust disk

Impact of eccentric bound stellar companions
J. C. Augereau1 and J. C. B. Papaloizou2

1  Leiden Observatory, PO Box 9513, 2300 Leiden, The Netherlands
2  Astronomy Unit, School of Mathematical Sciences, Queen Mary & Westfield College, Mile End Road, London E1 4NS, UK

(Received 26 May 2003 / Accepted 14 October 2003)

Abstract
Scattered light images of the optically thin dust disk around the 5 Myr old star HD 141569 A have revealed its complex asymmetric structure. We show in this paper that the surface density inferred from the observations presents similarities with that expected from a circumprimary disk within a highly eccentric binary system. We assume that either the two M stars in the close vicinity of HD 141569 A are bound companions or at least one of them is an isolated binary companion. We discuss the resulting interaction with an initially axisymmetric disk. This scenario accounts for the formation of a spiral structure, a wide gap in the disk and a broad faint extension outside the truncation radius of the disk after 10-15 orbital periods with no need for massive companion(s) in the midst of the disk resolved in scattered light. The simulations match the observations and the star age if the perturber is on an elliptic orbit with a periastron distance of 930 AU and an eccentricity from 0.7 to 0.9. We find that the numerical results can be reasonably well reproduced using an analytical approach proposed to explain the formation of a spiral structure by secular perturbation of a circumprimary disk by an external bound companion. We also interpret the redness of the disk in the visible reported by Clampin et al. (2003) and show that short-lived grains one order of magnitude smaller than the blow-out size limit are abundant in the disk. The most probable reason for this is that the disk sustains high collisional activity. Finally we conclude that additional processes are required to clear out the disk inside 150 AU and that interactions with planetary companions possibly coupled with the remnant gas disk are likely candidates.


Key words: stars: planetary systems -- stars: HD 141569 -- stars: planetary systems: formation

Offprint request: J. C. Augereau, augereau@strw.leidenuniv.nl

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