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Issue A&A
Volume 370, Number 2, May I 2001
Page(s) 447 - 455
Section Formation, structure and evolution of stars
DOI http://dx.doi.org/10.1051/0004-6361:20010199



A&A 370, 447-455 (2001)
DOI: 10.1051/0004-6361:20010199

Dynamical modeling of large scale asymmetries in the $\beta$ Picto ris dust disk

J. C. Augereau1, R. P. Nelson2, A. M. Lagrange1, J. C. B. Papaloizou2 and D. Mouillet1

1  Laboratoire d'Astrophysique de l'Observatoire de Grenoble, Université J. Fourier, CNRS, BP 53, 38041 Grenoble Cedex 9, France
2  Astronomy Unit, School of Mathematical Sciences, Queen Mary & Westfield College, Mile End Road, London E1 4NS, UK

(Received 27 October 2000 / Accepted 19 January 2001)

Abstract
We report a new and complete model of the $\beta$ Picto ris disk, which succeeds in accounting for both the surface brightness distribution, warp characteristics, the outer "butterfly"asymmetry as observed by HST/STIS in scattered light, as well as the infrared emission. Our model includes the presence of a disk of planetesimals extending out to 120-150 AU, perturbed gravitationally by a giant planet on an inclined orbit, following the approach of Mouillet et al. (1997b). At any time, the planetesimal disk is assumed to be the source of a distribution of grains produced through collisional evolution, with the same initial orbital parameter distribution. The steady state spatial grain distribution is found incorporating the effects of radiation pressure which can cause the distribution of the smallest particles to become very distended. With realistic assumptions about the grains' chemical properties, the modeling confirms the previously evident need for an additional population of hot grains close to the star, to account for the 12 $\mu$m fluxes at short distances from the star. It also indicates that this population cannot explain the outer 12 $\mu$m flux distribution when the effects of gravity and radiation pressure determine the distribution. Very small grains, produced by collisions among aggregates, are tentatively proposed to account for this 12 $\mu$m outer emission.


Key words: stars: cir cum stel lar matter -- stars: $\beta$ Picto ris

Offprint request: J. C. Augereau, augereau@obs.ujf-grenoble.fr

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