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Issue A&A
Volume 448, Number 2, March III 2006
Page(s) 633 - 639
Section Interstellar and circumstellar matter
DOI http://dx.doi.org/10.1051/0004-6361:20053884

A&A 448, 633-639 (2006)
DOI: 10.1051/0004-6361:20053884

Moving shadows on the dusty disks of young stars

L. V. Tambovtseva1, 2, V. P. Grinin1, 2, 3 and G. Weigelt2

1  Main Astronomical Observatory Pulkovo, Pulkovskoe shosse 65, St. Petersburg 196140, Russia
    e-mail: tamb@gao.spb.ru; grinin@vg1723.spb.edu
2  Max-Planck-Institute für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
    e-mail: weigelt@mpifr-bonn.mpg.de
3  Crimean Astrophysical Observatory, Crimea, Nauchny, Ukraine

(Received 22 July 2005 / Accepted 25 October 2005 )

Abstract
We investigate the formation of moving shadows on the circumbinary (CB) disk of young binary systems. Moving shadows can be created by a dusty disk wind of the secondary component. The densest parts of the dusty disk wind and the associated common envelope can be optically thick and may block the stellar radiation inside a certain solid angle, resulting in the appearance of a moving shadow zone. Its shape and size depends on the mass loss rate, the disk wind velocity, and optical properties of the dust. Our calculations show that the shadow zone is observable if the mass loss rate $\dot M_{\rm w}$ is greater than 10 $^{-9} \,M_{\odot}$ per year. This shadow resembles a clock hand. If the orbit is an elliptical, the properties of this clock hand will change during the orbital motion of the secondary.


Key words: accretion, accretion disks -- stars: formation -- binaries: close -- circumstellar matter -- stars: pre-main sequence

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© ESO 2006


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