Volume 372, Number 3, June IV 2001
|Page(s)||L61 - L64|
|Published online||15 June 2001|
Asymmetries in the HD 141569 cir cum stel lar disk*
Laboratoire d'Astrophysique de l'Observatoire de Grenoble, Université J. Fourier/CNRS, BP 53, 38041 Grenoble Cedex 9, France
2 DSM/DAPNIA/Service d'Astrophysique, CEA/Saclay, 91191 Gif-sur-Yvette, France
3 Canada-France-Hawaii Telescope Corporation, PO Box 1597, Kamuela, HI 96743, USA
Corresponding author: D. Mouillet, email@example.com
Accepted: 9 May 2001
We present HST/STIS coronagraphic observations of the disk around HD 141569. The data, with a spatial resolution and signal to noise higher than those previously obtained with HST/NICMOS2 allow a more detailed insight in the system. They reveal a very structured system, in which two ring-like structures at distances 200 and 325 AU from the star are the most prominent features. The region between 125 and 175 AU is clearly devoid of material. An arc-like structure is also detected at about 250 AU, as well as a diffuse extended emission, both on the North side of the disk. The system appears to be highly asymmetrical, both with respect to its major and minor axes. Surprisingly, the brightness asymmetry with respect to both axes in the inner and outer parts of the disk is reversed. Possible explanations to the asymmetries include anisotropic scattering and/or non axisymmetrical distribution of the dust within the system. It is shown that anisotropic scattering cannot alone be responsible for all observed asymmetries. It is concluded that HD 141569 disk is non axi-symmetrical. Eventhough no detailed modeling is given in this observational paper, it is probable that the sculpting and brightness properties of the disk are due to the gravitational perturbation of a massive body.
Key words: stars: cir cum stel lar matter / stars: HD 141569, β Picto ris, planetary formation, circumstellar disks, young stars
© ESO, 2001
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