Computer Science
Scientific paper
Oct 2005
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005nrdd.conf...30r&link_type=abstract
Proceedings of the Miniworkshop on Nearby Resolved Debris Disks. October 19-20, 2005. Space Telescope Science Institute, Baltimo
Computer Science
Scientific paper
The debris dust disk around Vega has been the subject of several studies in the recent years. Submillimeter and infrared images of the disk have revealed very different aspects (Holland et al. 1998, Su et al. 2005). Infrared observations show a quite uniform and smooth disk, while in submillimeter observations a very asymmetric disk appears with two main distinct regions of emission. The probable explanation for these differences is that at each wavelength domain we see a dust population with a specific size range. The dynamics of dust particles is indeed controlled by radiation pressure which depends highly on their size. There are thus two separate issues related to the dynamics of this disk : First, one needs to explain the strong asymmetries in the submillimeter observations, and second, the link between the size of the particles and the wavelength domain needs to specified.
The scenario often invoked to explain the asymmetries is inspired by Kuiper belt studies in the Solar System. It involves a Neptune-like planet migrating towards external regions of the debris disk. During this migration, the planet traps many dust particles in its mean-motion resonance. The dust spatial distribution is then no longer axisymmetric but presents structures able to generate the observed asymmetries. Wyatt (2003) has made the most complete dynamic study for this scenario applied to Vega. He used a semi-analytical approach to find the best orbital and migration parameters of the suspected planet. He has nevertheless assumed two hypotheses: the planet is on a circular orbit and the radiation pressure is null. We have reinvestigated this scenario using symplectic integration, testing in particular the importance of these two hypotheses. We have found that the asymmetries are very sensitive to the radiation pressure and to the eccentricity of the planet. Either with a small eccentricity (0.05) or with a small radiation pressure, they disappear. Although the original model is still valid, this motivates us for a further investigation of this problem (for instance with very eccentric planets) in order to find more robust solutions.
Augereau Jean-Charles
Beust Hervé
Reche Rémy
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