Conclusions

Large-scale dust structures should exist in the outer Solar System due to perturbations from Neptune. Similar interactions between dust disks and unseen planets should also exist in many extrasolar planetary systems. Using structures on a dust disk to detect and characterize planets provides a different way for extrasolar planet detection. In some cases, for example if a system has a close-to-face on orientation and/or the planet is very far away from the central star, this method may be more powerful than any other.

Figure 1. A simulated image of the e Eridani disk with a Jupiter-like planet in the system.

Figure 2. The observed e Eridani disk, adapted from [7].

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