Investigating the flyby scenario for the HD141569 system

Details Investigating the flyby scenario for the HD141569 system Investigating the flyby scenario for the HD141569 system

Feb 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aipc.1094..405b&link_type=abstract

COOL STARS, STELLAR SYSTEMS AND THE SUN: Proceedings of the 15th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun.

Astronomy and Astrophysics

Astronomy

Circumstellar Shells, Clouds, And Expanding Envelopes, Circumstellar Masers, Molecular And Chemical Processes And Interactions, Celestial Mechanics

Scientific paper

The debris dust disk around HD 141569 assumes a complex structure, with gaps, asymmetric features and a spiral structure. At least part of these features, are supposed to be due to the gravitational influence of the two M2-M4 stellar companions of the primary star. Recent observations have been able to re-measure the radal velocities of the components of this system. The two low mass companions are unbound to the system. Using radial velocity and proper motion constraints we are able to contrain the fly-by orbit. Using symplectic integration tools, we simulate the gravitational perturbation of the passing stars on the dust disk. The flyby scenario reproduces most of the observed features in the disk. However, not all structures are explained by this model. We then add a hidden planet in the disk to the simulations. With this planet+flyby model, the present shape of the disk can be much better reproduced this way. We also derive constraints on the characteristics of the suspected planet. Subsequently, we discuss the implications of this scenario. It turns out that the three stars probably formed formerly a bound system, on a more distant orbit. A passing star then perturbed the companions at apoastron, thus making them unbound to the primary.

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