Other
Scientific paper
Jan 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21741501b&link_type=abstract
American Astronomical Society, AAS Meeting #217, #415.01; Bulletin of the American Astronomical Society, Vol. 43, 2011
Other
Scientific paper
The planetary system of υ Andromedae is the first to display evidence for mutually inclined orbits around a main sequence star (McArthur et al. 2010). Moreover, the planets υ And c and d have orbital elements that oscillate with large amplitudes and lie very close to the limits of stability. The substantial mutual inclination, as well as its other orbital characteristics, may offer insight into the dynamical history of this system, and thus into planetary formation processes in general. The υ And system may be influenced by a nearby low-mass star, υ And B, which could perturb the planetary orbits, but the effect is too weak to modify two coplanar orbits into the observed mutual inclination of 30 degrees. However, it could have perturbed the original planetary system enough to incite encounters or collisions among the planets that subsequently raised the mutual inclinations of the remaining planets to the current values. Our simulations do produce systems similar to that of υ And, although even with the high inclinations they tend to be further from the stability boundary than suggested by the current best orbits for the observed system. Thus, scattering is a plausible mechanism to explain the observed inclinations of υ And c and d. While, perturbations from υ And B may have incited the scattering, it may also have been caused by instabilities among the planets themselves. We also examine a wide range of masses and orbits for planet b, which has not been detected astrometrically, in order to constrain the parameter space that can support a stable three-planet system.
Antonsen A.
Barnes Rory
Benedict George F.
Greenberg Richard
McArthur Barbara
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