Dynamical Stability of Terrestrial and Giant Planets in the HD 155358 Planetary System

Details Dynamical Stability of Terrestrial and Giant Planets in the HD 155358 Planetary System Dynamical Stability of Terrestrial and Giant Planets in the HD 155358 Planetary System

Oct 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007dps....39.2207h&link_type=abstract

American Astronomical Society, DPS meeting #39, #22.07; Bulletin of the American Astronomical Society, Vol. 39, p.451

Astronomy and Astrophysics

Astronomy

Scientific paper

We present the results of a study of the dynamical evolution and the habitability of the system HD 155358. This system is unique in that it is one of the two low metallicity stars discovered to host a multiple planet system. HD 155358 is host to two Jupiter-sized planets, with minimum masses of 0.86 and 0.50 Jupiter-masses. The orbit of the lower mass planet of this system is located at the inner edge of the system's habitable zone. To determine whether this system can harbor terrestrial-type planets, we numerically integrated the orbits of its planets and an Earth-like object for different values of their masses and orbital eccentricities. Results indicate that this system could potentially host stable orbits for terrestrial-sized planets in its habitable zone, but the stability of these orbits is very sensitive to the precise characteristics of the giant planets of the system. We also studied the long term stability of larger bodies (Neptune- and Saturn-mass) in the system. Our results show that a Neptune- or Saturn-mass body could exist in stable orbits in this system fairly close in, potentially within the range of present detection techniques, again depending on the precise configurations of the giant planets.

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