Other
Scientific paper
May 2000
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000dda....31.0102r&link_type=abstract
American Astronomical Society, DDA Meeting #31, #01.02; Bulletin of the American Astronomical Society, Vol. 32, p.856
Other
Scientific paper
We present results of long-term numerical orbital integrations designed to test the stability of the three-planet system orbiting υ Andromedae. Our initial conditions are based on the latest fit to the radial velocity data obtained by the Marcy planet-search group at Lick Observatory. In comparison with the fit they presented last year (Butler et al. 1999, ApJ 526, 916), the fit for the outer planet has significantly changed; the eccentricity has dropped from 0.36 to 0.31 and the period has increased from 1269 to 1319.7 days. Assuming that the middle planet is inclined by 1o with respect to the plane containing the other two bodies, we multiplied the planetary masses by some mass factor mf ≡ 1/sin i. An approximate analytic analysis of the star and the two outer planets shows that this subsystem is Hill stable for mf up to 10 (note that this approximation is not very good for large mf). Our integrations involving all three planets show that the system is typically stable for at least 5 Myr for mf <= 5. In comparison, our analysis using the initially announced observed orbital elements (Rivera & Lissauer 2000, ApJ 530, 454), resulted in analogous systems which became unstable on time scales less than 1 Myr for mf>2. We observed a secular resonance between the outer two planets in both our previous and current analyses. This research was supported in part by NASA's OSSRP under grant NAG 5-4640.
Lissauer Jack . J.
Rivera Eugenio J.
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