Eccentricity Excitation and Apsidal Resonance Capture in the Planetary System Upsilon Andromedae

Details Eccentricity Excitation and Apsidal Resonance Capture in the Planetary System Upsilon Andromedae Eccentricity Excitation and Apsidal Resonance Capture in the Planetary System Upsilon Andromedae

2002-05-16

arxiv.org/abs/astro-ph/0205273v1

Astrophys.J. 576 (2002) 473-477

Astronomy and Astrophysics

Astrophysics

accepted to ApJ

Scientific paper

10.1086/341617

The orbits of the outer two known planets orbiting Upsilon Andromedae are remarkably eccentric. Planet C possesses an orbital eccentricity of e1 = 0.253. For the more distant planet D, e2 = 0.308. Previous dynamical analyses strongly suggest that the two orbits are nearly co-planar and are trapped in an apsidal resonance in which the difference between their longitudes of periastron undergoes a bounded oscillation about 0 degrees. Here we elucidate the origin of these large eccentricities and of the apsidal alignment. Resonant interactions between a remnant circumstellar disk of gas lying exterior to the orbits of both planets can smoothly grow e2. Secular interactions between planets D and C can siphon off the eccentricity of the former to grow that of the latter. Externally amplifying e2 during the phase of the apsidal oscillation when e2/e1 is smallest drives the oscillation amplitude towards zero. Thus, the substantial eccentricity of planet C and the locking of orbital apsides are both consequences of externally pumping the eccentricity of planet D over timescales exceeding apsidal precession periods of order 1e4 yr. We explain why the recently detected stellar companion to Upsilon Andromedae is largely dynamically decoupled from the planetary system.

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