Secular resonance in extrasolar system

Details Secular resonance in extrasolar system Secular resonance in extrasolar system

Apr 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003eaeja....13896r&link_type=abstract

EGS - AGU - EUG Joint Assembly, Abstracts from the meeting held in Nice, France, 6 - 11 April 2003, abstract #13896

Astronomy and Astrophysics

Astronomy

Scientific paper

The two orbits in the HD 160691 planetary system at first appeared highly unstable, but using a new technique called MEGNO (the acronym of Mean Exponential Growth factor of Nearby Orbits), we were able to identify a stability valley in the parameter space. This stability zone is due to the 2:1 mean motion resonance coupled with relative orbital positions of the planets avoiding close approaches in the closeness of their periastron, the two apsidal lines being anti-aligned. The mechanism itself is preserved by librations of the mean motion resonance variables while the longitudes of periapse on average precess at the same rate. The secular resonance variable of the HD 160691 system librates around 180o while it librates around 0o in the Gliese 876 system. We present an extended study of such mechanisms to the Io-Europa pair and the planetary system HD 82943 in order to compare in details these four original cases of secular resonances associated to the 2:1 resonance (Io-Europa, Gliese 876, HD 82943, HD 160691). We concluded that in order to be dynamically stable, the extrasolar planetary systems close to the 2:1 mean motion resonance have to satisfy an apsidal secular resonance and apparently high eccentricities. Because of high eccentricities of the orbits, and despite their relatively small semi-major axes, the relative distances between the two planets may indeed remain sufficiently large over the whole evolutionary time scale of the system.

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