1. 1 Why exoplanets have so high eccentricities - By Line Drube - November 2004

2. 2 of 17 Characteristic of exoplanets Over 130 planets found by - Doppler Spectroscopy - The stars light curve Mass distribution 0.1 to10 Mj Brown dwarf desert

3. 3 of 17 All is under 5.9 AU Smallest orbit 0.038 AU (Mercury 0.38 AU) Within the snow line of 4-5 AU Migration Table of all planets and their semimajor axis

4. 4 of 17 Eccentricities High eccentricity small orbits Median eccentricity: 0.28 Pluto’s e = 0.25 Planet expected to have circular orbits.

5. 5 of 17 Theories for the eccentricities Close encounters between planets Resonant interactions between planets Interaction with the protoplanetary disk Interaction with a distant companion star Propagation of eccentricity disturbances Formation from protostellar cloud

6. 6 of 17 Close encounters between planets (1) During formation 1) Masses increase & differential migration => dynamical instability Or 2) The planets mutual perturbed each other => instability Ejection or collision 1 planet far out & 1 close Explains the migration inwards

7. 7 of 17 Close encounters between planets (2) Problem: Ecc. distribution: too many in close circular orbit, median ecc. 0.6. Equal masses Expected: small m => higher ecc.

8. 8 of 17 Resonant interactions between planets (1) Differential inward migration Migration caused by a torques from interactions between planet and disk Locked in orbital resonances Continued migration => ecc. Pluto/Neptune (outwards)

9. 9 of 17 Resonant interactions between planets (2) Problems Needs extremely strong ecc. dampening. Have to be captured just before migration stops Have mostly observed single planets Expected: low-mass planets to have higher ecc.

10. 10 of 17 Interaction with the protoplanetary disk Interactions at certain resonances can excite or dampen ecc. The dampening resonances are easier to saturate => ecc. can grow Problem: Many parameters Numerical 2D simulation, shows only ecc. growth for >10Mj

11. 11 of 17 Interaction with a distant companion star Binary stars A weak tidal force can excited large ecc. Force needs to be stronger than other effect Problems Expected: multi-planet system have low ecc. Expected: high ecc. in binary system. Unseen companions?

12. 12 of 17 Propagation of eccentricity disturbances (1) During formation: Stars passing within a couple 10 2 AU Excite outer planetesimals Propagate inwards as a wave In solar neighborhood values => ecc 0.01-0.1 Dense open clusters => higher ecc.

13. 13 of 17 Propagation of eccentricity disturbances (2) Problems: Works only with a long-lived extended disk Works only in dense open clusters It haven’t been shown if this reproduce the ecc. distribution.

14. 14 of 17 Formation from protostellar cloud (1) Protoplanetary disk vs. protostellar cloud Same distribution of periods and eccentricities as binary stars.

15. 15 of 17 Formation from protostellar cloud (2) Problems: Fragmatation Brown dwarf desert

16. 16 of 17 Conclusion None of the theories can explain everything Likely a combination of several mechanisms Future: Better statistic with more planets Finding smaller planets and longer periods. Giving new clues to the mystery.

17. 17 of 17 References Tremaine S., Zakamska N.L., “Extrasolar Planet Orbits and Eccentricities” by. arXiv 2003 Tremaine S., Zakamska N.L., “Excitation and progation of eccentricity disturbances in planetary system”, 2004 ApJ Zucker S., Mazeh T., “Derivation of the mass distribution of extrasolar planets with MAXLIMA.”, 2001 ApJ Stepinski T.F. and Black D.C., “On orbital elements of extrasolar planetary candidates and spectroscopic binaries”, 2001 A&A Marzari F., Weidenschilling S.J., “Eccentric Extrasolar Planets: The Jumping Jupiter Model”, 2002 Icarus Ivanov P.B., Papaloizou J.C.B., “On the tidal interaction of massive extrasolar planets on highly eccentric orbits”, 2004 Mon.Not.R.Astron.Soc Marcy G., Butler P., http://exoplanets.org