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Tidal interactions of close-in extrasolar planets with their host stars Ludmila Carone

Tidal interactions of close-in extrasolar planets with their host stars Ludmila Carone Institut für Geophysik und Meterologie Universität zu Köln, Cologne, Germany 5th Corot Week, 11. December 2003 in Berlin. Very close-in extrasolar planets. Tides raised by the star on the planet.

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Tidal interactions of close-in extrasolar planets with their host stars Ludmila Carone

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  1. Tidal interactions of close-in extrasolar planets with their host stars Ludmila Carone Institut für Geophysik und Meterologie Universität zu Köln, Cologne, Germany 5th Corot Week, 11. December 2003 in Berlin

  2. Very close-in extrasolar planets

  3. Tides raised by the star on the planet • Close-in extrasolar planets (a < 0.05 AU) experience extreme gravitational interaction • ->Tidal bulge on planet -> synchronous rotation (rotation = revolution)

  4. Time to reach synchronous rotation • Tides raised by the star on the planet • -> synchronous rotation of the planet -> depends on planetary mass and radius

  5. Time to reach synchronous rotation all planets a < 0.20 AU

  6. Tides raised by the planet on the star • Tidal bulge on the host star • -> increase/decrease of semi major axis -> decrease/increase of stellar rotation

  7. Tidal evolution • Tides raised by the planet on the star • decrease/increase of semi major axis • Spin-up/decrease of star rotation depends on planetary mass and star radius

  8. The parameters k* and Q* • Evolution time scale depends strongly on stellar love number k*and the stellar tidal dissipation factor Q* • Pätzold & Rauer (2002) favor:

  9. OGLE-TR-56b (an extreme planet) • OGLE-TR-56b was discovered during the OGLE-survey (Konacki et al, 2003) • Parameters: • extremly close distance to its host star & large mass -> very strong tidal interactions

  10. OGLE-TR-56b: Evolution of semi major axis

  11. OGLE-TR-56b: Evolution of stellar rotation

  12. OGLE-TR-56b: Evolution of stellar rotation(only in convection envelope)

  13. Time to reach roche limit

  14. Conclusion • OGLE-TR-56b may reach the roche limit within the lifetime of its host star • Tidal effects could lead to a considerable spin up in stellar rotation • Even more so, when only spin-up in convection envelope is considered (no friction between core and envelope) • The strength of tidal effects depends strongly on the planet‘s mass and the semi major axis • But for a better prediction the geophyisical properties Q* and k* have to be determined -> we need more data

  15. Very close-in extrasolar planets

  16. OGLE-TR-3b: Evolution of semi major axis

  17. OGLE-TR-3b: Evolution of stellar rotation

  18. OGLE-TR-3b: Evolution of stellar rotation(only in convection envelope)

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