1. Are there Planets outside the Solar System ? First answer : 1992 Discovery of the first Extra-Solar Planet around the pulsar PSR1257+12 (Wolszczan &Frail) First answer : 1992 Discovery of the first Extra-Solar Planet around the pulsar PSR1257+12 (Wolszczan &Frail) Are there Planets moving around other Sun-like stars ? Are there Planets moving around other Sun-like stars ?

2. The EXO Planet: 51 Peg b Mass: M sin i = 0.468 m_Jup Mass: M sin i = 0.468 m_Jup semi-major axis: a = 0.052 AU semi-major axis: a = 0.052 AU period: p = 4.23 days period: p = 4.23 days eccentricity: e = 0 eccentricity: e = 0 a of Mercury: 0.387 AU a of Mercury: 0.387 AU Discovered by: Michel Mayor Didier Queloz

3. Status of Observations 292 Extra-solar planetary systems 292 Extra-solar planetary systems 337 Planets near other solar-type stars 337 Planets near other solar-type stars 33 Mulitple planetary systems 33 Mulitple planetary systems 43 Planets in binaries 43 Planets in binaries 292 Extra-solar planetary systems 292 Extra-solar planetary systems 337 Planets near other solar-type stars 337 Planets near other solar-type stars 33 Mulitple planetary systems 33 Mulitple planetary systems 43 Planets in binaries 43 Planets in binaries

4.  Binaries  Single Star and Single Planetary Systems  Multi-planetary systems

5. Interesting Questions How frequent are other planetary systems ? How frequent are other planetary systems ? Are they like our Solar System (no. of planets, masses, radii, albedos, orbital paramenters, …. ) Are they like our Solar System (no. of planets, masses, radii, albedos, orbital paramenters, …. ) What type of environments do they have? (atmospheres, magnetosphere, rings, … ) What type of environments do they have? (atmospheres, magnetosphere, rings, … ) How do they form and evolve ? How do they form and evolve ? How do these features depend on the type of the central star (mass, chemical composition, age, binarity, … ) ? How do these features depend on the type of the central star (mass, chemical composition, age, binarity, … ) ?

6. 55 Cancri 5 Planeten bei 55 Cnc: 5 Planeten bei 55 Cnc: 55Cnc d -- the only known Jupiter-like planet in Jupiter- distance 55Cnc d -- the only known Jupiter-like planet in Jupiter- distance Binary: a _ binary = 1000 AU

7. Extra-solare Planeten ca. 130 Planeten entdeckt ca. 130 Planeten entdeckt massereich (~M jup ) massereich (~M jup ) enge Umlaufbahnen enge Umlaufbahnen Radialgeschwindigkeits- messungen Radialgeschwindigkeits- messungen

8. Mass distribution

9. Only 28% of the detected planets have masses < 1 Jupitermass Only 28% of the detected planets have masses < 1 Jupitermass About 33% of the planets are closer to the host-star than Mercury to the Sun About 33% of the planets are closer to the host-star than Mercury to the Sun Nearly 60% have eccentricities > 0.2 Nearly 60% have eccentricities > 0.2 And even 40% have eccentricities > 0.3 And even 40% have eccentricities > 0.3 Facts about Extra-Solar Planetary Systems:

10. Distribution of the detected Extra-Solar Planets Mercury Earth Mars Venus Jupiter

11. TemperatureLifetime 315 stars Target Stars for Darwin/TPF AF G K M 10 pc

12. Sources of uncertainty in parameter fits:  the unknown value of the orbital line-of-sight inclination i allows us to determine from radial velocities measurements only the lower limit of planetary masses;  the relative inclination i r between planetary orbital planes is usually unknown.  In most of the mulitple-planet systems, the strong dynamical interactions between planets makes planetary orbital parameters found – using standard two-body keplerian fits – unreliable (cf. Eric Bois) All these leave us a substantial available parameter space to be explored in order to exclude the initial conditions which lead to dynamically unstable configurations All these leave us a substantial available parameter space to be explored in order to exclude the initial conditions which lead to dynamically unstable configurations

13. Major catastrophe in less than 100000 years (S. Ferraz-Mello, 2004)

14. Long-term numerical integration: Stability-Criterion: No close encounters within the Hill‘ sphere (i)Escape time (ii) Study of the eccentricity: maximum eccentricity Chaos Indicators: Fast Lyapunov Indicator (FLI ) C. Froeschle, R.Gonczi, E. Lega (1996) MEGNO RLI Helicity Angle LCE Numerical Methods

15.  Binaries  Single Star and Single Planetary Systems  Multi-planetary systems

16. OGLE 06-109L Planet b: (0.71 +/-0.08 M J ) a=2.3 +/-0.2 AU a=2.3 +/-0.2 AU e= ? e= ? P = 1825 (+/- 365) d P = 1825 (+/- 365) d Planet c: (0.27 +/- 0.03 M J ) Planet c: (0.27 +/- 0.03 M J ) a = 4.6 (+/-0.5) AU a = 4.6 (+/-0.5) AU e = 0.11 e = 0.11 i = 59 deg i = 59 deg P = 5100 (+/-730) d P = 5100 (+/-730) d

17. www.univie.ac.at/adg/exostab/ ExoStab appropriate for single-star single-planet system - Stability of an additional planet - Stability of the habitable zone (HZ) - Stability of an additional planet with repect to the HZ

18. Stability of an additional planet known parameters of system: mass of star [M_sun]: 0.5 mass of giant planet [M_jup]: 0.21 semi-major axis of giant planet [AU]: 4.6 eccentricity of giant planet: 0.11 +/- error of eccentricity: 0.05 newly discovered planet: Probable range of semi-major axis for the new planet: semi-major axis of planet [AU]: 2.3 +/- error of semi-major axis: 0.2

19. Results of the Exocatalogue (Sandor et al., 2007)

20. The EXOCATALOGUE: http://www.univie.ac.at/adg/ http://www.univie.ac.at/adg/http://www.univie.ac.at/adg/ Details: Sándor, Zs., Süli, A., Érdi, B., Pilat-Lohinger, E. and Dvorak, R.: "A Stability Catalogue of the Habitable zones Dvorak, R.: "A Stability Catalogue of the Habitable zones in Extrasolar Planetary Systems", Monthly Notices of the in Extrasolar Planetary Systems", Monthly Notices of the Royal Astronomical Society (MNRAS), 2006 Royal Astronomical Society (MNRAS), 2006

21. Habitable Zone Zone around a star where liquid water can exist on the surface of a terrestial-like planet Zone around a star where liquid water can exist on the surface of a terrestial-like planet This zone depends on: This zone depends on: the spectraltype, the mass, the age, …. of the star the spectraltype, the mass, the age, …. of the star the orbit of the planet the orbit of the planet the mass, the composition, the atmosphere, ……of the planet the mass, the composition, the atmosphere, ……of the planet the parameters of other planets in this system (mass, orbit, …) the parameters of other planets in this system (mass, orbit, …)

22. based on the definition given by Kasting et al. (1993). Size of the habitable zone of a planetary system

23. Types of Habitable Zones: (1) Hot-Jupiter type (2) Solar system type (3)+(4) giant planet type: habitable moon or trojan planet

24. Stability maps Inner region (Solar system type) Outer region (Hot-Jupiter-type)

25. Computations distance star-planet: 1 AU variation of - a_tp:[0.1,0.9] [1.1,4] AU - e_gp: 0 – 0.5 - M_gp: 0 and 180 deg - M_tp: [0, 315] deg Dynamical model: restricted 3 body problem Methods: (i)Chaos Indicator: - FLI (Fast Lyapunov) - RLI (Relative Lyapunov) (ii) Long-term computations - e-max

26. ANIMATION

27. How to use the catalogue HD114729: m_p=0.82 [Mjup] (0.93 [Msun]) a_p= 2.08 AU e_p=0.31 m=0.001 HZ: 0.7 – 1.3 AU

28.  = 0.005 HD10697: m_p= 6.12 [Mjup] (1.15 Msun) a_p = 2.13 AU e_p = 0.11 HZ: 0.85 – 1.65 AU