Introduction to extra solar planets

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1 Introduction to extra solar planets D.N.C. Lin Kavli Institute for Astronomy & Astrophysics Peking University, Beijing, China Planetary Astrophysics Kavli Institute for Astronomy & Astrophysics Peking University, Beijing December 12th, slides

2 Fundamental Questions Are we alone? If not, where is ET? If so, why is our solar system so unique? How did Earth & other planets emerge? What fates await for planetary systems? How did life form, evolve, and proliferate? 2/32

3 3/32

4 Epoch of observational discovery Solar system relics (archeology) Protostellar disks (pediatrics) Extra solar planets (anthropology) 4/32

5 A landmark discovery: Hot Jupiters Stars have Jupiters with diverse properties. 5/32

6 Frontiers of exploration Udry Exoplanets.org 6/32 Eccentric planets

7 Precision Cosmogony Udry SuperEarth everywhere 7/32

8 Probing planets & their host stars through transits Nutzman 8/32

9 Microlensing, A/O imaging, astrometry 9/32

10 Near-future prospects 10/32

11 Mechanical Universe vs Meta-stable world Planetary Ubiquity & Diversity: Origin & Evolution Great circle => coplanar orbits => Nebula hypothesis 11/32

12 Paradigm shift: building blocks are mobile 12/32

13 Relocation of protoplanetary embryos Shepherding & embedded moons Density waves & torque imbalance Extrapolation to solar nebula: Rapid migration of Earth mass cores Goldreich, Tremaine, Ward 13/32

14 Gas giants environmental impacts & migration 10/22 Last of Mohegans 14/32

15 Proliferation of gas giant planets Induced formation & proliferation Emergence of metastable systems Limited extent of relaxation Ceaseless dynamical instability 15/32

16 Population synthesis model With planet formation & disk evolution, a ini =(integration on 10 9 y) M p, a final core accretion > 5-10M gas envelope contraction >100M protoplanetary disk: H/He gas (99wt%) + dust grains (1wt%) planetesimals coagulation of planetesimals type I migration terrestrial planets cores runaway gas accretion gas accretion onto cores gas giants type II migration 16/32 Newton Press

17 Why do greater fraction of metal-rich stars have gas giants 16a/32 Homogenous DF e <5%G dwarfs in Pleiaides stars (100 Myr old).

18 Model calibration Gas giants hatchery Many but not all gas giants migrate Destiny bank Comparisons with data 17/32

19 Observable predictions: test 1. Planetary desert 2. rare brown dwarfs & many super-earths 3. Cradle of gas giants: bimodal periods 4.Domains of gas giants: period boundary 5. Epoch of planet formation (1-10 Myr) 6. Dependence on stellar mass: K giants & M dwarfs and metallicity 18/32

20 Planets on the go during gas & planetesimal clearing 19/32

21 Rich population of super earths Super-Earths as born-again embryos or remnant icy cores of failed attempts to form giants 20/32

22 Population synthesis of planetary systems gaseous rocky icy 21/32

23 Ubiquity of Earths Gaudi Hot Neptunes around M dwarfs (Ida) 15/16 22/32

24 LIFE Life started ASAP on Earth Information to regulate self assembly & self reproduction 23/32 37/46

25 Elements of biological evolution Metastable molecular bases: adiabatic versus impulsive mutation Dissemination: diffusion cross section Proliferation: exponential growth 24/43

26 Extinction and survival: natural selection Environmental impacts (feedback, self destruction) Natural catastrophes (evolving boundary conditions) 25/32

27 Anthropic Principle Astrophysical and cosmological theorists run the risk of error in the interpretation of astronomical and cosmological information unless due account is taken of the biological restraints under which the information was acquired. Biological theorists also run the risk of error in the interpretation of the evolutionary records unless they take due heed of the astrophysical restraints under which evolution took place. Brandon Carter 1983 Copernican Principle The Earth is not in a central, specially favored position. 26/32

28 Planetary mobility & diffusion of microbial lifes Diverse environments to initiate life Mobility for life to proliferate (panspermia) Evolving boundary conditions for life to adapt Range of time scales for metastability to evolve & to diversify 27/32 ``Multi-verse habitats to foster unlnown lives

29 Transmission of intelligent life Human genome contains about a meter of DNA with 4 bases nm apart => 6 x 10 9 bits Transmission bit rate = bandwidth x ln 2 (1 + P/N) Telephone line khz, TV station MHz bandwidth We can transmit human genome map to habitable planets with current facilities in 2 weeks (Goldreich) 28/32

30 Fermi s paradox: where is ET? SETI What signs should we look for? 29/32

31 Sidney Harris 30/32

32 Are we alone? 31/32

33 Summary & Discussions 1) Habitable planets are common. 2) Planets form with mobility. 3) Planetary structure and planetary-system architecture are diverse (statistical mechanics). 4) Planetary distribution is patchy. 5) Planetary systems ongoing evolution drives life dissemination 6) Life is likely to be diverse in this universe 32/32

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