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A Turtorial Lecture on Exoplanets

A Turtorial Lecture on Exoplanets. Wing-Huen Ip Institutes of Astronomy and Space Science National Central University August 31, 2012. Introduction. Planets before 1995…. small rocky planets close to the Sun gas-giant planets more distant from the star. You are here!.

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A Turtorial Lecture on Exoplanets

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  1. A Turtorial Lecture on Exoplanets Wing-Huen Ip Institutes of Astronomy and Space Science National Central University August 31, 2012

  2. Introduction

  3. Planets before 1995… small rocky planets close to the Sungas-giant planets more distant from the star You are here!

  4. Discovery of the first exoplanet: Peg 51b in 1995 http://spiff.rit.edu/classes/phys230/lectures/planets/planets.html

  5. Periodic Variation of the Spectral Lines http://www.cfa.harvard.edu/afoe/51Peg.html

  6. http://lcogt.net/spacebook/radial-velocity-method

  7. Doppler Effect http://mail.colonial.net/~hkaiter/Doppler_Effect_Shift.html

  8. Red Shift Effect and Hubble Constant http://www.answersingenesis.org/articles/tba/universe-confirms-bible http://astronomy21st.blogspot.tw/2010/03/universe-expansion-is-speeding-up.html

  9. Hot Jupiters Hot-Jupiters are Gas-Giant planets, orbiting VERY close to their parent star. They are probably tidally locked, i.e. one face is always illuminated and the other is in perpetual darkness. They easily reach Temperatures 1000-2000 K

  10. Mass vs semi-major axis http://jila.colorado.edu/~pja/planets/extrasolar.html

  11. A new class of planets: Super-Earths! Neptune/GJ436 GJ1214 Earth Kepler 10b 55 Cnc e CoRoT-7b

  12. Radial velocity & astrometry Mp sin I Effect Sin i : large Mayor & Queloz, 1995 Sin i : small

  13. Exoplanet Transit http://www.astro.caltech.edu/people/faculty/wasp10_transit_600.jpg

  14. What are these planets actually like? • (atmospheric composition? thermal properties?) • Why are they as they are?

  15. Habitable Zone https://www.e-education.psu.edu/astro801/content/l12_p4.html

  16. There is more to mass and radius…

  17. The Hot Jupiters

  18. Orbital distribution

  19. Thermal evaporation of the atmosphere of hot Jupiters http://star.herts.ac.uk/RoPACS/JoGo.html

  20. WASP-12b

  21. Space Weather

  22. The Hot Jupiters • Tidal interaction and/or electromagnetic effects (Cuntz and Shkolnik, 2002)? • Superflares from star-planet interaction )Rubenstein and Schaefer (2000)?

  23. Star-planet Magnetic Interaction Three Types of Magnetic Coupling Power = VB2L2 ergs/s ~ 1027 ergs/s Ip, Kopp and Hu (2004)

  24. Magnetospheric Substorms

  25. Observational Test • Detection of excessive Ca II H and K line emission-synchronized to orbital period of the Hot Jupiter ( Skholnik et al. 2005) • On/off nature of such hot spots (Skholnik et al., 2008)

  26. Kepler Observations • Maehara et al. (2012): Superflares on solar-type stars • 9751 sola-type stars in Kepler field • 365 superflares (>1035 ergs) in 148 stars

  27. Kepler Observations • Maehara et al. (2012): Superflares on solar-type stars • 9751 sola-type stars in Kepler field • 365 superflares (>1035 ergs) in 148 stars • None of them has Hot Jupiter!

  28. Sun spots and star spots http://go.owu.edu/~physics/StudentResearch/2003/BethCademartori/index.html

  29. Kepler Observations • Maehara et al. (2012): Superflares on solar-type stars • 9751 sola-type stars in Kepler field • 365 superflares (>1035 ergs) in 148 stars • One million times stronger than the biggest solar flares ever obeserved. • Frequency is about once every 5000 years • None of them has Hot Jupiter! Could Superflares happen on the Sun?

  30. Space weather

  31. http://www.eee.metu.edu.tr/~etulunay/ytulunay/

  32. Electricity black out on March 13, 1989

  33. Electricity blackout of August 14, 2003,in New York

  34. Electricity blackout in July, 2012

  35. Search for Earth-like Habitable Exoplanets by the Kepler Mission:New Results from IAU GA, Beijing (20-31, 8, 2012)

  36. The Kepler Mission • The scientific objective of Kepler is to explore the structure and diversity of planetary systems.[45] This spacecraft observes a large sample of stars to achieve several key goals: • To determine how many Earth-size and larger planets there are in or near the habitable zone (often called "Goldilocks planets")[46] of a wide variety of spectral types of stars. • To determine the range of size and shape of the orbits of these planets. • To estimate how many planets there are in multiple-star systems. • To determine the range of orbit size, brightness, size, mass and density of short-period giant planets. • To identify additional members of each discovered planetary system using other techniques. • Determine the properties of those stars that harbor planetary systems.

  37. Kepler FOV 115 sq. deg.

  38. Planetary candidates observed by Kepler III. Analysis of the first 16 months of data • Batalha, N. et al. • arXiv:1202.5852, 2012

  39. Kepler-20: A sun-like star with three-sub-Naptune exoplanets and two Earth-size candidates • Gautier, T.N., et al. • ApJ, 749, 15, 1, 2012

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