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Solar System Formation

Solar System Formation. 1. Rotating cloud of gas & dust. 2. Cloud spins & flattens, forms a disk. solar nebula. 3. Core of disk forms young star. 4. Outer material accretes to form planetesimals. rocky planets (Terrestrial). gas planets (Jovian).

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Solar System Formation

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  1. Solar System Formation 1.Rotating cloud of gas & dust 2.Cloud spins & flattens, forms a disk solar nebula 3.Core of disk forms young star 4.Outer material accretes to form planetesimals

  2. rocky planets (Terrestrial) gas planets (Jovian) Our Solar System • Types of planets depend on: - temperature - amount of material • Rocky planets formed closer to Sun • Gas giants formed further out STANDARD MODEL

  3. Constellation Orion Hubble Stellar Nurseries • Example: Orion Nebula • birthplace of new stars, new solar systems?

  4. •Extra Solar Planet (ESP): a planet around a star other than our Sun •brown dwarf: less mass than a star, more mass than Jupiter ESP high eccentricity (more oval) low eccentricity (more circular) Vocabulary •light year:distance light travels in 1yr •eccentricity:how elliptical an orbit is 1030 kg 1027 kg 1024 kg

  5. Planet Quest

  6. dust disk outside galaxy Hubble Beta Pictoris The First Searches • 1920s - Edwin Hubble: identified neighboring galaxies • 1980s - B. Smith & R. Terrile: captured 1st image of debris disk around star

  7. Mayor & Marcy ESP & 51 Peg Discovery At Last 51 Peg • 1995: Michel Mayor & Didier Queloz (Swiss) - 1st ESP orbiting star 51 Pegasus • 1995: Geoff Marcy & Paul Butler (SF State, UC Berkeley) - confirmed discovery - found many more • 2000’s: dozens more • by 2006: 193 planets 14 multiple planet systems and many more now…

  8. Star GQ Lupi & planet GQ Lupi planet

  9. 55 Cancri Tau Bootis 70 Virginis 47 Ursae Majoris 16 Cygni B

  10. Extra Solar Planets Stars 2 1 Distance from parent star (AU) MJUP = mass of Jupiter

  11. “Hot Jupiters” Eccentric orbits Orbit close to star Characteristics of ESPs • Jupiter-sized and bigger • Orbit close to star (closer than Mercury) • Orbits highly eccentric

  12. Detection • Obstacles - Too far away - Don’t produce any of own light - Lost in glare of parent star • Solution: look for effects on parent star

  13. • Doppler Shift • Transit Method • Direct Detection Doppler Shift Transit Method Direct Detection Methods of Detection • plus others……

  14. gravity Doppler Shift & Orbit Wobble • Star and planet orbit center of mass X • Planet has small gravitational affect on star • Tug of gravity causes star to wobble X X = center of mass

  15. BIGGER wavelengths smaller wavelengths Review: Light Waves

  16. light moving away from observer light moving toward observer DOPPLER SHIFT Red ‘Shift’ vs. Blue ‘Shift’ waves appear stretched waves appear compressed RED SHIFT BLUE SHIFT observer of star

  17. Detection: Doppler Shift • Planet causes star to wobble in circular orbit moving toward observer moving away from observer • Light from star is Doppler shifted

  18. Detection: Doppler Shift

  19. Wobbles from Neptune-sized planet orbiting star Gliese 436 Real Star Wobbles Gliese 436 Star moving toward Star moving away

  20. Detection: Transit Method • planet passes between star and observer • planet blocks out tiny portion of star’s light • star’s light appears to dim

  21. Detection: Transit Method • planet passes between star and observer • planet blocks out tiny portion of star’s light • star’s light appears to dim

  22. Direct Detection • state-of-art infrared images • detect light 200+ light years away Giant planet and young brown dwarf

  23. Keck Interferometer SIM Planet Quest Terrestrial Planet Finder Future Missions • 2001: Keck Interferometer - began capturing 1st images of gas giant EPSs • 2011: Space Interferometry Mission (SIM) Planet Quest - will detect evidence for earth-sized planets • 2014: Terrestrial Planet Finder - will send back 1st pictures of nearby planetary systems

  24. What is your favorite planetary body? Give one scientific reason why.

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