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![Page 1: Www.astro.washington.edu/observatory/ Extra-Solar Planets Theodore Jacobson Observatory University of Washington Brian Stephanik October 5 th, 2005.](https://reader030.fdocuments.net/reader030/viewer/2022032523/56649d775503460f94a5887d/html5/thumbnails/1.jpg)
www.astro.washington.edu/observatory/
Extra-Solar Planets
Theodore Jacobson Observatory
University of Washington
Brian Stephanik
October 5th, 2005
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Topics for tonight
What are (extra-solar) planets?Very brief historyDetectionThe presentThe future
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Where do planets fit in?
Asteroids, planets, and stars: where to draw the line? Rocky core – gaseous atmosphere – nuclear fusion On-going debate: Pluto
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History
A very new science– Last 15 years
1989 – Mention of (possible) extra-solar planets in a research paper
1993 – Confirmed detection1995 – Main sequence detection: 51 PegasiLate 1990s – Large number of discoveries due to
advances in technology– CCDs, telescopes, etc.
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Detection
Stars outshine their planets– Direct detection is difficult
Need to be clever1. Astrometry
2. Occultation
3. Doppler
4. Microlensing
(Scary names, not so scary ideas)
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Detection #1: astrometry
“Star wobble”– Playground connection
• Teeter-Totter & Center of Mass
– Key idea: Objects orbit around the center of mass - even stars!
– Viewed from “above”
– First attempted: 1943
– Not used today: technology
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Detection #2: occultation
Who turned off the lights?– Venus transit & lunar
eclipse
What happens on Earth during a lunar eclipse?
Key idea: planets block light from stars
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Detection #2: occultation
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Detection #3: Doppler
Radial velocity– Doppler effect for sound
• What sound does a speeding ambulance make?
– Radar guns
– Viewed “edge-on”
– Key idea: moving sources appear to change their frequency
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Detection #4: microlensing
Einstein– Massive objects bend light.– Some of this (extra) bent
light arrives at Earth.– Causes objects to appear
brighter (more light rays).
– Key idea: objects with mass bend light (toward Earth, perhaps)
– What do one of these look like? And how would a planet affect it?
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Detection #4: microlensing
This is not the light form the host star.
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Detection: a summary
Astrometry– Star wobble
Occultation– Transit
Doppler effect– Think speeding sirens
Microlensing– Oddness of otherwise smooth light curve
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So what do we know?
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The present
Today: 160+ known ESPs
June 2005: Gliese 867
Most ESPs are HUGE!– Why is this?
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Why are ESPs big
Teeter-totter– BIG
• 1st grader invites friends• 5th grader must move out to balance• 5th grader (sun) farther from center of mass
– CLOSE• Time…• Closer planets move faster
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The present: first image
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What does tomorrow hold?
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The future
TPL: Terrestrial Planet Finder 2014 and 2020 launches Interferometry: directly observe light from a planet Spectroscopy on atmosphere of planet
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The future is tomorrow!
Thursday, Oct 6, 4:00pmPhysics/Astro Auditorium: A102
Jian Ge, University of Florida: An All Sky Extrasolar Planet Survey with the Sloan
Telescope Detection between 2008-2020
– Monitor 1,000,000 nearby stars
– Tens of thousands of new ESPs possible
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Thank you
Questions?