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This 2 page Class Notes was uploaded by Lindsey Kangas on Thursday October 13, 2016. The Class Notes belongs to 10273 at Texas Christian University taught by Dr. Ingram in Fall 2016. Since its upload, it has received 4 views. For similar materials see Intro Astronomy: Earth&Planets in PHYSICS (PHY) at Texas Christian University.
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Date Created: 10/13/16
Notes 10/12 Extrasolar Planets (detection) Indirect methods: o Doppler wobble technique— Two rules of Doppler shifting: 1. (a) Objects moving toward you appear “blueshifted” (shorter waves) (b) Objects moving away appear “redshifted” (longer waves) 2. The amount of shift is proportional to radial velocity o Radial meaning along line of sight; parallel to radius What do we deduce? 1. Amplitude of wobble (V orbitor star/planet) if system is edge-on 2. How long it takes to repeat itself (period) Perio d What we Tim measur e Vradial The closer you are orbiting to the sun, the faster you go Period equation: 2Πr orbit(V orbit (T) Determines how far away a star is and how massive Almost all exoplanets found using Doppler wobble technique are very massive (Jupiter or larger) and VERY close to parent star (possible 5 day orbit) Opposite of our planetary hypothesis Called hot Jupiters Do we throw out our theory? o NO o Our sample is biased/not representative o Biased in favor of finding only massive planets Low mass planets do not make wobble strong enough to detect In favor of stars very close to parent star because that have short orbital periods; we have only been looking for a short time SO we cannot see planets farther out (must follow for 20-30 years)
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