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Transient Exoplanet and Differential Photometry

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Transient Exoplanet and Differential Photometry Exoplanets Transient Exoplanet and Differential Photometry Edge on Face on Lab 5: Detecting Exoplanet Transit Lab 5: Detecting Exoplanet Transit • Due: March 6 (Monday) 4:09pm (before the class) • Target: GJ 1214 b • Data: from ACAM on the William Herschel Telescope • Lectures on Exoplanets and Differential Photometry • Group Presentations: Feb 13 and 27 • Feb 13 class: starts at 5:10pm (lab from 4:10pm) • Feb 13 group discussion: - 4 minutes for presentation; 1 minute for Q/A - should include 3 slides for summarizing the the detailed steps of Lab 5 - should include your results by the key step #2 • Class dinner sometime in March after class Exoplanets Extra-solar Planets (Exoplanets) How Do We Detect? Exoplanet discoveries per year 2,000 confirmed exoplanets discovered so far! Exoplanets So how do we detect them? ● Direct Imaging ● Stellar Motions − velocities, timing, astrometry ● Light curve − transient planets Direct Imaging • Currently heating up with adaptive optics, high contrast imaging systems • Earth-like planet around a sun-like star is 10 billion times fainter than its star • Need to find a faint object very close to a bright star Beta Pictoris HR 8799 Direct Imaging • Only about ~ 20 planets directly imaged • Technically challenging Stellar Motions • Radial velocity, timing, astrometry Stellar Motions Radial Velocity Comparisons 1995 • Best measurements now measure variations of 0.5 m/s (a slow walk) Stellar Motions Radial Velocity Comparisons • 51 Pegasi b – First planet around sun-like star • P = 4.23 days! -> Hot Jupiter Exoplanets How do we detect exoplanets? Light Curve Method: Transient Planets A transient planet changes blocks the light from a star = eclipse! ● Eclipse depth in terms of planet and star radii (for circular orbit)? ● Transit probability in terms of star radius and distance between the planet and star (for circular orbit)? Light Curve – Transiting Planets HD 209458 Transit Transit Secondary Eclipse Orbital Period Can reach 10 parts-per-million accuracy for the brightest stars from space Exoplanets How do we detect exoplanets? Light Curve Method: Transient Planets A transient planet changes blocks the light from a star = eclipse! “Challenges and Advantages of Detecting Transient Planets?” Exoplanets How do we detect exoplanets? Light Curve Method: Transient Planets Large Transit Planet Survey: OGLE, Kepler, Corot, … Exoplanets How do we detect exoplanets? Transient Planets The Kepler Project The Kepler Mission: Field FOV The Kepler Mission The Kepler Mission The Kepler Mission Exoplanets How do we detect exoplanets? Transient Planets Example: HD209458b (1999) Small telescope discovery Hubble Space Telescope data Density measurement Density measurement: Example Kepler-78 Star KIC 8435766 (Kepler-78) Constellation Cygnus h m s Right ascension (α) 19 34 58 Declination (δ) +44°26′ 54″ Apparent magnitude (mV) 12 Radius (r) 0.73±0.15 R☉ Temperature (T) 5143 (±70) K Metallicity [Fe/H] -0.08 (±0.13) A planet was discovered in 2013 by analyzing data from Kepler space telescope. The planet was found not only transiting the star, but its occultation and reflected light from the parent star due to orbital phases were also detected. Density measurement: Example Kepler-78b (formerly known as KIC 8435766 b) is an exoplanet orbiting around the star Kepler-78. Mass (m) 1.69-1.85 M⊕ Radius (r) 1.12 R⊕ Bond Albedo (%) 20-60 % -3 Density (ρ) 5.3-5.6 g cm So how de we measure the density of exoplanets? Let’s look into more! What do we know from transit light curves? • Transit Depth • Transit Duration • Transit Period • Ingress and Egress Times Sky-projected distance between the center of the star and planet. The total transit duration is heavily dependent on the impact parameter. Ingress Egress Transit Depth Limb Darkening Primary and Secondary Eclipses .
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