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Extra-Solar Planets

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Extra-Solar Planets Extra-Solar Planets The Ongoing Discovery Era Keith Horne SUPA, St.Andrews Extra-Solar Planets The Discovery Era • < 1995 Solar System planets • 1995 first extrasolar planet • ( 51 Peg ) a Hot Jupiter! • 2005 ~150 Hot-Cool Jupiters • 2010-15 Habitable Earths -- common or rare? • 2015-25 Are we alone? Extra-solar Life? Direct Imaging HARD! Extreme Adaptive Optics Coronography Nulling Interferometry GQ Lup Faint companions to: White Dwarfs Brown Dwarfs with common proper motion GQ Lup: 22 mJ 100 AU Neuhaeuser et al. 2005 2M1207: 5 mJ 55 AU Chauvin et al. 2005 AB Pic : 14 mJ 280 AU Chauvin et al. 2005 Indirect Discovery Methods • Doppler Star Wobbles: • Transits: • Microlensing: Exoplanet Discovery Space Jupiter Earth Key Technology: 1995 First Doppler Wobble Planet: 51 Peg Discovered by accident: Mayor & Queloz (1995) Quickly confirmed: Marcy & Butler (1995) P = 4.2 days (!) a = 0.05 AU T ~2000K m sin(i) = 0.5 mJ New class of planet: “Hot Jupiter” Doppler Wobble Planets 2005 Sep (first decade) 134 stars 158 planets 18 multi-planet . systems ~5% of stars “wobble” 1-2 planets / month Wide range of planet masses and orbit sizes < m 10mJ P >2d Jupiter Earth Eccentric Orbits Unclear why. Planet-planet interactions Small planets ejected Tidal circularisation High metalicity of planet host stars more more metals --> planets Enhanced planet formation ? Pollution of stellar atmosphere? Santos 2003 Fischer & Valenti 2004 GJ 876 M4V star + 2 gas giants in resonant orbits : m sin(i) = 0.56 m J P = 30 d m sin(i) = 1.89 mj P = 60 d Marcy et al. 2001 + smallest hot planet ( terrestrial ? ) m sini ~ 8 m e P = 1.9 d Rivera et al. 2005 Lessons from Doppler Wobbles • > 5% of Sun-like stars host a Jupiter • Metalicity matters • Orbits differ from Solar System – wide range of orbit radii ( P > 2d ) – wide range of eccentricities • New processes – Migration -- inspiral – eccentricity pumping – ejection • What about the other 95% ? – Is the Solar System typical or rare ? Planets form in dusty disks Computer simulations of planet formation Orbital migration • Spiral waves induced by planet – Exchange angular momentum with disk ) Gravitational Instability • Type 1 -- no gap. Fast. * M – m < Saturn / Type III k s i Type II -- gap. Slow. d • M ( Type I Type II – m > Saturn g o no gap gap • Type III -- runaway L – m ~ Saturn Log( m p / M * ) • Planets migrate into the star! – Need to suppress Type I migration. e.g. Masset & Papaloizou, 2003 Ida & Lin Model Distribution Observed Distribution Most of these planets accrete onto star Masses) Mass (Earth Mass Presently Unobservable Semi-Major Axis (AU) Semi-Major Axis (AU) Ida and Lin (2004, 2005) carried out a large number of Monte-Carlo simulations which draw from distributions of disk masses and seed-planetesimals to model the process of core accretion in the presence of migration. These simulations reproduce the planet “desert”, and predict a huge population of terrestrial and ice giant planets somewhat below the current detection threshold for radial velocity surveys. Transits: Hot Jupiters Jupiter Earth Transit Lightcurves ≈ rJup 0.1 RSun Depth: 2 −2 ∆f rp R∗ ≈1% f rJup RSun Duration: 2/3 M P 1/ 3 ∆t ≈ 3h ∗ MSun 4d Probability: −1/3 − R M P 2/3 P ≈10% ∗ ∗ t RSun MSun 4d 1999 First Transiting Planet HD 209458 V=7.6 mag 1.6% “winks” last 3 hours repeat every 3.5 days ) Charbonneau & Brown (2000) STARE 10 cm telescope STARE data HD 209458 “Bloated” Gas Giant m ~ 0.63 mJ r ~ 1.3 rJ i ~ 87 o HST/STIS HD 209458 Transits Brown et al. (2001) r = 1.35 ± 0.06 rJ i = 86 o.6 ± 0 o.2 1% HST: Fit Residuals ~10 -4 No Moons r > 1.2 rEarth No Rings r > 1.8 rEarth winds clouddecks composition planetary atmosphere Spectroscopy Brown (2001) Transit Transit transit depth 1.5% 1.6% Na Na I wavelength (microns) HST Transit Spectroscopy detects Na I in the atmosphere of HD 209458b 3.2 ×10 −4 × −4 Charbonneau et al. (2002) 3.1 10 Evaporating Atmosphere Vidal-Madjar et al. (2003) 5% 10% 10% Star occults planet 0.2 % Spitzer/IRAC 4.5, 8.0 micron Direct detection of TrES-1: Charbonneau et al. 2005 infrared light from planet HD 209458: Deming et al. 2005 2005 Ground-based Transit Surveys WASP Wide Deep OGLE 19 mag = 1.3m OGLE 3 kpc 300pc 13 mag = 11cm WASP Wide Deep Wide Deep 10cm 1-4m 10o < 1o OGLE III Transit Candidates 1. 3m Las Campanas (microlens survey telescope) Mosaic 8-chip CCD camera 2001 Galactic Bulge -- 64 candidates 2002 Carina -- 73 candidates 2004 Nov Deep surveys of Galactic Plane fields yield many false alarms : grazing or blended eclipsing binaries, brown dwarf eclipses 6 planets discovered by transits and confirmed by radial velocities 3 with P < 3d (?) Period Distribution New class of very-hot Jupiters? Different selection effects ? Radius vs Mass At least 2 parameters Rapid inward migration ---> no time to cool Wide Transit Survey Discovery Potential Assume HD 209458 (V=7.6 mag) is brightest. mag 8 9 10 11 12 13 all sky 1 4 16 64 256 1024 16 ox16 o - - 0.1 0.4 1.6 7 How long to find them all ? ~ 150 16 ox16 o fields ~ 2 months / field ~ 25/ N years N = number of 16 ox16 o cameras UK WASP Experiment Wide-Angle Search for Planets 2004 SuperWASP La Palma 2005 SuperWASP SAAO Robotic Mount 8 cameras / mount 11cm F/1.8 lens 2K x 2K E2V CCD 8o x 8 o field 15 arcsec pixels UK WASP Consortium: Belfast, St.Andrews, Keele, Open, Leicester, Cambridge, IAC, SAAO. D.Pollacco = PI SuperWASP La Palma 2004 Data Under Analysis Spectroscopic follow-up of candidates is underway SuperWASP 2004 Transit Candidate -- 1% -- How to find Earths ? • Hot Earths : Transits from Space – 2006-08 … Corot – 2008-12 … Kepler • Habitable Earths: Hard to Find – Habitable Zone: T~300K liquid water on rocky planet surfaces • Cool Earths : Gravitational Lensing – 2004-12 … OGLE, PLANET, RoboNet, microFUN, MOA “Habitable” Earths: common or rare? ~100 Doppler wobble planets Jupiter Earth Hot Planets Cool Planets Hot Earths Transits from Space Earth transit depth: ∆f ~ 10−4 = 0.01% f HST results suggest this is detectable. Space Transit Missions Designed to detect Earth analogs r ~ r⊕ ~ 0.01 Rsun T ≈ 300K P ~ 1 yr a ~ 1 au ∆t ~ 13 h ∆f / f ~ 10−4 Transit probability: Pt ~ 5.0 % “The Habitable Zone” T~300K ⊕ Eddington Planet Catch Simulation habitable hot Jupiters Earths Gravitational Microlensing Hunting for Cool Planets near the Lens Star Gravitational Lensing Observer’s View: 2 distorted images Lensing by a Star with a Planet Lens star … no planet Lens star with a planet ~600 Galactic Bulge lensing events found each year −3 M lens~ 3.0 M sun RE ~ 4 AU ~ 10 arcsec (Animations by Scott Gaudi) Planet Hunting Method planet d1 m / mJ t p ~ t E ~ 30d M / 0.3 M sun h1 m / mE Three-Stage Approach • Stage 1: discover microlens events -6 – prob ~10 , tE ~ 10 - 100 d – OGLE (+ MOA) find ~ 600 / yr • Stage 2: discover planet-like anomalies – Jupiters: prob ~ 15% tp ~ 1 d Earths: prob ~ 1.5% t ~ 1 h – p t ∝ m • Stage 3: characterise planets – continuous monitoring • Teams: OGLE, MOA , PLANET, microFUN – 2005… UK 2m Robotic telescope network RoboNet • COOL EARTHS DETECTABLE OGLE III Galactic Bulge Microlens Search Fields 1.3 m Las Campanas ~ 150 million stars ~ 4 day sampling ~ 600 microlens events . each year Early Warning System internet alerts Planet Detection Zones OGLE III data (~600 events / yr) Planet exclusion zones --------10%--- residuals (no anomalies) Planet detection probability Planet-like Anomalies Several found each year Brief (<4d) 60% brightening Must intensify monitoring to discover more, and to characterise the planet masses. Microlens Follow-up Networks: PLANET, MOA, microFUN, RoboNet PLANET 4 southern sites 0.6-1.5 m telescopes selected events ~24-hour coverage Cool Planet Hunting with the UK’s 2m Robotic Telescopes Liverpool Telescope: La Palma Faulkes Telescopes: FT-N, Maui FT-S, Siding Springs RoboNet 1 --> REX REX = Robotic EX oplanet discovery Network REX proposal for 2 more southern telescopes. Dedicated to exoplanet hunting Doppler wobbles, transits, microlensing. OB -03 -235/MB -03 -053 first microlens planet m ~ 1.5 mJ OGLE alert Bond et al. (2004) OB-05-071 m ~ 3 mJ Udalski et al. (2005) OB-05-390 m ~ 5 m⊕ Beaulieu et al. (2005) Lowest-mass exoplanet to date Ida & Lin Model Distribution Observed Distribution Most of these planets accretemicrolensing onto star Masses) Mass (EarthMass Presently Unobservable Semi-Major Axis (AU) Semi-Major Axis (AU) Ida and Lin (2004, 2005) carried out a large number of Monte-Carlo simulations which draw from distributions of disk masses and seed-planetesimals to model the process of core accretion in the presence of migration. These simulations reproduce the planet “desert”, and predict a huge population of terrestrial and ice giant planets somewhat below the current detection threshold for radial velocity surveys. Are “Habitable” Planets common or rare ? Jupiter Earth ESA: Darwin ~ 2015-20? infrared space interferometer destructive interference cancels out the starlight snapshot ~500 nearby systems study ~ 50 in detail NASA’s Terrestrial Planet Finder 2014 : TPF-C 4-6 m visible light coronagraph 2020 : TPF-I 3-4 m infrared interferometer Life’s Signature: disequilibrium atmosphere (e.g. oxygen-rich) simulated Darwin spectrum Which planet is alive? The Road Ahead • Doppler Wobbles –2005 ... 150 --> 200 Jupiters –longer periods, multi-planet systems • Transits –2005-10 … WASP ~10 3 Hot Jupiters –2006-08 … Corot Hot Earths –2008-12 … Kepler Hot --> Habitable Earths • Microlensing –2005-15 … cool Jupiters --> Earths • Darwin / TPF –2015-2025 … direct images, spectra, Life? Thanks for listening! Thanks for Listening! And thanks to G.Laughlin, G.Lodato, R.Nelson for slides used in this talk.
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