Chapter 12. Extrasolar Systems Extrasolar planet discovery: - Pulsar planets
Extrasolar planets Emre Işık (MPS, Lindau) S 3 lecture Origin of solar systems 14 February 2006.
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Transcript of Extrasolar planets Emre Işık (MPS, Lindau) S 3 lecture Origin of solar systems 14 February 2006.
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Extrasolar planets
Emre Işık (MPS, Lindau)
S3 lecture
Origin of solar systems
14 February 2006
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Outline
• Planet detection methods– Methodology– Some recent results
• Statistical properties of exoplanets• Future prospects
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Struve, O. 1952 Obs., 870, 199
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Detection techniques IPrecise stellar radial velocities to observer
N. S
trob
el
N. S
trob
el
to observer
N. S
trob
el
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Detection techniques IITransit photometry
a = (PorbR) / t
f / f = (Rp / R)2
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Detection techniques IITransit photometry
Advantages
• Easy (if automated!), small telescopes with good sites/detectors
• Possibility to detect low-mass planets, especially from space (Kepler mission, 2008)
Disadvantages
• Transit probability low; simultaneous observations of many stars
• Confusion with starspots, multiple stars
Planets around binary stars
Deeg (1998)
Reflection effect
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HST light curve of HD 209458 b
Brown et al. (2001) • Stellar radius and limb-darkening profile • Planet's mass and radius • No rings around the planet • No moons with M > 3 ME (repeated obs.)
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Detection techniques IIIMicrolensing
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Detection techniques IIIMicrolensing eventsOGLE 2003-BLG-235/MOA 2003-BLG-53
Discovered planet: 1.5 MJ @ 3 AU
Bond et al. 2004, Astroph. J. Letters , 606 , L155
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Detection techniques IIIMicrolensing events
Discovery of a Cool Planet of 5.5 Earth Masses. OGLE-2005-BLG-390
Beaulieu et al., 2006, Nature, 439, 437
Discovered planet: 5.5 ME @ 2.6 AU
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Detection techniques IVAstrometry
“Celestial” motion of the Sun due mainly to Jupiter & Saturn, as seen from 33 light years
away…
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Astrometry
A Jupiter analog orbiting 5 AU from a solar-type star produces an astrometric amplitude of 0.5 milliarcsec (mas).
A star with planet close to (about 1 arcmin) to a star without planet is needed.
Direct, short CCD exposure at Palomar 5m and Keck telescopes may yield 0.1 mas.
Palomar test-bed interferometer yields 60-70 μas, VLTI should allow 20 μas.
Space missions may do better as interference from terrestrial atmosphere is eliminated.
As of 1998, no object has been found.
Technique is in its infancy. Big telescope resources are needed.
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Detection techniques VDirect imaging !
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Detection techniques VDirect imaging !
Visible light
Infrared light
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• Name: 2M1207 b
• Msini: 5 ± 1 MJ
• Radius:1.5 RJ
• Temperature1240 ± 60 K
• Semi-major axis: (projected dist.) ~ 55 AU
• Orbital period: > 2450 yr
• Mass (star/M_sun): 0.025 NACO/VLT image, Chauvin et al. 2005
Detection techniques VDirect imaging !
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Substellar companion to GQ Lupi
• IR image (NACO/VLT) GQ Lupi (A) orbited by a planet (b) at a distance of ~20xJupiter-Sun.
• GQ Lupi: 400 ly, 0.7 M
• Mass: 1-42 MJ
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Detection techniques VI [reflection/absorption]
spectroscopy
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Detection techniques VI [reflection/absorption]
spectroscopy
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Detection techniques VI [reflection/absorption]
spectroscopy
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Caution: “planet occurrence” is biased by RV sensitivity!
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Properties of the detected planets
Lineweaver & Grether 2003
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Properties of the detected planets
Lineweaver & Grether 2003
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Extrapolations
Lineweaver & Grether 2003
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Lineweaver & Grether 2003
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Evolutionary models
• Different assumptions on the inhibition of cooling by irradiation from the parent star, and the planet's internal structure (Burrows et al. [2000], Bodenheimer et al. [2001] and Guillot and Showman [2002])
Fig.: Collier Cameron (2002)
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The future:Future of future:
2015 - 2025
CO2
O3