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EXOPLANETS
Experimental Lab
THE FIRST: PSR B1257+12a, b, & c
• Found in 1992 &
1994 by
Wolszczan+
• Smallest extra-
solar bodies ever
found, including 1
the size of the
moon
• Demonstrate
alternative planet-
forming
mechanisms
THE FIRST AROUND A NORMAL STAR: 51 PEGASI b
Fomalhaut b (“Dagon”) HR 8799 b, c, d, & e
CAN WE SEE EXOPLANETS DIRECTLY? A FEW (ALL GIANTS).
FOR THE REST, WE HAVE…LOTS OF OPTIONS
• Transit photometry
• Transit timing/duration
variation
• Reflection/emission
modulation
• Radial velocity (↓)
• Pulsar timing
• Gravitational
microlensing
TRANSIT PHOTOMETRY
• Record starlight intensity/photon flux
over time; watch for periodic dimming
• Compute tentative orbital parameters
& plan for >2 follow-up observations
THE DIFFERENCE A STAR MAKES
DO TRANSIT PHOTOMETRY, GET REFLECTION/EMISSION
MODULATION FOR FREE
THE KEPLER MISSION
EXOPLANET POPULATIONS“Hot Jupiters”
(51 Peg b was
prototype)Jupiter
analogs
Mini-Neptunes
/ Super-Earths
THE HABITABLE ZONE (HZ, OR GOLDILOCKS ZONE)
E.g. Kepler-186f is the
most Earth-like (1.4 ME)
planet found in the HZ
of another star to date.
The HZ also evolves with
time – not just at the end of
a star’s life but throughout.
E.g. the sun brightens ~10%
every 1 billion years
PROCEDURES
• All the instructions are given in the widget
• Fill out all 4 columns on your data sheet,
then answer the 3 “your report” questions
• FOR NEXT WEEK: Read “Features of the
Moon”