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PTYS 214 – Spring 2011
Homework #10 DUE in class TODAY
Review Guide will be uploaded to class website soon
Class website: http://www.lpl.arizona.edu/undergrad/classes/spring2011/Pierazzo_214/
Useful Reading: class website “Reading Material” http://en.wikipedia.org/wiki/Extrasolar_planet http://exoplanet.eu/catalog.php
http://www.solstation.com/stars/gl581.htm
Announcements
Planetary Sciences Graduate Teaching Assistant Excellence Award
Planetary Science Department initiative to promote, recognize and reward exemplary performance among graduate teaching
assistants assigned to PTYS undergraduate courses
If you think your PTYS-214 Teaching Assistant qualifies for the award, please fill out a nomination form describing:1) Why you are nominating the TA2) How the TA has contributed to your learning experience
After April 25th, nomination forms and the drop box will be located on the table outside your classroom, room 308
The Teaching Assistants for PTYS214-2 are:
Lissa Ong & Devin Schrader
Extrasolar Planets
Also called exoplanets, they are planets that orbit other
stars beyond our Sun
The existence of other solar systems has been suspected for centuries, but verified only
in the 1990s
In 1995, a breakthrough:the first planet around another star
A Swiss team discovers a planet around 51 Pegasi – 50 light years from Earth
Artist's concept of an extrasolar planet (Greg Bacon, STScI) 7
Didier Queloz &Michel Mayor
And then the discoveries started rolling in:
“First new solar system discovered” USA TODAY - April 16, 1999
“10 More Planets Discovered” Washington Post - August 6, 2000
“New Planet Seen Outside Solar System”New York Times - April 19, 1996
…if you know where to look
Planet of 70 Virginis
=7.42 Jupiter masses
Planet of Tau Bootes
=4.41 Jupiter masses
Just how far are these new planets?
from Mars…it would take3-22 minutes
from the nearest extrasolar planet…
it would takeover ten years!
from the Moon… it would take<2 seconds
IF YOU WANTED TO RADIO HOME
FOR YOUR WORDS TO REACH EARTH
Detecting Extra-Solar Planets
Problem #1: Planets are not bright objects!
Problem #2: Planets are relatively small and close to a bright star(DSun ~ 10 DJupiter ~ 100 DEarth)
Successful detection techniques: Stellar Radial Velocity, or Doppler Method Planetary Transit
Direct Imaging
Gravitational microlensing
Most extrasolar planets orbit very close to their star—“hot Jupiters”
As of today (4-21-11)~544 mostly Jupiter-sized planets (~300 Earth masses) have been discovered(http://exoplanet.eu/catalog.php)
Radial Velocity TechniqueMost exoplanets (~499) are detected
by radial velocity technique
Uses the Doppler Effect to measure changes in the radial velocity of a star caused by the small gravitational force of an unseen orbiting planet
….but it can only measure motion along the line of sight (edge on)
Allows to determine the planet’s mass plus shape and size of orbit
Radial Velocity Technique
Observe red-shifting and blue-shifting of the star’s spectral lines caused by Doppler effect
Amount of blue or red shift corresponds to the star’s radial velocity towards or away from us
Planetary Transit Technique
Measures dimming of star light as planet passes in front
of star
Star-light may dim by only 0.000001 (10-6)
About 127 planets have been detected by the
transit technique
Planetary Transit Technique
Disadvantages: a) Bias towards large planets and in short period orbits b) False detections due to stellar variability c) Planet’s orbit must be seen edge-on from the observer point of view (so the planet passes in front of the star)
Advantages: a) Relatively cheap b) Can determine the size of the planet
Direct Imaging Direct detection of planets is extremely difficult
Rare cases when direct imaging can work are:− Planet is very large (considerably larger than Jupiter)− Planet is widely separated from its parent star − Planet is young (so that it is hot and emits intense infrared
radiation)
Few exoplanets are imaged directly ~21 candidates
Image of a planet around GQ Lupi (early K-type star)
The planet is believed to be about twice the mass of Jupiter and to have an orbital radius of about 30 AU (similar to Neptune)
2005; European Southern Observ.
Gravitational Microlensing Use the gravitational effect of large objects that can bend light around them
If the object is a star with a planet, the planet can be detected by its effect on the microlensing
About 12 potential exoplanets detected by this technique
Several extrasolar planets are Super-Earths, 1-10 times more massive than Earth
The smallest extrasolar planet discovered so far (in 2009) is Gliese 581e, estimated to be about 2 Earth masses
About 20 percent of extrasolar planets are within the Habitable Zone of their parent stars
Extrasolar Planets: discovered so far
Most Earth-like: Gliese 581d
Gliese 581 is a red dwarf star (about 1/3 the Sun’s mass),
located 20.3 light years from Earth
Planet Mass Distance(AU)
Orbit (days) Eccentr.
e 2ME
0.03 3.15 0
b 16ME
0.04 5.37 0
c 5ME
0.07 12.9 0.17
d 7ME
0.22 66.8 0.38
Venus-like?
Potential for life?
Gliese 581d animation
• http://www.youtube.com/watch?v=wJXSSYyIVqw
• http://www.youtube.com/watch?v=_kcquVBYbGw&feature=related
Prospects for finding habitable planets
Best candidates are F, G, and early K-type stars, i.e., stars not too different from the Sun
Early-type stars (blue stars)– High UV fluxes– Short life (not enough time for life to evolve)
Late-type stars (red dwarfs) – M-class, M dwarfs– Targets for many habitable, earth-sized planet
searches– Examples: GJ 436b, Gl 581c, OGLE-2005-BLG-
390L
Much less massive than Sun-like stars (G-type stars)Deeper transits, better RV detectionVery low luminosity Smaller HZs
Consider an M5 dwarf which has a luminosity L = 0.0055 x L(solar) [Recall L(Solar) = 3.84 x 1026 W]. At what distance (D) from the M5 dwarf would a planet receive the same total radiation flux of the Earth? [Recall S0 = 1370 W/m2]
Habitable Planets around M dwarf stars
So why looking at M dwarf stars?
More numerous than Sun-like stars– Constitute 20 of the 30 stars nearest to
Earth
Much longer life spans than Sun-like stars – Some can live for trillions of years!
Problems with M-dwarfsLimited Habitable Zone (too cold?)Tidal locking (only one face of planet facing star, becomes synchronously rotating)Stellar variability: lots of flares
HOWEVER: • A study by Joshi et al. 1997 has shown that atmospheric circulation should help reduce day-night temperature variations.• Heath et al. 1999 concluded that even during a flare, radiation received by a planet in the HZ of an M dwarf is comparable to that received by the Earth.
These planets could still be habitable!