distribution and future of life in the universe Reminder No class this Wednesday Happy Thanksgiving Next Monday primarily review Next Wed YOU each do class presentation 30 of your final ID: 806018
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Slide1
Astrobiology: the origin, evolution, distribution, and future of life in the universe
Reminder:No class this Wednesday, Happy Thanksgiving!Next Monday: primarily reviewNext Wed: YOU each do class presentation (30 % of your final)Mon, Dec 9 Final exam. Would you all like to follow this with a potluck supper? (Colette and I will contribute major items!) No need to cook something!
Outline of this class:
Life, extreme life on earth
Where else in solar system could life exist? Mars, Titan&
Europa
,
Habitable zone (review), difficulty with estimating probability of life,
Drake equation for estimating likelihood
SETI: Search for Extraterrestrial Intelligence
What defines life?
the capacity to grow, metabolize (convert food to energy)respond (to stimuli), adapt reproduceWhat is necessary? Recent discoveries of life under extreme conditions on earth (extremophiles) show that neither sunlight nor oxygen are required
Slide3yellowstone
Yellowstone National Park: microbes live in boiling water (90 C). Other pools are extremely acidic, yet microbes and bacteria thrive there
Slide4Life in extreme conditions on earth
Black smoker, deep in the ocean: an example of life that has no need of sunlight:From vents deep in the ocean hydrogen sulfide provide energy for bacteria, which in turn feed clams, tube worms (up to 10 ft long)
Slide5A NASA favorite: Tardigrade (water bear) that survive at temps from absolute zero to above boiling, pressures up to 6x that of deepest ocean trenches, ionizing radiation. They can go without food or water for more than 10
years and then revive.
Bacteria up to a mile underground: water seeps in, and bacteria generates energy from chemical reactions
(Less than 1 mm long)
Slide6Are there other places in our solar system that might harbor life?
We discussed the Goldilocks idea for Venus (too hot), Mars (too cold), Earth (just right)Temperatures that allow liquid water may be very important
Slide7Could there have been life on Mars in the distant past?
1996: Martian meteorite found on earth, could it be possible fossil life from Mars? Current thinking is that this is not a fossil, but it raises interesting questions
Slide8What about other places? The moons of gas
giants
Slide9Moons of Jupiter (Ganymede, Europa) and Saturn (Titan)
NASA missions in past 20 years have revealed a great deal:Europa: covered with ice, possibly liquid beneath the iceTitan: has atmosphere, and liquid surface (but not water…)
Slide10Europa:
One of 4 Jupiter moons easily seen with small telescope- About the size of earth’s moon- Orbits Jupiter in about 4 days – so relatively close to JupiterNASA Galileo mission, launched 1989, reached Jupiter 1995, orbited
with
flybys of moons
until 2003
Found the surface of Europa is covered in ice, long fractures – suggests liquid water underneath ( heated by strong
tides
from Jupiter)
Liquid water: raises possibility of primitive life?
Next, an Aside on tides:
Slide11Aside on tides:
Earth- moon: ocean tides caused by gravity ( force = mass, inverse distance)Tides consume energy (friction): lead to tidal locking
Example of tidal locking: moon keeps one face to the earth all the time)
Slide12Surface of Europa, from the Galileo mission, showing “ice rafts”
A t
heoretical
model of possible
ocean on
Europa
.
(Rick Greenberg, UA)
Scale: This image is 20
by 50 miles
Slide13NASA Cassini mission to Saturn:Launched 1997, arrived
2004Cassini made multiple flybys of Venus, Earth and Jupiter to gain the required energy to reach SaturnIt carried a probe, named Huygens, that parachuted to the surface of the moon Titan in 2005, sending back images of the descent
Cassini is still orbiting Saturn, sending back data
Slide14Saturn’s largest moon:
TitanView of surface from Huygens probe, which parachuted to the surface
atmosphere
Surface:
Surface from about 30 km
Slide15Titan: further exploration suggest lakes of liquid methane, ethane: a “water cycle” than involves no water!
While these are interesting places, we have no evidence of any form of life on them. Let’s turn to the stars.
Slide16Is extrasolar intelligent life likely? Let’s start with a statistical estimate exercise:
how many left-handed, 8 year old boys are there is the US right now?
Slide17how many left-handed, 8 year old boys are there is the US right now?Population of the US, P:Fraction of males, FmFraction of people who are left handed Fl
Fraction of population who are 8 years old F
8
Answer = P * F
m
* F
l
* F
8
Slide18Scientific Notation: or handling big numbers
scientific notation: 1,000 = 103 = one thousand1,000,000 = 106 = one million1,000,000 = 109 = one billion 100 = 102 1000 = 103 , 102 x 10
3
= 10
5
(add the exponents)
(2 x 10
2
) x (3 x 10
3)
= 6 x 10
5
10
5
/ 10
3
= 10
2
(subtract
the exponents)
Our CCD at 0.9m was 4
x
10
3
by 4
x
10
3
pixels. How many pixels total?
Slide19The Drake Equation: statistical estimate of the number of intelligent, communicating civilizations in our galaxy right now
Number of stars in our galaxyFraction of stars that have planets around themNumber of planets per star that are capable of supporting life (see habitable zone)Fraction of planets where life evolvesFraction of these planets where intelligent life evolvesFraction of intelligent life that communicatesFraction of a planet’s lifetime during which the civilizations communicate
N equals the product of all these factors!
Slide201. How can we measure the number of stars in our galaxy?
(This isn’t an actual picture of our galaxy. Why?)
Slide21How do we measure the number of stars in our galaxy?
We can use the law of gravity to measure how much mass is within our galactic orbit.
V
c
= velocity of sun around galactic center
r = distance from sun to galactic center
We divide this mass by the average mass per star to get the number of stars
Current best number:
2-4x10
11
stars
(200 to 400 billion)
Slide222. What is the fraction of stars that have planets?
Kepler Project: indicates that practically all sun-like stars have planetsAlthough Kepler looks at a very small fraction of the Milky Way galaxy, it should be representative of most
Slide23Is is appearing that the majority of planets are more earth-like
than Jupiter-like
Slide24http://astro.unl.edu/naap/habitablezones/animations/stellarHabitableZone.html
Slide25Recall the habitable zone concept – warm enough for liquid waterNOV 4 2013: KEPLER PRESS RELEASE:
“one in five stars like the sun is home to a planet up to twice the size of Earth, orbiting in a temperate environment. “3. What number of planets are able to support life?
Slide26The other factors ( 4 through 7 ) are up to you:
Note that this ONLY addresses our galaxy: there are about as many galaxies in the known universe as there are stars in our galaxy!Values you get?
Slide27So, how far might the nearest earth-like planet be?
If there is intelligent life there, do they know about us? (the “I Love Lucy” effect)
Slide28Listening for intelligence: from Project Ozma (1960) to SETI (today)
Slide29SETI Project: search for intelligent signals
SETI@home: 1998, citizen science program, using personal computers to help with data reduction, also support from Planetary Society (private group)
Small percent of time devoted to this search,
Slide30SETI Project: the Allen Telescope array
Need for more telescope time: proposal to build up to 350 small radio telescopes, supported by Paul Allen (Microsoft founder), located at Hat Creek Obs, CA
Went on line in
2007, only 3 telescopes in place
Survey 1,000,000
“
nearby”stars
for SETI
emission
Survey the galactic plane for very powerful transmitters
Slide31What sort of signal is SETI looking for?
The Arecebo telescope does not track the sky, so a exterrestrial signal will drift through its beam.
We might expect an intelligent
exterrestrial
signal to be narrow in frequency, rather than covering a broad range
If the signal contains information, it will be pulsed
Since planets (like us) probably rotate, it may show a Doppler shift , or change in frequency – and this would include
pulses
If we detect a signal, how will we decode it?
Slide32Needless to say, we haven’t heard anything…
do you think we will? How will we decode it?
Slide33Slide34