Transcript The Origin of the Solar System

The Origin of the
Solar System
Movie: The History
of the Solar System
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How old is the Solar System?
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1.3 million years
350 million years
1.7 billion years
4.5 billion years
13 billion years
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The Formation of Stars:
Giant Molecular Clouds
Barnard 68
Visible
Star formation ← collapse of the cores of giant molecular clouds:
Dark, cold, dense clouds obscuring the light of stars behind them.
Which wavelength range is adjacent to
the visible spectrum and has longer
wavelengths than visible light?
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X-rays
Gamma-Rays
Stingrays
Infrared light
Ultraviolet light
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The Formation of Stars:
Giant Molecular Clouds
Barnard 68
Infrared
Visible
Star formation ← collapse of the cores of giant molecular clouds:
Dark, cold, dense clouds obscuring the light of stars behind them.
(More transparent in infrared light.)
Parameters of Giant Molecular Clouds
Size: r ~ 50 pc
Mass: > 100,000 Msun
Temp.: a few 0K
Dense cores:
R ~ 0.1 pc
M ~ 1 Msun
(Bok) Globules
Compact,
dense pockets
of gas which
may contract
to form stars.
~ 10 – 1000
solar masses;
Contracting to
form protostars
Protostars
Protostars =
pre-birth state
of stars:
Hydrogen to
Helium fusion
not yet ignited
Still enshrouded
in opaque
“cocoons” of dust
=> barely visible
in the optical, but
bright in the
infrared.
Do you expect stars to form isolated?
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Yes.
No, they should form in
groups of a few (2 – 5)
No, they should form in
large groups (several
100s or 1000s)
No, actually all stars in a
galaxy (several billions)
should form at the same
time.
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Open
Clusters
of Stars
Large masses of
Giant Molecular
Clouds => Stars
do not form
isolated, but in
large groups,
called Open
Clusters of Stars.
Open Cluster M7
What happens to a spinning
object if it contracts?
1) It stops rotating.
2) Its rotation slows down.
3) Its rate of rotation
remains unchanged.
4) Its rotation speeds up.
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Protostellar
Disks
Conservation of angular
momentum leads to the
formation of protostellar
disks → birth place of
planets and moons
The Solar Nebula
Hypothesis
Planets form at the
same time from the
same cloud as the star.
Planet formation sites
observed today as dust
disks of T Tauri stars.
Sun and our Solar system
formed ~ 4.6 billion years ago.
Would you expect that other stars
have planetary systems too?
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1) Yes.
2) No.
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Extrasolar Planets
All stars have gone through basically the
same formation process as the sun.
→ Many stars should have planets!
→ planets orbiting
around other stars =
“Extrasolar planets”
Extrasolar planets can
not be imaged directly.
Detection using the
“wobbling” technique:
Look for “wobbling”
motion of the star due to
the gravitational pull of
the planet on the star.
Would you expect that there are still new
solar systems being formed at this time?
1) Yes.
2) No.
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Evidence
for Ongoing
Planet
Formation
Many young
stars in the Orion
Nebula are
surrounded by
dust disks:
Probably sites of
planet formation
right now!
Dust Disks
around
Forming
Stars
Dust disks around
some T Tauri stars
can be imaged
directly (HST).
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The decay of atomic nuclei,
resulting in the emission of
radio waves.
The decay of atomic nuclei,
resulting in the emission of
gamma-rays.
The fusion of atomic nuclei,
resulting in the emission of
radio waves.
The fusion of atomic nuclei,
resulting in the emission of
gamma-rays.
The emission of radio waves
by stars like our sun.
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What is
radioactivity?
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The Age of the Solar System
Sun and planets should
have about the same age.
Ages of rocks can be
measured through
radioactive dating:
Measure abundance of a
radioactively decaying
element to find the time
since formation of the rock
Dating of rocks on Earth,
on the Moon, and
meteorites all give ages of
~ 4.6 billion years.
If you start out with 1 kg of a radioactive
substance with a half-life of 150 years, how
long does it take until there is nothing left?
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150 years.
300 years.
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1,500 years.
An infinite amount of
time (in principle).
Impossible to tell with
the given information.
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What is “condensation”?
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The melting of a substance.
The transition of a substance
from the liquid to the gas
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The transition of a substance
from the gas to the liquid
phase.
The transition of a substance
from the liquid to the solid
phase.
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Condensation in the Early Solar System
Only condensed materials
could stick together to
form planets
Temperature in the
protostellar cloud
decreases outward.
Further out → Protostellar
cloud cooler → metals
with lower melting point
condensed → change of
chemical composition
throughout solar system
→ Average density of planets
decreases outwards!
Lighter substances
condense at lower
temperatures.
Formation and Growth
of Planetesimals
Planet formation starts
with clumping together of
grains of solid matter:
Planetesimals
Planetesimals (few cm
to km in size) collide to
form planets.
Planetesimals grow
through condensation
and accretion.
What happens if you try to
mix oil and water?
1)
They will mix to a uniform
solution.
The oil will sink to the bottom,
the water will “swim” on top of
it.
The water will sink to the
bottom, the oil will “swim” on
top of it.
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The Growth of
Protoplanets
As rocks melted,
heavier elements sink
to the center →
differentiation
→ Terrestrial planets
have heavy-metal (iron)
cores and mantles of
lighter substances
The Story of Planet Building
Planets formed from the same
protostellar material as the sun.
Rocky planet material formed from clumping
together of dust grains in the protostellar cloud.
Mass of less than ~ 15
Earth masses:
Planets can not grow by
gravitational collapse
Earthlike planets
Mass of more than ~ 15
Earth masses:
Planets can grow by
gravitationally attracting material
from the protostellar cloud
Jovian planets (gas giants)
Which features on the surface of the moon tell
us that there were many small bodies (rocks)
remaining in the solar system after it formed?
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A dense atmosphere.
The large, uncratered
maria.
Lots of impact craters
in the lunar highlands.
High mountains.
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Clearing the Nebula
Remains of the protostellar nebula were cleared away by:
• Sweeping-up of space debris by planets
• Ejection by close encounters with planets
Surfaces of the Moon and Mercury show evidence for
heavy bombardment by asteroids.
Ejection of small bodies by
massive planets
Clearing the Nebula
Remains of the protostellar nebula were cleared away by:
• Sweeping-up of space debris by planets
• Solar wind
• Ejection by close encounters with planets
• Radiation pressure of the sun
Surfaces of the Moon and Mercury show evidence for
heavy bombardment by asteroids.
Final overview movie