The Sun - University of Toledoastro1.panet.utoledo.edu › ~relling2 › teach › archives... ·...
Transcript of The Sun - University of Toledoastro1.panet.utoledo.edu › ~relling2 › teach › archives... ·...
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The SunOur very own star
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simultaneous image of
entire sun
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Our own starAn “Average” Star, one of hundreds of billions in the galaxy (but it’s our very own!).
Made entirely of gas. Far too hot for liquids or solids:
Surface: 6000 K
Center: 10 million K
Composed of 70% hydrogen, 28% Helium, 2% everything else (C, N, O, Fe, etc.)
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The stellar family portrait
O B A F G K MType:
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The Sun
The stellar family portrait
O B A F G K MType:
1.0 Msun
5800 K
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The Sun
The stellar family portrait
O B A F G K MType:
1.0 Msun 40 Msun 0.1 Msun
5800 K35000 K 3000 K
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Radius: 6.9 x 108 m (109 times Earth)
Mass: 2 x 1030 kg (300,000 Earths), 99.9% of mass in solar system
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Why does the Sun Shine?
Powered by Human Sacrifice?
The Aztecs thought so.
But... it’s still shining 500 years later.
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Why does the Sun Shine?
Is it on fire, maybe made of Wood, or Coal?
The chemical energy in the sun would only last for 10,000 years! It’s been going for 5 billion!
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Why does the Sun Shine?
Due to gravitational contraction? Works for Jupiter!
It would run out of energy in 25 million years.
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Why does the Sun Shine?
What else is there?
Mass Energy! E=mc2
Much greater source of energy than any other!
One gram of matter holds energy of 15,000 barrels of oil!
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“ The sun is a mass of incandescent gas,A gigantic nuclear furnaceWhere hydrogen is built into heliumAt a temperature of millions of degrees”
— They Might be Giants, Why Does the Sun Shine?
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“ The sun is a mass of incandescent gas,A gigantic nuclear furnaceWhere hydrogen is built into heliumAt a temperature of millions of degrees”
— They Might be Giants, Why Does the Sun Shine?
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What keeps it shining?Sun is in “Hydrostatic Equilibrium”.
It’s large mass creates intense pressure in the center, which makes it HOT (millions of degrees).
Overcomes Coloumb Barrierleads to nuclear fusion, which generates photons and energetic particles.
Sun’s luminosity is 400,000,000,000,000,000,000,000,000 Watts! (also known as ... 4×1026 Watts).
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What keeps it shining?Sun is in “Hydrostatic Equilibrium”.
It’s large mass creates intense pressure in the center, which makes it HOT (millions of degrees).
Overcomes Coloumb Barrierleads to nuclear fusion, which generates photons and energetic particles.
Sun’s luminosity is 400,000,000,000,000,000,000,000,000 Watts! (also known as ... 4×1026 Watts).
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Gravity vs. Pressure
It’s a battle: gravity fighting against pressure.
Pressure created by the heat, heat produced by the nuclear reactions!
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The solar thermostat
TemperatureRestored
TemperatureDecreases
Fusion Rate Decreases
Corecompresses
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What would happen inside the Sun if a slight rise in core temperature led to a rapid rise in fusion energy?
A) The core would expand and heat up slightly
B) The core would expand and cool
C) The Sun would blow up like a hydrogen bomb
A BC D
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What would happen inside the Sun if a slight rise in core temperature led to a rapid rise in fusion energy?
A) The core would expand and heat up slightly
B) The core would expand and cool
C) The Sun would blow up like a hydrogen bomb
A BC D
✪
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What makes stars shine?
16
gravity5,800 K
16,000,000 K
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What started The Sun shining?
Gravitational contraction!
(even though it doesn’t explain why it shines now).
Contracting material heated up, until hot enough for nuclear “fusion” to occur.
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Nuclear Reactions• Fusion:
two light nuclei joined into one nucleus
powers the Sun
• Fission:
massive nucleus splits in smaller nuclei
powers nuclear reactors (Davis-Besse)
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Converting Mass to EnergyNuclear reactions change mass of constituents
Mass increase consumes energy
Mass decrease releases energy
Mass decreases in
Fission of heavy nucleiCan occur spontaneously
natural radioactivity
Fusion of light nucleiLike charges repel
Fusion requires high speed
Temperature > 10 million K
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Fusion: Sun’s Energy Source
Sun’s core:
Temperature = 15 million K
Hot enough to fuse hydrogen
p-p chain (proton-proton)
Series of fusion reactions
Converts:4 hydrogen to 1 helium
mass of 4 H great than mass of 1 He: this mass decrease is the energy source!! Only 0.7% difference
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Fusion on Earth
Always 30 years away.
Elaborate magnetic plasma chambers.
How does the sun do it so well?
In solar core, power production density from fusion is 250 W/m3.
Compare this to yourself.
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Sun: latest View
8 hrs ago!
From the SOHO
spacecraft
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More SOHO
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Major Regions of the Sun
InteriorCore
Radiative Zone
Convective Zone
AtmospherePhotosphere
Chromosphere
Corona
Solar Wind
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Photosphere
Effective “surface” of sunnot solid, just the region we see by eye
Thin atmospheric layerFew hundred km
Low density gas0.01% Earth’s atmosphere
Close-up shows granulationconvection cells
SunspotsSomewhat Cooler than surrounding gas. appear dark
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The sun’s atmosphere
Photosphere: 6000K lower layer.
Chromosphere: 10,000 K “middle layer”
Corona: 1 million K “outermost layer”, extends to several million KM above the surface!
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Spacecraft HinodeThursday, January 17, 13
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How does energy get out of the sun?
Convection (think of boiling oatmeal).
Radiation: A random walk.
takes a photon a fewmillion years to reachthe surface!
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How does energy get out of the sun?
Convection (think of boiling oatmeal).
Radiation: A random walk.
takes a photon a fewmillion years to reachthe surface!
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Bright Blobs: where hot gas reaches the surface by convection
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Bright Blobs: where hot gas reaches the surface by convection
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Atmospheric Features
SunspotsOften larger than Earth
Occur in groups
Associated with magnetic fields
Galileo used to measure solar rotation
25 days at equator (longer at poles)
Number of sunspots is cyclical, with 11 year period (actually 22)
Correlated with solar activity: greatest activity at sunspot maximum, least at minimum
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Galileo’s Sunspot Drawings
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Solar Rotation
Fastest at
Equator
Slower at
Poles
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Magnetic Fields
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Sunspot Cycle
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Sunspot +Granulation
Umbra(T ~ 3900K)
Penumbra
NOAO/NSO
Photosphere(T ~ 5770K)
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Most Detailed Sunspot Image Ever!
Swedish Vacuum TelescopeThursday, January 17, 13
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Atmospheric Features
Prominences
Loops of hot gas
Base near sunspots
Trace magnetic fields
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Image Credit:NASA/SOHO
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Solar Wind
Gas flows away from sun
10 million tons/yr
protons & electrons
speed 400-800 km/s
Material goes outward into solar system
Hits Earth’s atmosphere
makes it glow (aurorae)
trapped in Earth’s magnetic field lines
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Solar Wind
Gas flows away from sun
10 million tons/yr
protons & electrons
speed 400-800 km/s
Material goes outward into solar system
Hits Earth’s atmosphere
makes it glow (aurorae)
trapped in Earth’s magnetic field lines
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Solar Flare Image Credit:NASA/TRACE
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Solar Flares
Eruptions caused by magnetic fields
may last 5-10 min
release huge amounts of energy
gas heated to 107 K, produces X-rays and UV radiation
Coronal Mass Ejections
very large flares
large mass of gas ejected from corona
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Image Credit:NASA/SOHO
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Image Credit:NASA/SOHO
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Solar Variability & Earth’s ClimateSolar Luminosity Varies by 1%
Highest at sunspot maximum
Lowest at minimum activity
Maunder minimum 1650-1700
Very few sunspots
“Little Ice Age” in
Europeextreme cold temps
shorter growing season
Still learning how Sun affects Earth’s climate
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Blackbody Radiation
A perfect absorber is “black”
Absorbs all light shining on it
Absorbed light (energy) heats object
Temperature increases until:
emitted energy = absorbed energy
Emitted radiation called Blackbody Radiation
The thermal radiation emitted by most objects, include stars is similar to blackbody
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Thermal Radiation
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All “solid” objects emit light
55
15,000 K Star
6,000 K Sun
3,000 K Star
X−Ray UV Visible Infrared Radio
0.01 0.1 1 10 100 1000 10000Wavelength (µm)
106
108
1010
1012
1014
1016
1018
1020
Rel
ativ
e In
tens
ity
Orion
Betelgeuse
Rigel
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All “solid” objects emit light
55
15,000 K Star
6,000 K Sun
3,000 K Star
X−Ray UV Visible Infrared Radio
0.01 0.1 1 10 100 1000 10000Wavelength (µm)
106
108
1010
1012
1014
1016
1018
1020
Rel
ativ
e In
tens
ity
Orion
Betelgeuse
Rigel
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All “solid” objects emit light
55
15,000 K Star
6,000 K Sun
3,000 K Star
X−Ray UV Visible Infrared Radio
0.01 0.1 1 10 100 1000 10000Wavelength (µm)
106
108
1010
1012
1014
1016
1018
1020
Rel
ativ
e In
tens
ity
Orion
Betelgeuse
Rigel
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Planck FunctionWien’s law, rayleigh-Jeans Tail, known empirically.
Planck derived the function in 1900, to account for laboratory measurements of the spectra of heated objects.
Required a minimum “quantum of action” and it’s associated constant... first serious step to quantization of light
B�(T ) =2hc2
�5
1
ehc/�kT � 1
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Spectra
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The Sun’s spectrum is not so simple
59
6,000 K SunActual Sun
X−Ray UV Visible Infrared Radio
0.01 0.1 1 10 100 1000 10000Wavelength (µm)
106
108
1010
1012
1014
1016
1018
1020R
elat
ive
Inte
nsity
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Fate of the SunSun has a finite lifetime (why?) around 10 billion years. Currently around halfway through.
A.D. 5,000,000,000: Sun’s luminosity will go up by 1000×! Earth temperature 1000K.
Sun will swell to the earth’s orbit, before turning into a white dwarf.
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Planetary Nebulae
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