Astronomy 2. Most of human history, people thought sun burned some type of fuel to make energy Not...
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![Page 1: Astronomy 2. Most of human history, people thought sun burned some type of fuel to make energy Not until the 21 st century did scientists figure out.](https://reader030.fdocuments.us/reader030/viewer/2022032607/56649ed15503460f94bdf61a/html5/thumbnails/1.jpg)
Astronomy 2
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Most of human history, people thought sun burned some type of fuel to make energy
Not until the 21st century did scientists figure out where sun’s energy comes from
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Electromagnetic energy is a type of energy that can travel through space an example is visible light
Light travels in wavelengths There are many things
that travel in wavelengths (radio waves, microwaves, ultraviolet rays, x-rays)
The electromagnetic spectrum breaks visible light down into the colors that make it up When you shine light
through a prism you can see the different colors of visible light
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Visible light is composed of red, orange, yellow, green, blue and violet – like a rainbow
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1. Core2. Inner zones3. Atmosphere
Inner zones and atmosphere divided into more layers
Continuous – gradual change between layers
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Makes up 10% of sun’s diameter
Diameter = 1,300,000 km
Temp at core is 15,000,000 ℃
No liquid or solid can exist – entirely plasma
Sun’s mass 300,000 times bigger than Earth’s mass
So, gravity is greater Center of sun – 10 times
more dense than iron
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Pressure and heat of sun change structure of atoms in core
Most atoms are nucleus surrounded by electrons
Heat and pressure of sun strips electrons from nuclei plasma
Nuclei can be changed by nuclear reactions
Hydrogen fused into helium
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Nuclei of hydrogen atoms are primary elements in fusion of sun
Hydrogen made of 1 proton, 1 electron
Electron ripped off, so only protons remain
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1. Two hydrogen nuclei (protons) collide and fuse
2. One of the protons changes to neutron
3. Another proton combines with proton-neutron pair making a nucleus of 2 protons
4. Two of these nuclei collide and fuse
5. Resulting group throws off two protons
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Remaining combination of 2 protons and 2 neutrons is nucleus of helium atom
During each step, energy given off
Helium nucleus has about 0.7% less mass than hydrogen nuclei that combined to form it
Loss in mass converted to energy
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Hoover Dam provides energy to most of Western US
2,080 megawatts
380 billion billion megawatts EVERY SECOND
380,000,000,000,000,000,000
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Before reaching sun’s atmosphere, energy made in core moves through two inner zones
Radiative zone surrounds core
Temp is about 2,500,000℃
Energy moves from atom to atom as radiation
Electromagnetic radiation transfers energy through space
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Convective zone around radiative zone
Temp about 1,000,000℃
Energy made in core moves by convection transfer of energy by moving liquids or gases
Hot gases carry heat energy to sun’s surface
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As atoms of hot gases move out and expand, they radiate and lose heat
Cooling gases become denser than other gases Sink to bottom of convection zone There, cooled gases heated by radiative zone
and rise again Heat transferred to surface as gases rise and
sink
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Surrounds convective zone Atmosphere uppermost area of solar
gases Has 3 layers1. Photosphere2. Chromosphere3. Corona
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Photosphere innermost layer of solar atmosphere
Made of gases bubbling up from convective zone
Temp about 6,000℃ Layer has grainy
appearance called granulation
Results from gases rising and sinking
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Much of energy given off is as visible light
It’s what we see from earth
So, photosphere is considered “surface” of the sun
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Chromosphere “color sphere” above photosphere
Thin layer of gases that glows with reddish light
Temp ranges from 4,000-50,000℃
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Gases of chromosphere move away from and toward photosphere
In upward movement, they sometimes form narrow jets of hot gas that shoot out from chromosphere then fade
Sometimes these jets reach 16,000 km high
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Corona “crown” outermost layer of sun’s atmosphere
Huge cloud of gas heated by sun’s magnetic field to temp of about 2,000,000℃
Relatively thin Prevents most atomic particles from sun’s
surface from escaping into space
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Some electrically charged particles (ions) leak into space through holes in corona
Particles are called solar wind
Chromosphere and corona not seen from earth b/c of brightness of blue sky during the day
During solar eclipse – moon blocks sun – can see corona
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Solar Activity
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Gases of inner zones and atmosphere are in constant motion
Energy made in sun’s core and force of gravity combine to cause rising and falling of gases
Gases also move because sun rotates on its axis
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Because the sun is plasma/gas, not solid, different parts rotate at different speeds
Closest to sun’s equator take only 25.3 earth days to make one rotation
Points near poles take 33 earth days
Average = 27 earth days
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Combination of up-and-down movement of gases in convective zone and movement of sun’s rotation produces magnetic fields
These fields slow down activity in convective zone
Slower convection means less gas is transferring heat from core to photosphere
So, regions of photosphere near strong magnetic fields are up to 3,000℃ cooler than surrounding areas
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Cooler areas appear darker than areas around them
Sunspots cool, dark areas of gas within photosphere that are caused by magnetic fields
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Large sunspots can be more than 100,000 km in diameter (several times the size of earth)
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Astronomers found that sunspots first appear in groups midway between sun’s equator and poles
As they disappear, new ones seems to appear near sun’s equator
Shift of sunspots was one of first indications that sun rotates
Number of sunspots also changes according to average 11-year cycle called the sunspot cycle
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Sunspot cycle begins when number of sunspots is very low but is starting to increase
May not see any for several weeks
Gradually see more and more
Increases over next few years until it reaches a peak
At peak, 100 or more sunspots may be visible
After, they decrease Cycle begins when more
sunspots begin to appear
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Magnetic fields also create other disturbances
Prominences great clouds of glowing gases
Form huge arches that reach above sun’s surface
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Each solar prominence follows curved lines of magnetic force from one sunspot area to another
Some may last for several weeks or a year
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One violent solar disturbance is solar flare sudden outward eruption of electrically charged atomic particles
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May extend upward several thousand km within minutes
Few last more than 1 hour
Usually occur near sunspots
During peak in sunspot cycle, 5-10 solar flares can be seen each day
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Some particles from solar flare flung out so forcefully they escape into space
These particles increase strength of solar wind
As they enter atmosphere of earth, they produce sudden disturbance in earth’s magnetic field magnetic storm
Interfere with communications on earth
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Auroras effect of magnetic storm appears in sky as bands of light
When ions of solar wind approach earth, they are guided toward magnetic poles of earth by earth’s magnetosphere
Magnetosphere contains the magnetic field of earth
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The ions hit the gas molecules in upper atmosphere, and produces green, red, blue or violet lights
Usually seen near poles
Also called northern lights or southern lights
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Auroras usually happen 100 and 1,000 km above earth’s surface
Most frequent just after peak in sunspot cycle, especially after solar flares
Visible about 5 times a year
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http://www.youtube.com/watch?v=982cTjWx_zc&feature=player_embedded
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Formation of the Solar System
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Includes sun and bodies revolving around the sun
1600-1700s scientists thought sun formed first, then threw off materials that later formed the planets 8 major bodies revolving around the sun
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1796 – Marquis Pierre Simon de Laplace had a new idea
The sun and planets made from same spinning nebula
The entire solar system formed at about the same time
Nebular theory
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From big bang, some matter gathered into clouds of dust and gas
Cloud of gas and dust that developed into our solar system is called the solar nebula
Larger than our solar system now
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About 4-5 billion years ago, shock waves from nearby supernova or some other force caused cloud of gas and dust to contract, forming solar nebula
A star (the sun) started to form in center When temp high enough, fusion began About 99% of matter in solar nebula
became part of the sun
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Planets formed in outer regions of solar nebula
Small bodies of matter in solar nebula called planetesimals joined together through collisions
Formed larger bodies called protoplanets
Gravity of protoplanets acted like magnets, pulling in other planetesimals from solar nebula
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Eventually protoplanets condensed into existing planets and moons
Moons smaller bodies that orbit the planets
Both planets and moons are smaller and denser than protoplanets
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Distance between protoplanet and developing sun influenced the composition of the planet that formed from the protoplanet
Four protoplanets closest to sun became Mercury, Venus, Earth and Mars
Contained large amounts of heavier elements like iron
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Next four protoplanets became Jupiter, Saturn, Uranus, and Neptune
These formed in the cold areas of solar nebula
Icy material of outer protoplanets made of helium and hydrogen and frozen gases (water, methane, ammonia)
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Inner planets probably could not build up gases b/c gravity is weak
Solar wind may have stripped away early atmosphere of lighter elements
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b/c outer planets further away from sun and have HUGE gravity, they kept most of their original gases
Called the gas giants
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When first formed, it was very hot 3 things contributed to heat1. Earth kept a lot of heat made when it
collided with planetesimals2. Increasing weight of outer layers pressed
on inner layers, making more heat3. Radioactive materials (radiate heat) were
plenty when earth first formed
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Temp on young earth enough to melt iron Gravity pulled molten iron to center Denser materials flowed to center Less dense materials forced to outer
layers Earth eventually separated into 3 layers
Crust Mantle Core
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The protoplanet that became earth could not hold gases b/c gravity was too weak
Collisions added more mass to protoplanet, gravity increased
Eventually it captured some hydrogen and helium that were in solar nebula
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By the time earth was formed, the atmosphere was mostly hydrogen and helium
Today these two found mostly in upper atmosphere
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Much of earth’s first atmosphere was probably lost as result of solar explosion or solar wind
Earth’s second atmosphere results from explosions within earth about 3 billion years ago
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Heat in interior caused volcanoes to form
Volcanic eruptions released large amounts of gases
Mostly water and carbon dioxide
These formed new atmosphere
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Sunlight probably caused ammonia and some water in atmosphere to form nitrogen, hydrogen and a little oxygen
Most of hydrogen escaped to outer space (too light to be held by gravity)
Early green plants – photosynthesis – increase levels of oxygen
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Some oxygen formed ozone (in upper atmosphere)
Shielded earth from UV radiation from sun
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As atmosphere was developing, earth was cooling enough for liquid water to form
Between 3-3.5 billion years ago water vapor started to condense
Fell as rain and formed oceans in lower surface areas
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Ocean water absorbed carbon dioxide from atmosphere
By 1.5 billion years ago, atmosphere similar to what it is today