The Sun Our Star. Warm Up Summarize what you remember from the film “The Elegant Universe” in a...

The SunThe Sun

Our StarOur Star

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Summarize what you remember from Summarize what you remember from the film “The Elegant Universe” in a the film “The Elegant Universe” in a few paragraphs. Is string theory a few paragraphs. Is string theory a “theory” or a “philosophy?” Why or “theory” or a “philosophy?” Why or why not?why not?

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1.1. Describe stage 1 on the proton-proton Describe stage 1 on the proton-proton chain, products and remnants.chain, products and remnants.




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1.1. To make the math work out correctly, To make the math work out correctly, how many dimensions are required in how many dimensions are required in the Universe?the Universe?

2.2. What is a membrane or “brane” to a What is a membrane or “brane” to a string theorist?string theorist?

3.3. What happens (theoretically) when What happens (theoretically) when membranes collide?membranes collide?

4.4. What is the purpose of the What is the purpose of the supercollider in CERN?supercollider in CERN?

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1.1. What historical event occurred that What historical event occurred that provided the catalyst to create the provided the catalyst to create the Mercury space program.Mercury space program.

2.2. Who was the first man is space?Who was the first man is space?

3.3. Who was the first American in space?Who was the first American in space?

4.4. Who was Chuck Yeager and what did Who was Chuck Yeager and what did he do that made him famous?he do that made him famous?

5.5. Who was the last Mercury Who was the last Mercury

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1.1. How far away is the Sun?How far away is the Sun?

2.2. How much more massive is the Sun How much more massive is the Sun than the Earth?than the Earth?

3.3. What are the three layers of the What are the three layers of the Sun?Sun?

4.4. What are the two zones of the Sun?What are the two zones of the Sun?

Warm UpWarm Up1.1. What is the northern-most constellation at What is the northern-most constellation at

midnight tonight?midnight tonight?

2.2. What was the eastern-most constellation on What was the eastern-most constellation on Christmas at 10:00 pm?Christmas at 10:00 pm?

3.3. What was the southern-most constellation on What was the southern-most constellation on New Years Day at 8:00 pm.New Years Day at 8:00 pm.

4.4. What constellation is located at the center of What constellation is located at the center of your planesphere?your planesphere?

5.5. What was the northern-most constellation on What was the northern-most constellation on your past birthday at noon.your past birthday at noon.

6.6. Name 3 constellations that are visible tonight at Name 3 constellations that are visible tonight at 9:00 pm.9:00 pm.

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1.1. What powers the SunWhat powers the Sun

2.2. What does the Sun do, besides give off heat What does the Sun do, besides give off heat and light?and light?

3.3. What are the Sun’s two atmospheric layers?What are the Sun’s two atmospheric layers?

4.4. What happens in the radiative zone of the What happens in the radiative zone of the Sun?Sun?

5.5. What happens in the convective zone of the What happens in the convective zone of the Sun?Sun?

6.6. How old is our Sun?How old is our Sun?

7.7. What is hydrostatic equilibrium?What is hydrostatic equilibrium?

Sun Webquest Sun Webquest http://jn016.k12.sd.us/sun_webquest_sites.htmhttp://jn016.k12.sd.us/sun_webquest_sites.htm

1. How old is the sun? 1. How old is the sun? 2. What is the temperature of the sun? (in Fahrenheit)2. What is the temperature of the sun? (in Fahrenheit)3. How far away is the sun from the Earth? ( Tell us in miles & 3. How far away is the sun from the Earth? ( Tell us in miles & kilometers)kilometers)4. What are the layers of the Sun? Give a brief description of the 4. What are the layers of the Sun? Give a brief description of the major layers AND include a labeled picture of our Sun's layers.major layers AND include a labeled picture of our Sun's layers.5. What is the chemical make up (elements)of the sun?5. What is the chemical make up (elements)of the sun?6. What are the percentages of those chemicals?6. What are the percentages of those chemicals?7. What are sunspots?7. What are sunspots?8. When were sunspots first discovered and who discovered 8. When were sunspots first discovered and who discovered them?them?9. How are magnetic storms on Earth related to sunspot activity?9. How are magnetic storms on Earth related to sunspot activity?10. How does the number of sunspots change over time?10. How does the number of sunspots change over time?11. Describe what causes each of the following: prominences, 11. Describe what causes each of the following: prominences, solar flares, solar wind, CME’s (coronal mass ejections)solar flares, solar wind, CME’s (coronal mass ejections)12. How does the sun get its energy?12. How does the sun get its energy?13. What is nuclear fusion? 13. What is nuclear fusion? 14. How can you safely observe the sun?14. How can you safely observe the sun?

Our StarOur StarOur star, the Sun, is a dazzling Our star, the Sun, is a dazzling luminous ball of burning gas one luminous ball of burning gas one hundred times the radius of the hundred times the radius of the Earth. Viewed normally, the Sun Earth. Viewed normally, the Sun seems peaceful and regular, but seems peaceful and regular, but viewed through a telescope, the Sun viewed through a telescope, the Sun is a teaming, explosive place where is a teaming, explosive place where fountains of heated gas leap 100’s of fountains of heated gas leap 100’s of miles above the surface.miles above the surface.

Scale of the Solar SystemScale of the Solar SystemThe Sun dwarfs the rest of the solar The Sun dwarfs the rest of the solar system. 100 times the radius of the system. 100 times the radius of the Earth, the Sun has a mass 300, 000 Earth, the Sun has a mass 300, 000 times that of our planet. times that of our planet.

Solar FactsSolar FactsThe Sun is about 93 million miles from Earth.The Sun is about 93 million miles from Earth.

Surface gravity on the Sun is about 30 times Surface gravity on the Sun is about 30 times that felt by a body on Earth.that felt by a body on Earth.

The Sun’s surface temperature is about The Sun’s surface temperature is about 5,800 K.5,800 K.

The Sun’s core temperature is about 15 The Sun’s core temperature is about 15 million K.million K.

The Sun’s core is 100 times denser than The Sun’s core is 100 times denser than water.water.

Solar FactsSolar FactsThe mass of the Sun is about The mass of the Sun is about 333,000 times the mass of the Earth.333,000 times the mass of the Earth.

It is estimated that the Sun releases It is estimated that the Sun releases about 4 X 10about 4 X 102626 watts into space from watts into space from its surface.its surface.

The Sun is composed of 71% The Sun is composed of 71% hydrogen, 21% helium and 2% hydrogen, 21% helium and 2% heavier materials such as carbon and heavier materials such as carbon and iron.iron.

The Sun’s InteriorThe Sun’s Interior

The Sun is The Sun is composed of composed of several layers:several layers:

1.1. The PhotosphereThe Photosphere

2.2. The ChromosphereThe Chromosphere

3.3. The CoronaThe Corona

And two distinct And two distinct zoneszones

1.1. Radiative ZoneRadiative Zone

2.2. Convective ZoneConvective Zone

The PhotosphereThe PhotosphereThe outside of the Sun is relatively The outside of the Sun is relatively transparent, however, with increased transparent, however, with increased depth the Sun becomes opaque. The depth the Sun becomes opaque. The cause of this is that at a certain depth cause of this is that at a certain depth the weight of the overlying gas crushes the weight of the overlying gas crushes the underlying gases together so tightly the underlying gases together so tightly that they can not be seen.that they can not be seen.

The photosphere The photosphere makes up the portion of makes up the portion of the Sun that we cannot see.the Sun that we cannot see.

Radiative ZoneRadiative ZoneNear the Sun’s core, energy is moved Near the Sun’s core, energy is moved by radiation carried by photons by radiation carried by photons (remember those?). This area is (remember those?). This area is called the called the radiative zoneradiative zone. Because . Because the gas there is so dense, before the gas there is so dense, before most photons travel an inch, they are most photons travel an inch, they are absorbed by an atom and stopped. absorbed by an atom and stopped. The photon will be re-emitted later The photon will be re-emitted later only to be stopped by another atom. only to be stopped by another atom.

Radiative ZoneRadiative ZoneLike traffic stuck at a light, the Like traffic stuck at a light, the photons are delayed. This delay is photons are delayed. This delay is quite long, to the extent that the quite long, to the extent that the sunlight we see today was generated sunlight we see today was generated about 16 million years ago.about 16 million years ago.

The Convection ZoneThe Convection ZoneJust below the photosphere where Just below the photosphere where the gas is cooler and less the gas is cooler and less transparent, the flow of energy is transparent, the flow of energy is slowed. In this region, photons are slowed. In this region, photons are even less effective at moving energy.even less effective at moving energy.

The Convective ZoneThe Convective ZoneConvection currents carry energy from Convection currents carry energy from this region toward the Sun’s surface. this region toward the Sun’s surface. These are like similar currents within These are like similar currents within the Earth and the gas giant planets.the Earth and the gas giant planets.

This is why the This is why the

region is called the region is called the

convection zone.convection zone.

The Convective ZoneThe Convective ZoneWhile we can’t see these gases, we While we can’t see these gases, we can infer their motion by observing can infer their motion by observing tiny bright regions surrounded by tiny bright regions surrounded by darker areas that appear on the darker areas that appear on the surface. These are called surface. These are called granulesgranules. . These These granulationsgranulations form from form from bubbles of rising hot gas. bubbles of rising hot gas.

The Convective ZoneThe Convective ZoneThese rising bubbles burst and cool, These rising bubbles burst and cool, emanating heat and light into space. emanating heat and light into space. The cooling gases subside and turn The cooling gases subside and turn dark, creating the dark edges that dark, creating the dark edges that surround each granule.surround each granule.

The Convection ZoneThe Convection ZoneUsing the Doppler Effect, scientists Using the Doppler Effect, scientists have measured how rapidly this have measured how rapidly this granules rise and found that their granules rise and found that their average speed is about one average speed is about one kilometer per second (km/s).kilometer per second (km/s).

The Sun’s AtmosphereThe Sun’s AtmosphereScientist refer to the very low density Scientist refer to the very low density gases above the Sun’s photosphere gases above the Sun’s photosphere as the Sun’s atmosphere. This as the Sun’s atmosphere. This atmosphere, like the Earth’s, atmosphere, like the Earth’s, becomes gradually thinner the becomes gradually thinner the farther it extends into outer space. farther it extends into outer space.

The Sun’s AtmosphereThe Sun’s Atmosphere

You’d think with the density of the You’d think with the density of the gases decreasing, that the temperature gases decreasing, that the temperature would decrease too, but just the would decrease too, but just the opposite occurs. Because they are opposite occurs. Because they are more easily heated at higher altitudes, more easily heated at higher altitudes, the gases burn with great intensity. the gases burn with great intensity. The temperature immediately above The temperature immediately above the photosphere has an average the photosphere has an average temperature of several million Kelvin.temperature of several million Kelvin.

The Sun’s AtmosphereThe Sun’s AtmosphereThe Sun’s atmosphere consists of The Sun’s atmosphere consists of two major divisions; the two major divisions; the chromospherechromosphere lies directly about lies directly about the photosphere and it is the Sun’s the photosphere and it is the Sun’s lower atmosphere. lower atmosphere.

ChromosphereChromosphereThe chromosphere consists of The chromosphere consists of millions of jets of hot gas called millions of jets of hot gas called spicules. Spicules are generally spicules. Spicules are generally thousands of kilometers long. The thousands of kilometers long. The chromosphere’s red color comes chromosphere’s red color comes from the strong emission spectrum of from the strong emission spectrum of hydrogen.hydrogen.

The CoronaThe CoronaThe outer-most layer of the Sun’s The outer-most layer of the Sun’s atmosphere is the corona.atmosphere is the corona. The The temperature in the chromosphere is temperature in the chromosphere is about 4,500 K, but only about 2,000 about 4,500 K, but only about 2,000 km’s higher the temperature soars to km’s higher the temperature soars to 50,000 K. 50,000 K.

The CoronaThe CoronaSince rising into the corona from the Since rising into the corona from the chromosphere, the temperature of a chromosphere, the temperature of a gas may have climbed 1 million gas may have climbed 1 million degrees. Despite its high degrees. Despite its high temperatures, the corona has very temperatures, the corona has very little energy due to its lack of little energy due to its lack of density.density.

Stellar EquilibriumStellar EquilibriumOur Sun, like all healthy stars, exists in a Our Sun, like all healthy stars, exists in a state of equilibriumstate of equilibrium. Gravity pulls in the . Gravity pulls in the Sun’s mass toward its center with Sun’s mass toward its center with tremendous force. But, the Sun also tremendous force. But, the Sun also pushes out (with heat and energy) with pushes out (with heat and energy) with great force. It pushes out exactly as hard great force. It pushes out exactly as hard as gravity pulls it in.as gravity pulls it in.

This balance of forcesThis balance of forces

maintains the stabilitymaintains the stability

of our star. This is knownof our star. This is known

as as hydrostatic equilibriumhydrostatic equilibrium..

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2.2. Why does the Sun have a limited life time?Why does the Sun have a limited life time?

3.3. What does heat create?What does heat create?

4.4. What is a granule?What is a granule?

5.5. What is a spicule?What is a spicule?

6.6. The earliest astronomers thought that the Sun The earliest astronomers thought that the Sun was fueled by what? And would last how long?was fueled by what? And would last how long?

7.7. Who was the first dude to think that the Sun was Who was the first dude to think that the Sun was power by subatomic energy?power by subatomic energy?

8.8. Who was the first dude to confirm it?Who was the first dude to confirm it?

9.9. What did Einstein have to do with all this?What did Einstein have to do with all this?

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2.2. Why does the Sun have a limited life Why does the Sun have a limited life time?time?

3.3. What does heat create?What does heat create?

4.4. What is a granule?What is a granule?

5.5. What is a spicule?What is a spicule?

Stellar EquilibriumStellar EquilibriumEquilibrium comes at a price, Equilibrium comes at a price, however. In order to maintain its however. In order to maintain its outward force, outward force, the Sun has to the Sun has to consume itself as fuelconsume itself as fuel. As an area of . As an area of limited resources, the Sun will one limited resources, the Sun will one day exhaust its fuel supply and die. day exhaust its fuel supply and die. Every second the Sun consumes 4 Every second the Sun consumes 4 million tons of itself.million tons of itself.

Pressure in the SunPressure in the Sun

The The pressurepressure that counter-balances that counter-balances gravity’s forces comes from the rapid gravity’s forces comes from the rapid motion of atoms. For a better motion of atoms. For a better understanding of the Sun, we must understanding of the Sun, we must understand understand pressurepressure..

Pressure cookerPressure cooker

Pressure in the SunPressure in the Sun

Pressure comes from atoms and Pressure comes from atoms and molecules colliding. The more molecules colliding. The more you compress something, the you compress something, the closer its atoms and molecules closer its atoms and molecules are and the more collisions that are and the more collisions that occur. This is called occur. This is called densitydensity. . This creates pressure.This creates pressure.

Pressure in the SunPressure in the SunThe more you heat something, The more you heat something, the faster its atoms and the faster its atoms and molecules move and the more molecules move and the more violently they collide. This violently they collide. This creates pressure as well.creates pressure as well.

The Ideal Gas LawThe Ideal Gas Law

We’ve established the relationship between We’ve established the relationship between pressure and temperature and density. Stated pressure and temperature and density. Stated formally, it is known as the Ideal Gas Law and it formally, it is known as the Ideal Gas Law and it states:states:Pressure = Density X Temperature X some Pressure = Density X Temperature X some constantconstant

Scientists have calculated that given the mass of the Scientists have calculated that given the mass of the Sun and its tremendous gravitational pull inward, its Sun and its tremendous gravitational pull inward, its internal temperature must be about 15 million K to internal temperature must be about 15 million K to remain at equilibrium.remain at equilibrium.

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1.1. Define the followingDefine the following: The Photosphere, The : The Photosphere, The Chromosphere, The Corona, Radiative ZoneChromosphere, The Corona, Radiative Zoneand Convective Zoneand Convective Zone

2. 2. What is the diameter and mass of the Sun What is the diameter and mass of the Sun relative to Earth?relative to Earth?

3.3. What are granules and how do they form?What are granules and how do they form?4.4. What are the two layers of the Sun’s What are the two layers of the Sun’s

atmosphere?atmosphere?5.5. What is stellar equilibrium? Why is it What is stellar equilibrium? Why is it

important?important?6.6. According to the Ideal Gas law, what effects According to the Ideal Gas law, what effects

pressure?pressure?7.7. What is the cost to the Sun for maintaining What is the cost to the Sun for maintaining

its equilibrium?its equilibrium?8.8. What is a spicule?What is a spicule?

Powering the SunPowering the SunEnergy created by the Sun is Energy created by the Sun is eventually lost into outer space by eventually lost into outer space by heat and light. If the Sun did not heat and light. If the Sun did not replace this lost heat, the pressure replace this lost heat, the pressure pushing the Sun out would diminish pushing the Sun out would diminish until the Sun eventually collapsed until the Sun eventually collapsed under its own gravity.under its own gravity.

Powering the SunPowering the SunMany early astronomers believed Many early astronomers believed that the Sun burned conventional that the Sun burned conventional fuels such as coal. The supply of fuels such as coal. The supply of coalcoal would have been exhausted would have been exhausted after about 10,000 years.after about 10,000 years.

Powering the SunPowering the SunIn the late 1800’s, Lord Kelvin (English) In the late 1800’s, Lord Kelvin (English) and Hermann Helmholtz (German) and Hermann Helmholtz (German) independently proposed that the Sun independently proposed that the Sun was not at hydrostatic equilibrium, but was not at hydrostatic equilibrium, but was actually slowly collapsing.was actually slowly collapsing.

The Sun could onlyThe Sun could onlysustain itself forsustain itself forabout 10 millionabout 10 millionyears doing this.years doing this.

Powering the SunPowering the Sun

In 1899, T.C. Chamberlin suggested In 1899, T.C. Chamberlin suggested that subatomic energy might power that subatomic energy might power the stars, but could offer no the stars, but could offer no explanation as to how.explanation as to how.

Powering the SunPowering the Sun

It was not until 1905 that Albert It was not until 1905 that Albert Einstein proposed that energy might Einstein proposed that energy might actually come from mass with his actually come from mass with his equation E=mcequation E=mc22. .

Einstein’s EquationEinstein’s EquationE = mcE = mc22, where E is energy (joules), , where E is energy (joules), m is mass and c is the speed of light m is mass and c is the speed of light (3X10(3X1088 m/s m/s22). The amount of energy ). The amount of energy that is available from nuclear that is available from nuclear reactions is staggering. One gram of reactions is staggering. One gram of mass (one paper clip) could be mass (one paper clip) could be converted into 20 kilotons worth ofconverted into 20 kilotons worth of

energy. energy.

Follow Up WorkFollow Up Work

In 1919, Arthur S. Eddington showed In 1919, Arthur S. Eddington showed that converting hydrogen to helium that converting hydrogen to helium could provide enough energy to could provide enough energy to power stars including our Sun.power stars including our Sun.

Follow Up WorkFollow Up Work

Physicists Hans Bethe and Carl von Physicists Hans Bethe and Carl von Weizsacker proposed that the Sun Weizsacker proposed that the Sun produced its energy by the process produced its energy by the process of of nuclear fusionnuclear fusion..

Nuclear FusionNuclear FusionUnder normal conditions, hydrogen Under normal conditions, hydrogen nuclei repel each other due to similar nuclei repel each other due to similar electrical charges, but under electrical charges, but under conditions of extreme heat when conditions of extreme heat when these atoms collide their nuclei are these atoms collide their nuclei are driven extremelydriven extremely

close to each other.close to each other.

The Proton-Proton ChainThe Proton-Proton Chain Hydrogen fusion takes place in three Hydrogen fusion takes place in three

stages called the proton-proton stages called the proton-proton chain.chain.

The Proton-Proton ChainThe Proton-Proton ChainStage 1: Two hydrogen nuclei Stage 1: Two hydrogen nuclei

collide to form a hydrogen isotope collide to form a hydrogen isotope called called 22H. This process converts one H. This process converts one proton into a neutron and releases a proton into a neutron and releases a positron (epositron (e++) and a ) and a

neutrino (v).neutrino (v).

The Proton-Proton ChainThe Proton-Proton Chain Step 2: The Step 2: The 22H nucleus collides with H nucleus collides with a a 11H nucleus to make an isotope of H nucleus to make an isotope of 33He. This process releases energy in He. This process releases energy in the form of gamma rays (g).the form of gamma rays (g).

The Proton-Proton ChainThe Proton-Proton Chain Stage 3: Two Stage 3: Two 33He nuclei collide He nuclei collide together and fuse. This forms two together and fuse. This forms two separate particle types, separate particle types, 44He and two He and two 11H nuclei.H nuclei.

Searching for NeutrinosSearching for Neutrinos

During Stage 1 of the During Stage 1 of the proton-proton chain, proton-proton chain, we saw that the Sun we saw that the Sun generates neutrinos generates neutrinos in the fusion process. in the fusion process. Scientists have Scientists have searched for these searched for these neutrinos as neutrinos as evidence of the evidence of the fusion process in the fusion process in the Sun.Sun.

Searching for NeutrinosSearching for NeutrinosScientists calculated the amount of Scientists calculated the amount of neutrinos that they expected to be neutrinos that they expected to be generated by the Sun. Because generated by the Sun. Because neutrinos have so little mass, they neutrinos have so little mass, they can penetrate anything and are very can penetrate anything and are very hard to detect, like bullets shooting hard to detect, like bullets shooting through tissue paper.through tissue paper.


The first neutrinos detectors were built in The first neutrinos detectors were built in the late 1970’s, one in Japan and one in the late 1970’s, one in Japan and one in the United States. They were built deep the United States. They were built deep under ground for shielding fromunder ground for shielding from

cosmic rays.cosmic rays.

The detectors wereThe detectors were

filled with a solutionfilled with a solution

like heavy water.like heavy water.


When a neutrino When a neutrino passes through passes through the solution and the solution and collides with a collides with a neutron, it neutron, it creates a flash creates a flash of light from an of light from an electron. Light electron. Light sensors count sensors count the flashes.the flashes.

Searching for NeutrinosSearching for NeutrinosAnother thing that makes neutrinos Another thing that makes neutrinos hard to detect in that they come in hard to detect in that they come in three separate structures (called three separate structures (called , , and and -neutrinos). They transform -neutrinos). They transform themselves as the travel. Initially, themselves as the travel. Initially, scientist only detected a third of the scientist only detected a third of the neutrinos that they expected to find. neutrinos that they expected to find. They could only detect one of the They could only detect one of the types.types.

Summary of PointSummary of PointNot until very recently have we Not until very recently have we discovered evidence of how our Sun discovered evidence of how our Sun actually manufactures its energy. actually manufactures its energy. We didn’t even have a good guess We didn’t even have a good guess until the 1950’s. There is still a lot until the 1950’s. There is still a lot that we do not know about our star!that we do not know about our star!

Solar Magnetic ActivitySolar Magnetic Activity

The Sun’s magnetic field gives rises The Sun’s magnetic field gives rises to several solar phenomenon. These to several solar phenomenon. These includeinclude Solar prominences, Solar Solar prominences, Solar prominences, Sun spots and the prominences, Sun spots and the Earth’s aurora borealis.Earth’s aurora borealis.

Solar PhenomenonSolar PhenomenonSolar prominencesSolar prominences: : Are magnetic Are magnetic disturbances in the disturbances in the Sun’s atmosphere. Sun’s atmosphere. Gigantic plumes of hot Gigantic plumes of hot gas from the lower gas from the lower chromosphere jump chromosphere jump into the corona. into the corona. Prominences form as Prominences form as cooling gas trapped cooling gas trapped within the Sun’s within the Sun’s magnetic field. They magnetic field. They are usually seen arcing are usually seen arcing between sunspots. between sunspots.

Solar PhenomenonSolar PhenomenonSolar flaresSolar flares: These : These

are not well are not well understand but are understand but are thought to be the thought to be the Sun’s magnetic field Sun’s magnetic field being twisted by being twisted by hot, rising gas. The hot, rising gas. The fields can only be fields can only be twisted to much, twisted to much, before they readjust, before they readjust, forming a flare. Like forming a flare. Like a rubber-band toy. a rubber-band toy.

Solar PhenomenonSolar PhenomenonSun spotsSun spots: charged : charged particles are particles are attracted to the attracted to the Sun’s magnetic field. Sun’s magnetic field. These particles These particles spiral down the spiral down the magnetic field lines magnetic field lines and slow the ascent and slow the ascent of heat. This creates of heat. This creates colder areas on the colder areas on the surface. These cool, surface. These cool, black areas are black areas are known as sunspots.known as sunspots.

The Solar WindThe Solar WindAs the Sun burns, it releases heat As the Sun burns, it releases heat and energy in several forms. One of and energy in several forms. One of these forms is as charged particles. these forms is as charged particles. These particles streak across space These particles streak across space at the speed of light. They strike the at the speed of light. They strike the Earth’s magnetic field and glow in an Earth’s magnetic field and glow in an eerie phenomenon known as the eerie phenomenon known as the aurora borealisaurora borealis..

Solar PhenomenonSolar Phenomenon

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1.1. What is the source of the Sun’s energy?What is the source of the Sun’s energy?

2.2. Describe the three stages of the proton-Describe the three stages of the proton-proton chain.proton chain.

3.3. What is a solar prominence? How do What is a solar prominence? How do they occur?they occur?

4.4. What is a solar flare? How do they What is a solar flare? How do they occur?occur?

5.5. What is a sun spot? How do they occur?What is a sun spot? How do they occur?

6.6. What is a neutrino? Why are scientists What is a neutrino? Why are scientists looking for them so hard?looking for them so hard?

7.7. What is the aurora borealis?What is the aurora borealis?

Writing AssignmentWriting Assignment

Step 1: Within your group, discuss current Step 1: Within your group, discuss current issues in science. Focus on this question, issues in science. Focus on this question, “Is science destructive”? “Is science destructive”? Step 2: On a piece of paper, please write:Step 2: On a piece of paper, please write:

Paragraph 1: State three examples that Paragraph 1: State three examples that you discussed and tell why they are you discussed and tell why they are relevant to the question.relevant to the question.

Paragraph 2: Explain your personal Paragraph 2: Explain your personal position concerning the question, “Is position concerning the question, “Is science destructive”?science destructive”?

Solar CyclesSolar Cycles

We have lots of solar cycles.We have lots of solar cycles.

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