History of BeliefsHistory of Beliefs

Geocentricity TheoryGeocentricity Theory Greek Ptolemy’s theoryGreek Ptolemy’s theory The idea that the sun revolves around the The idea that the sun revolves around the

earthearth Supported by the ChurchSupported by the Church

Heliocentric TheoryHeliocentric Theory Earth revolves around the sunEarth revolves around the sun Considered by the Christian Church as heresy Considered by the Christian Church as heresy

until Copernicus (1543) and Galilei (1632)until Copernicus (1543) and Galilei (1632)

The SunThe SunThe Center of Our Solar SystemThe Center of Our Solar System

The Sun – Our Star AttractionThe Sun – Our Star Attraction (18 minutes)(18 minutes) Quiz at the endQuiz at the end

Facts about the SunFacts about the Sun

AgeAge 4.6 billion years old (half way through its life)4.6 billion years old (half way through its life)

Distance from EarthDistance from Earth 149,597,900 km149,597,900 km

MassMass 332,900 times Earth’s mass332,900 times Earth’s mass

VolumeVolume 1.3 million times the Earth’s volume1.3 million times the Earth’s volume

Rotation RateRotation Rate 25.38 Earth days (equator)25.38 Earth days (equator)

DiameterDiameter 109 time Earth’s diameter109 time Earth’s diameter 1,391,000 km1,391,000 km

Characteristics of the SunCharacteristics of the SunThe sun is about 72% hydrogen, 22% helium The sun is about 72% hydrogen, 22% helium and 1% of other elementsand 1% of other elements

At the core: Nuclear fusionAt the core: Nuclear fusion Every second, 600 million tons of hydrogen fuse Every second, 600 million tons of hydrogen fuse

to form 596 million tons of helium. to form 596 million tons of helium. The remaining 4 million tons of hydrogen is converted The remaining 4 million tons of hydrogen is converted into energy that makes the Sun shineinto energy that makes the Sun shine

It takes a million years for this energy to reach the It takes a million years for this energy to reach the Sun’s surface.Sun’s surface. Much of the energy is converted Much of the energy is converted from harmful gamma and x-rays in the form of from harmful gamma and x-rays in the form of visible light.visible light.

This light energy takes 8 minutes to reach This light energy takes 8 minutes to reach the Earththe Earth

Anatomy of the SunAnatomy of the Sun

1.1. CoreCore

2.2. Radiative ZoneRadiative Zone

3.3. Convection Convection ZoneZone

4.4. PhotospherePhotosphere

5.5. SunspotSunspot

6.6. Solar Solar ProminenceProminence

7.7. ChromosphereChromosphere

8.8. CoronaCorona

1.1. Core Core • The Sun’s nuclear furnace, where fusion reactions initially The Sun’s nuclear furnace, where fusion reactions initially

combine hydrogen atoms to produce helium yielding combine hydrogen atoms to produce helium yielding energy in the processenergy in the process

• Temperatures reach 15 million Temperatures reach 15 million ooC and pressure is C and pressure is enormousenormous

2.2. Radiative Zone (moving gases)Radiative Zone (moving gases)• Energy moves through a surrounding envelope of gas Energy moves through a surrounding envelope of gas

3.3. Convection ZoneConvection Zone• Big bubbles of hot gas transport energy to the surfaceBig bubbles of hot gas transport energy to the surface

4.4. PhotospherePhotosphere• The Sun’s visible surface. Due to its high temperature, it The Sun’s visible surface. Due to its high temperature, it

glows yellow.glows yellow.• It is made up of churning gases, it is not a solid surfaceIt is made up of churning gases, it is not a solid surface

5. 5. Sunspot (Active Region)Sunspot (Active Region)• A magnetic storm on the Sun’s surface that is generally cooler then A magnetic storm on the Sun’s surface that is generally cooler then

the photosphere around themthe photosphere around them• Sunspots always occur in pairs Sunspots always occur in pairs • Sunspots are intense magnetic fields that break the Sun’s surfaceSunspots are intense magnetic fields that break the Sun’s surface

• These field lines break through one sunspot and reenter into anotherThese field lines break through one sunspot and reenter into another

• These are 1000 to 20,000 km in diameterThese are 1000 to 20,000 km in diameter• These frequently generate solar flaresThese frequently generate solar flares

Solar Flare:Solar Flare:• A solar flare is an eruption of hot gases from the inner atmosphere A solar flare is an eruption of hot gases from the inner atmosphere

of the Sun’s surface. of the Sun’s surface. • It travels very quickly and last for only minutes.It travels very quickly and last for only minutes.• ““Fountains of hot gases” that travel outward from the Fountains of hot gases” that travel outward from the

chromosphere through the coronachromosphere through the corona• The charged particles from a solar flare affect us in two main ways: The charged particles from a solar flare affect us in two main ways:

They produce the beautiful auroras (the particles / energy interact They produce the beautiful auroras (the particles / energy interact with the Earth’s poles), and they cause problems in communication with the Earth’s poles), and they cause problems in communication systems.systems.

• Note: The number of sunspots and solar flares peaks every 11 years when Note: The number of sunspots and solar flares peaks every 11 years when the magnetic field of Sun flips over.the magnetic field of Sun flips over.

http://www.space.com/27834-monster-sunspot-solar-flares-video.html

6.6. Solar ProminenceSolar Prominence• A solar prominence is a burst of a huge sheet of gases, A solar prominence is a burst of a huge sheet of gases,

also from the inner atmosphere. It is much larger than a also from the inner atmosphere. It is much larger than a flare and may last for days or even weeks.flare and may last for days or even weeks.

• The huge sheet of gases lines itself up along the The huge sheet of gases lines itself up along the magnetic field created between the pairs of sunspotsmagnetic field created between the pairs of sunspots

• They can go as far as 50,000 km or more above the They can go as far as 50,000 km or more above the Sun’s surfaceSun’s surface

7.7. ChromosphereChromosphere• The inner atmosphereThe inner atmosphere

8.8. CoronaCorona• The Sun’s outer atmosphere where gas temperatures The Sun’s outer atmosphere where gas temperatures

reach over 1 million reach over 1 million ooCC

Sun’s RotationSun’s RotationThe Sun rotates on an axisThe Sun rotates on an axisThe Sun’s interior rotates at a different rate then The Sun’s interior rotates at a different rate then than outer surfacethan outer surface The The interiorinterior (the core and radiative zone) are believed to (the core and radiative zone) are believed to

rotate as a solidrotate as a solid The The outer partsouter parts (the convective zone and out) are believed (the convective zone and out) are believed

to to rotate at different rates that vary with latituderotate at different rates that vary with latitude The result: The outer surface does not rotate at the same The result: The outer surface does not rotate at the same

rate. rate. As latitude increases, the rate of rotation slows As latitude increases, the rate of rotation slows downdown..

At the equator (middle) – rotation rate is 28 (25) daysAt the equator (middle) – rotation rate is 28 (25) daysAt the poles – rotation rate is 37 (36) daysAt the poles – rotation rate is 37 (36) days

Sunspots are a great way to see the movementSunspots are a great way to see the movement

Activity 1 and 2Activity 1 and 2

Complete each of the following activities Complete each of the following activities on the Solar graph paper provided.on the Solar graph paper provided.

Answer questions in complete sentences Answer questions in complete sentences at the bottom of the solar graph paper (3).at the bottom of the solar graph paper (3).

Activity 1: Plotting Sunspots Activity 1: Plotting Sunspots

Plotting Sunspots ActivityPlotting Sunspots Activity Using the Solar Graph paper, plot the points Using the Solar Graph paper, plot the points

given in the table. Each represent a sunspot given in the table. Each represent a sunspot locationlocation

Label each plot with the corresponding Label each plot with the corresponding numbernumber

Question 1: Question 1: Where do sunspots appear to be occurring on Where do sunspots appear to be occurring on

the Sun? Give the value in degrees.the Sun? Give the value in degrees.

Activity 2: Tracking an Active RegionActivity 2: Tracking an Active Region

Tracking a SunspotTracking a Sunspot Using the Solar Graph paper, plot the points given in Using the Solar Graph paper, plot the points given in

the table. the table. Label each plot with the corresponding date Label each plot with the corresponding date

Question 2: Question 2: What pattern does the movement of AR7220 have? What pattern does the movement of AR7220 have?

How far does it move each day?How far does it move each day?

Question 3: Question 3: The first day AR7216 was seen it was located at The first day AR7216 was seen it was located at

N13E75. After 12 days, where would you expect it N13E75. After 12 days, where would you expect it be?be?

Activity 3: Historical Data Sunspot LocationActivity 3: Historical Data Sunspot Location

Using the data provided, graph the Using the data provided, graph the number of sunspots from the 1700’s to number of sunspots from the 1700’s to 2001. Look for patterns – does it match 2001. Look for patterns – does it match the research?the research?

Hand-inHand-in Properly labeled graph.Properly labeled graph. Questions answered in full sentences.Questions answered in full sentences.

Sunspots of Our SunSunspots of Our Sun

Approximately 11 year cycleApproximately 11 year cycle Discovered in 1843 by Samuel Heinrich SchwabeDiscovered in 1843 by Samuel Heinrich Schwabe

Solar maximum Solar maximum peak in number of sunspotspeak in number of sunspots Often high number of solar flares during this Often high number of solar flares during this

timetime

Solar minimum Solar minimum low number of sunspotslow number of sunspots

Fate of Our SunFate of Our Sun

https://www.windows.ucar.edu/tour/link=/sun/fate.html

Eventually our Sun will …Eventually our Sun will …Deplete its supply of hydrogenDeplete its supply of hydrogen

the core will shrink the core will shrink temperatures will climbtemperatures will climb And it will begin to burn helium which in turn will form heavier elementsAnd it will begin to burn helium which in turn will form heavier elements

Form a red giant as the surface will puff up like a balloon, growing Form a red giant as the surface will puff up like a balloon, growing cooler, reddercooler, redderIt will eat up all of the inner planetsIt will eat up all of the inner planetsNot be able to release enough energy to form new elements and Not be able to release enough energy to form new elements and hence, fusion will stophence, fusion will stopShed its outer layers, surrounding itself with a planetary nebula (a Shed its outer layers, surrounding itself with a planetary nebula (a colorful gas bubble)colorful gas bubble)This nebula will dissipate distributing various gases – carbon, This nebula will dissipate distributing various gases – carbon, oxygen, etc.. - throughout the solar systemoxygen, etc.. - throughout the solar systemOnly have a collapsed core = 60 percent of the Sun’s mass (the size Only have a collapsed core = 60 percent of the Sun’s mass (the size of earth) of earth) Be a dead remnant, White dwarf, that will eventually cool and fade Be a dead remnant, White dwarf, that will eventually cool and fade from sightfrom sight

Note that not all stars die this wayNote that not all stars die this way

The fate of a star is dependent on its massThe fate of a star is dependent on its mass

Average stars end as the Sun willAverage stars end as the Sun will

Larger stars will end in a massive Larger stars will end in a massive explosion – a supernovaexplosion – a supernova

Massive stars (10 times that of the Sun), Massive stars (10 times that of the Sun), simply collapse into their inner core simply collapse into their inner core forming a black holeforming a black hole

Crab NebulaCrab Nebula5 minutes5 minutes

Videos\The_Formation_and_Destruction_of_Stars.asf