OBJ: SWBAT identify parts of the sun and their characteristics

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OBJ SWBAT identify parts of the sun and their
characteristics

• Drill The sun contains approximately how much
  of the material within the solar system?

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The Suns Energy, continued
Section 1 Structure of the Sun
Chapter 29

• Nuclear Fusion
• nuclear fusion the process by which nuclei of
  small atoms combine to form a new, more massive
  nucleus the process releases energy
• Nuclear fusion occurs inside the sun. Nuclei of
  hydrogen atoms are the primary fuel for the suns
  fusion.
• Nuclear fusion produces most of the suns energy
  and consists of three steps.

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• The Final Product
• One of the final products of the fusion of
  hydrogen in the sun is always a helium nucleus.
• The helium nucleus has about 0.7 less mass than
  the hydrogen nuclei that combined to form it do.
  The lost mass is converted into energy during the
  series of fusion reactions that forms helium.
• The energy released during the three steps of
  nuclear fusion causes the sun to shine and gives
  the sun its high temperature.

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The Suns Interior
Section 1 Structure of the Sun
Chapter 29

• The Core
• Careful studies of motions on the suns surface
  have supplied more detail about what is happening
  inside the sun. The parts of the sun include the
  core, the radiative zone, and the convective
  zone.
• At the center of the sun is the core. The core
  makes up 25 of the suns total diameter of
  1,390,000 km. The temperature of the core is
  about 15,000,000 kmºC.
• The core is made up entirely of ionized gas, and
  is 10 times as dense as iron.

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Chapter 29

• The Radiative Zone
• radiative zone the zone of the suns interior
  that is between the core and the convective zone
  and in which energy moves by radiation
• The radiative zone of the sun surrounds the core.
  
• The temperature of the radiative zone ranges from
  about 2,000,000ºC to 7,000,000 ºC .
• In the radiative zone, energy moves outward in
  the form of electromagnetic waves, or radiation.

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Section 1 Structure of the Sun
Chapter 29

• The Convective Zone
• Convective zone the region of the suns interior
  that is between the radiative zone and the
  photosphere and in which energy is carried upward
  by convection
• The convective zone surrounds the radiative zone.
  The temperature of the convective zone is about
  2,000,000ºC.
• Convection is the transfer of energy by moving
  matter.

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The Suns Interior, continued
Section 1 Structure of the Sun
Chapter 29

• The diagram below shows the layers of the sun.

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The Suns Atmosphere
Section 1 Structure of the Sun
Chapter 29

• The suns atmosphere surrounds the convective
  zone of the suns core.
• Because the sun is made of gases, the term
  atmosphere refers to the uppermost region of
  solar gases.
• The suns atmosphere has three layers the
  photosphere, the chromosphere, and the corona.

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Section 1 Structure of the Sun
Chapter 29

• The Photosphere
• photosphere the visible surface of the sun
• Photosphere means sphere of light. The
  photosphere of the sun is the innermost layer of
  the suns atmosphere.
• The photosphere is made of gases that have risen
  from the convective zone. The temperature in the
  photosphere is about 6,000ºC.
• Much of the energy given off from the photosphere
  is in the form of visible light.

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Section 1 Structure of the Sun
Chapter 29

• Reading Check
• What layers make up the suns atmosphere?
• The suns atmosphere consists of the photosphere,
  the chromosphere, and the corona.

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Section 1 Structure of the Sun
Chapter 29

• The Chromosphere
• chromosphere the thin layer of the sun that is
  just above the photosphere and that glows a
  reddish color during eclipses
• The chromosphere lies just above the photosphere.
  The chromospheres temperature ranges from
  4,000C to 50,000 C.
• The gases of the chromosphere move away from the
  photosphere, forming narrow jets of hot gas that
  shoot outward and then fade away within a few
  minutes.

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Section 1 Structure of the Sun
Chapter 29

• The Suns Outer Parts
• corona the outermost layer of the suns
  atmosphere
• The corona is a huge region of gas that has a
  temperature above 1,000,000ºC.
• As the corona expands, electrons and electrically
  charged particles called ions stream out into
  space.
• These particles make up solar wind, which flows
  outward from the sun to the rest of the solar
  system.

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The Suns Atmosphere
Chapter 29
Section 1 Structure of the Sun
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Your Mission Make a graphic organizer showing
the layers of the sun and its atmosphere. Be
sure to include- Layer name-TemperatureImporta
nt features ex) fusion
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Identify the sun Layers!!
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Objectives
Section 2 Solar Activity
Chapter 29

• Explain how sunspots are related to powerful
  magnetic fields on the sun.
• Compare prominences, solar flares, and coronal
  mass ejections.
• Describe how the solar wind can cause auroras on
  Earth.

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Sunspots
Section 2 Solar Activity
Chapter 29

• sunspot a dark area of the photosphere of the
  sun that is cooler than the surrounding areas and
  that has a strong magnetic field.

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• Sunspots
• The movements of gases within the suns
  convective zone and the movements caused by the
  suns rotation produce magnetic fields.
• These magnetic fields cause convection to slow in
  parts of the convective zone.

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Sunspots
Section 2 Solar Activity
Chapter 29

• Slower convection causes a decrease in the amount
  of gas that is transferring energy from the core
  of the sun to these regions of the photosphere.
• Because less energy is being transferred, these
  regions of the photosphere are considerably
  cooler than surrounding regions, and form areas
  fo the sun that appear darker than their
  surrounding regions.
• These, cooler, darker areas are called sunspots.

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The Sunspot Cycle
Section 2 Solar Activity
Chapter 29

• Observations of sunspots have shown that the sun
  rotates.
• The numbers and positions of sunspots vary in a
  cycle that lasts about 11 years.

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• Sunspots initially appear in groups about midway
  between the suns equator and poles. The number
  of sunspots increases over the next few until it
  reaches a peak of 100 or more sunspots.
• After the peak, the number of sunspots begins to
  decrease until it reaches a minimum.

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Solar Ejections
Section 2 Solar Activity
Chapter 29

• Other solar activities are affected by the
  sunspot cycle, such as the solar-activity cycle.
• The solar-activity cycle is caused by the
  changing solar magnetic field.

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• This cycle is characterized by increases and
  decreases in various types of solar activity,
  including solar ejections.
• Solar ejections are events in which the sun emits
  atomic particles.

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• This cycle is characterized by increases and
  decreases in various types of solar activity,
  including solar ejections.
• Solar ejections are events in which the sun emits
  atomic particles.

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• Solar ejections include prominences, solar
  flares, and coronal mass ejections.

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Section 2 Solar Activity
Chapter 29

• Prominences
• prominence a loop of relatively cool,
  incandescent gas that extends above the
  photosphere.

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• Prominences are huge arches of glowing gases that
  follow the curved lines of the magnetic force
  from a region of one magnetic force to a region
  of the opposite magnetic polarity.

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Section 2 Solar Activity
Chapter 29

• Solar Flares
• solar flare an explosive release of energy that
  comes from the sun and that is associated with
  magnetic disturbances on the suns surface

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Section 2 Solar Activity
Chapter 29

• Coronal Mass Ejections
• coronal mass ejection a part of coronal gas that
  is thrown into space from the sun
• Some of the particles from a solar flare escape
  into space, increasing the strength of the solar
  wind.

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• Particles also escape as coronal mass ejections.
  The particles in the ejection can cause
  disturbances to Earths magnetic field.
• These disturbances have been known to interfere
  with radio communications, satellites, and even
  cause blackouts.

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Solar Ejections, continued
Section 2 Solar Activity
Chapter 29

• Reading Check
• How do coronal mass ejections affect
  communications on Earth?
• Coronal mass ejections generate sudden
  disturbances in Earths magnetic field. The
  high-energy particles that circulate during these
  storms can damage satellites, cause power
  blackouts, and interfere with radio
  communications.

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Auroras
Section 2 Solar Activity
Chapter 29

• aurora colored light produced by charged
  particles from the solar wind and from the
  magnetosphere that react with and excite the
  oxygen and nitrogen of Earths upper atmosphere
  usually seen in the sky near Earths magnetic
  poles.
• Auroras are the result of the interaction between
  the solar wind and Earths magnetosphere.
• Auroras are usually seen close to Earths
  magnetic poles because electrically charged
  particles are guided toward earths magnetic
  poles by Earths magnetosphere.

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Objective SWBAT graph sunspot data IOT
interpret and apply concepts of Solar Cycles

• Drill Blast from the past.
• What kind of clouds are dominating the weather
  this morning.. (hint it was sprinkling)

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• Today you will graph sunspot data for a 30yr
  span.
• Be sure to draw your scale appropriately IOT use
  as much of the graph paper as possible.
• You will need a calculator

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Objective SWBAT graph sunspot data IOT
interpret and apply concepts of Solar Cycles

• Drill Where does the energy come from that
  fuels the suns activity? Describe the process.

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• Anouncments
• Quiz tomorrow!! Will cover sun layers, solar
  ejections, sunspots, and solar cycles.
• Today Complete your sunspot cycle graph and
  questions.
• -You may want to extend your graph to answer
  the conclusion questions.
• - You will need to analyze the data provided
  IOT successfully answer the questions. (used a
  highlighter to highlight particular data of
  interest. This will help the data stand out
• - If you finish early, complete the Chapter 29
  review 1-39. You may omit 32. This will be
  due tomorrow morning.