Chapter I 0

The Sun,  our very own
star.
PCINS aft/7e Sun

Corona — Chromosphe Photosphere

Forms the sun’s re _ thin region — the part of the

outer atmosphere be...
‘ / 
k E nergiii* p1'0c1’uCii0n in the S1117
t it , 

 

° Energy from gravity is not
enough to power the sun, 
because if...
/ 
% N llC]€cIIt' F zzsion in the S 2m
1'’ V. 

° Is Where 2 or more low mass
nuclei join together. 

° Normally Hydrogen ...
__/ 
 F 2151' on
I . 

 

° Due to high heat and high
pressure,  hydrogen nuclei have
enough energy to over come the
repul...
5 Ci enfis IS
 
Einstein showed matter and
energy are interchangeable. 

° The Formula used to show the
relationship b/ t ...
Everything should be as simole as

" uossiblre.  but not simnler
E =  MC squared. ..
 
° Energy =  mass X square the
speed of light.
How it all works. ..

  
  

° Energy is made in the core of
the sun. 

° Energy then passes through a
dense region called...
° Hot gases are carried to the sun’s

visible surface from a region called
the convective zone. 

° Energy leaves the sun ...
° Some areas of the photosphere
become cooler than surrounding
areas b/ c the sun’s magnetic field
tends to slow down activ...
“St()rI72.s' on the S1117 

 

° The constant flow of magnetic
fields from the sun is called solar
wind. 

' Cooler,  darker...
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Chapter 10section 3

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Chapter 10section 3

  1. 1. Chapter I 0 The Sun, our very own star.
  2. 2. PCINS aft/7e Sun Corona — Chromosphe Photosphere Forms the sun’s re _ thin region — the part of the outer atmosphere below the corona sun we can see from the Earth Convection Radiative Core — center Zone — region Zone — very Of the Sun Where where the gases dense region the sun’s energy eireulate is produced.
  3. 3. ‘ / k E nergiii* p1'0c1’uCii0n in the S1117 t it , ° Energy from gravity is not enough to power the sun, because if all of the sun’s gravitational energy were released, the sun would last for only 45 million years.
  4. 4. / % N llC]€cIIt' F zzsion in the S 2m 1'’ V. ° Is Where 2 or more low mass nuclei join together. ° Normally Hydrogen nuclei would repel each other b/ c they have the same charge (+)
  5. 5. __/ F 2151' on I . ° Due to high heat and high pressure, hydrogen nuclei have enough energy to over come the repulsion and fuse together into helium. (see pic. Pg 289, or online videofication)
  6. 6. 5 Ci enfis IS Einstein showed matter and energy are interchangeable. ° The Formula used to show the relationship b/ t matter and energy is. . .
  7. 7. Everything should be as simole as " uossiblre. but not simnler
  8. 8. E = MC squared. .. ° Energy = mass X square the speed of light.
  9. 9. How it all works. .. ° Energy is made in the core of the sun. ° Energy then passes through a dense region called the radiative zone.
  10. 10. ° Hot gases are carried to the sun’s visible surface from a region called the convective zone. ° Energy leaves the sun as light from a region called the photosphere.
  11. 11. ° Some areas of the photosphere become cooler than surrounding areas b/ c the sun’s magnetic field tends to slow down activity in the convective zone. When this happens, parts of the photosphere become cooler than the rest of it.
  12. 12. “St()rI72.s' on the S1117 ° The constant flow of magnetic fields from the sun is called solar wind. ' Cooler, darker areas of the photosphere of the sun are called sunspots. A sunspot cycle lasts about 11 years.

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