CAPS Grade 9 Stars module. Covering the life, birth and death of stars. Guided by the unit covered in DocScientia

1. StarsTwitter: @LilyKotze

2. large balls of gas
Stars are
that radiate light.

3. Large quantities of energy come from hydrogen
nuclei colliding to form a Helium nucleus.
This is called nuclear fusion.
Stars exist for a
limited time.

4. Stars form inside nebulae, which are pulled
together by gravity.
Nebulae: Large clouds of dust and gas.

5. born,When a star is
it is relatively cold.
As gases are compressed
due to gravity, temperature
increases.
When temperatures
are high enough,
nuclear fusion
reactions occur.
Hydrogen nuclei join up.
Large amounts of
energy are radiated
into space.
changes

6. In the early phases, these stars are known as
protostars. They are often known as brown
dwarfs.

7. Stars change in appearance over a very
long time.
Stars that look blue are hotter and usually
younger than stars that look red.
Our sun is about halfway through its life cycle.
It is a medium-sized yellow star.
Towards the end of the life of a sun-like star, it
will swell up to form .
Life

10. A is a massive star:
• Small to medium size mass.
• Later stage of life
• Nuclear fusion: in the shell, on the outside of
the core.
• The gases in the core are extremely
compressed.
• The outer atmosphere is swollen and sparse.
• The tail of the star is enormous.
• The surface temperature is low.

12. Death
Some time to the end, the nuclear reactions
run out of fuel.
For stars like our sun, the core contracts to
become a .
The outer gases of the star are ejected into
space.
They become an expanding cloud around the
white dwarf.

13. Planetary nebulae are lit up by their central
white dwarf.
White dwarfs that are isolated can, cool down
and become dimmer until they eventually are
invisible.
They are then called black dwarfs.
The heavy elements that are created by stars
are the start of the next stars.

17. Title: https://farm6.staticflickr.com/5442/9076385353_8a75f19806_o_d.jpg
Slide 3: http://spaceplace.nasa.gov/review/story-superstar/page13.png ; fusion:
http://fusionforenergy.europa.eu/understandingfusion/whatisfusion/Whatisfusion_2.jpg ;
joke:
http://mrdclassified.weebly.com/uploads/1/3/5/0/13508015/627364475_orig.jpg?164
Slide 4: http://sci.esa.int/science-e-
media/img/5a/Herschel_Hubble_Crab_Nebula_highres.jpg
Slide 5: Hydrogen: http://theodoregray.com/PeriodicTable/Samples/001.x3/s15s.JPG ;
Helium: http://periodictable.com/Samples/002.6/s13.JPG
Slide 6: http://exoplanet.as.arizona.edu/~lclose/teaching/a202/disk-lr.jpg
Slide 8: http://whyfiles.org/wp-content/uploads/2013/06/sun_diagram.jpg
Slide 9 : http://kepler.nasa.gov/files/mws/kasc3.jpg
Slide 11: http://www.nasa.gov/images/content/49887main_stellar2.jpg
Slide 13: Helix nebula:
https://upload.wikimedia.org/wikipedia/commons/b/b1/NGC7293_(2004).jpg
Slide 14: http://scienceblogs.com/startswithabang/files/2011/09/star_dwarf_5.jpeg
Slide 15: http://www.einstein-
online.info/images/spotlights/redshift_white_dwarfsI/wd_comp.gif
Slide 16:
http://headwatersacademyearthsci.weebly.com/uploads/2/1/9/1/21919828/411679_orig.
jpg