1. Type I Supernova Bevi Wallenstein

2. What does the word mean?  Nova means "new" in Latin, which is referring to very vivid new star in the sky  The prefix super, lets us know that we are talking about supernova, not ordinary novae (which is a star increasing in brightness, but not as much, and by different means)  The word supernova was first used in print in 1926  Nova means "new" in Latin, which is referring to very vivid new star in the sky  The prefix super, lets us know that we are talking about supernova, not ordinary novae (which is a star increasing in brightness, but not as much, and by different means)  The word supernova was first used in print in 1926

3. What is a Supernova?  A supernova occurs at the end of a stars lifetime  The stars nuclear fuel is worn out and it is not supported by the release of nuclear energy any longer  During this short interval, a supernova can radiate as much energy as the Sun could emit over its life span  A supernova occurs at the end of a stars lifetime  The stars nuclear fuel is worn out and it is not supported by the release of nuclear energy any longer  During this short interval, a supernova can radiate as much energy as the Sun could emit over its life span

4. What does a Supernova look like?  The explosion is extremely luminous and sends out bursts of radiation that often briefly outshine an entire galaxy  Fades from view over several weeks or months  The explosion is extremely luminous and sends out bursts of radiation that often briefly outshine an entire galaxy  Fades from view over several weeks or months

5. What we can see  Supernovas can be seen in other galaxies  Quite rare in our galaxy  The last supernova in our galaxy was Kepler's star in 1604  A famous remnant of one was the Crab Nebula which exploded in 1054  Supernovas can be seen in other galaxies  Quite rare in our galaxy  The last supernova in our galaxy was Kepler's star in 1604  A famous remnant of one was the Crab Nebula which exploded in 1054

6. The difference between type I and type II  Type I: The explosion comes from sudden fusion on its surface Type II: The explosion comes from collapse of the core  Type I: The star is completely destroyed Type II: The core remains unbroken as a neutron star or black hole  Type I: The explosion comes from sudden fusion on its surface Type II: The explosion comes from collapse of the core  Type I: The star is completely destroyed Type II: The core remains unbroken as a neutron star or black hole

7. The difference between type I and type II (CONTINUED)  Type I: The mass and brightness is the consistent for each one Type II: The mass and brightness vary over a wide range  Type I: Occurs in a white dwarf Type II: Occurs in a giant star just after the main sequence but before becoming a stellar remnant  Type I: The mass and brightness is the consistent for each one Type II: The mass and brightness vary over a wide range  Type I: Occurs in a white dwarf Type II: Occurs in a giant star just after the main sequence but before becoming a stellar remnant

8. Type Ia, Ib, and Ic  Type Ia: Lacks hydrogen lines  Type Ib: Non-ionized helium lines  Type Ic: Weak or no helium lines  Type Ia: Lacks hydrogen lines  Type Ib: Non-ionized helium lines  Type Ic: Weak or no helium lines

9. Other facts  Solitary stars with a mass lower then 9 times the sun, turn into white dwarfs stars without ever becoming supernovae  The growing shock waves from supernova explosions can set off the creation of new stars  Solitary stars with a mass lower then 9 times the sun, turn into white dwarfs stars without ever becoming supernovae  The growing shock waves from supernova explosions can set off the creation of new stars

10. Works Cited  http://imagine.gsfc.nasa.gov/docs/teachers/lesso ns/xray_spectra/background-lifecycles.html http://imagine.gsfc.nasa.gov/docs/teachers/lesso ns/xray_spectra/background-lifecycles.html  http://www.flickr.com/photos/smithsonian/29414 98208/ http://www.flickr.com/photos/smithsonian/29414 98208/  http://heasarc.gsfc.nasa.gov/docs/snr.html http://heasarc.gsfc.nasa.gov/docs/snr.html  http://en.wikipedia.org/wiki/Supernova#Type_Ia http://en.wikipedia.org/wiki/Supernova#Type_Ia  http://imagine.gsfc.nasa.gov/docs/teachers/lesso ns/xray_spectra/background-lifecycles.html http://imagine.gsfc.nasa.gov/docs/teachers/lesso ns/xray_spectra/background-lifecycles.html  http://www.flickr.com/photos/smithsonian/29414 98208/ http://www.flickr.com/photos/smithsonian/29414 98208/  http://heasarc.gsfc.nasa.gov/docs/snr.html http://heasarc.gsfc.nasa.gov/docs/snr.html  http://en.wikipedia.org/wiki/Supernova#Type_Ia http://en.wikipedia.org/wiki/Supernova#Type_Ia