1. Life cycle of the Stars Source: Dr. Jim Lochner, NASA/GSFC Presented in Tudhoe by Christos & Dave

2. Twinkle, Twinkle, Little Star...

3. How I Wonder What You Are... Stars have Different colors  Which indicate different temperatures The hotter a star is, the faster it burns its life away.

4. Stellar Nursery Space is filled with the stuff to make stars. http://imgsrc.hubblesite.or g/hu/db/1995/44/videos/a/f ormats/low_mpeg.mpg

5. Collapse to Protostar Stars begin with slow accumulation of gas and dust. Gravitational attraction of Clumps attracts more material. Contraction causes Temperature and Pressure to slowly increase.

6. Nuclear Fusion ! At 15 million degrees Celsius in the center of the star, fusion ignites ! 4 ( 1 H) --> 4 He + 2 e + + 2 neutrinos + energy Where does the energy come from ? Mass of four 1 H > Mass of one 4 He E = mc 2

7. A Balancing Act Energy released from nuclear fusion counter- acts inward force of gravity. Throughout its life, these two forces determine the stages of a star’s life.

8. The Beginning of the End: Red Giants After Hydrogen is exhausted in core... Energy released from nuclear fusion counter-acts inward force of gravity. Core collapses,  Kinetic energy of collapse converted into heat.  This heat expands the outer layers.

9. A Red Giant

10. A Red Giant You Know Meanwhile, as core collapses,  Increasing Temperature and Pressure...

11. More Fusion ! At 100 million degrees Celsius, Helium fuses: 3 ( 4 He) --> 12 C + energy (Be produced at an intermediate step) (Only 7.3 MeV produced) Energy sustains the expanded outer layers of the Red Giant

12. The end for solar type stars Planetary Nebulae After Helium exhausted, outer layers of star expelled http://oposite.stsci.edu/pubinfo/mpe g/OrionAnim.mpg

13. White dwarfs At center of Planetary Nebula lies a White Dwarf. Size of the Earth with Mass of the Sun “A ton per teaspoon” Inward force of gravity balanced by repulsive force of electrons. http://imgsrc.hubblesite.org/hu/db/2002/1 0/videos/b/formats/low_mpeg.mpghttp://imgsrc.hubblesite.org/hu/db/2002/1 0/videos/b/formats/low_mpeg.mpg

14. The End of the Line for Massive Stars Massive stars burn a succession of elements. Iron is the most stable element and cannot be fused further.  Instead of releasing energy, it uses energy.

15. Supernova ! http://im gsrc.hub blesite.or g/hu/db/ 2001/09/ videos/b/ formats/l ow_mpe g.mpg http://c handra.harvar d.edu/r esourc es/ani mation s/sn19 87a_lg. mov

16. What’s Left After the Supernova Neutron Star (If mass of core < 5 x Solar) Under collapse, protons and electrons combine to form neutrons. 10 Km across Black Hole (If mass of core > 5 x Solar) Not even compacted neutrons can support weight of very massive stars. http://chandra.harvard.edu/resources/animatio ns/black_hole_sm.mov http://chandra.harvard.edu/resources/animatio ns/black_hole_sm.mov

17. A whole new life: X-ray binaries In close binary systems, material flows from normal star to Neutron Star or Black Hole. X-rays emitted from disk of gas around Neutron Star/Black Hole. http://im gsrc.hub blesite.o rg/hu/db/ 2000/24/ videos/a/ formats/l ow_quic ktime.m ov

18. Black Holes - Up Close and Personal Jet (not always present) Accretion Disk Event Horizon Singularity (deep in center)

20. Reprise: the Life Cycle Sun-like Stars Massive Stars

21. Materials for Life Cycles of Stars This presentation, and other materials on the Life Cycles of Stars, are available on the Imagine the Universe! web site at: http://imagine.gsfc.nasa.gov/docs/teachers/lifecycles/stars.html