* Your assessment is very important for improving the workof artificial intelligence, which forms the content of this project
Download 30.2 PowerPoint Stellar Evolution
Observational astronomy wikipedia , lookup
Star of Bethlehem wikipedia , lookup
History of supernova observation wikipedia , lookup
Theoretical astronomy wikipedia , lookup
Dyson sphere wikipedia , lookup
Orion (constellation) wikipedia , lookup
Spitzer Space Telescope wikipedia , lookup
Formation and evolution of the Solar System wikipedia , lookup
Cassiopeia (constellation) wikipedia , lookup
History of Solar System formation and evolution hypotheses wikipedia , lookup
Auriga (constellation) wikipedia , lookup
Stellar classification wikipedia , lookup
Nebular hypothesis wikipedia , lookup
Timeline of astronomy wikipedia , lookup
Astronomical spectroscopy wikipedia , lookup
Corona Australis wikipedia , lookup
Perseus (constellation) wikipedia , lookup
Future of an expanding universe wikipedia , lookup
Corvus (constellation) wikipedia , lookup
Stellar kinematics wikipedia , lookup
Aquarius (constellation) wikipedia , lookup
Cygnus (constellation) wikipedia , lookup
Star formation wikipedia , lookup
Stellar evolution wikipedia , lookup
Stellar Evolution Stellar Evolution NGC 3603 circumstellar disks around young stars blue super-giant with its ring and bipolar outflow marks the end of the life cycle. progressing to aging, massive stars in a young starburst cluster Bok globules and giant gaseous pillars (evidence of embryonic stars), STAGE ONE Stars begin as a NEBULA - a dark cloud of gas and dust Made mostly of hydrogen and helium with small amounts of heavier elements Eagle Nebula M16 Horse Head Nebula Veil Nebula Trifid Nebula Thackeray's Globules in IC 2944 Omega or Swan Nebula Ghost Head Nebula The nebula begins to contract and gravitational attraction increases It continues shrinking and starts to spin. Eventually it forms a flat disk with a PROTOSTAR in the middle Planetary Disks Forming STAGE TWO - Main Sequence Longest part Energy is produced as fusion take place in the core of the star The energy from fusion balances the force of gravity and makes it a very stable stage Stage Three Happens when almost all of the hydrogen atoms have fused into helium atoms The core contracts due to the force of gravity This increases the temp and causes the helium to fuse into carbon This gives off a lot of energy and the star swells up to a giant or supergiant star Stage Four Helium fusion ends The star loses its outer gases and reveals a core An expanding shell of gases shed by this dying star forms a PLANETARY NEBULA Ant Nebula Helix Nebula Stingray nebula (Hen-1357), the youngest known planetary nebula. The "Spirograph" Nebula Cat’s Eye Nebula The star collapses inward and forms a hot dense core of matter called a WHITE DWARF Some white dwarfs may explode into a NOVA while they are cooling What about really BIG stars?? Stars with masses 10 100 times greater than the sun can produce a huge explosion called a SUPERNOVA SN1987A What happens after the explosion? The core may contract into a very small, dense ball of neutrons called a NEUTRON STAR – If it rotates it is called a PULSAR Really large stars contract with greater force and become a BLACK HOLE Centaurus A (Hidden Black Hole) Classifying Stars Hertzsprung-Russell (HR) Diagram Plots temp. v. luminosity Most stars are main sequence