STELLAR EVOLUTION

SINGLE CLUSTER – TURNOFF MASS – AGE OF CLUSTER

All stars follow the same basic series of steps in their lives: Gas Cloud  Main Sequence  Red Giant  (Planetary Nebula or Supernova)  Remnant. How long a star lasts in each stage, whether a planetary nebula forms or a spectacular supernova occurs, and what type of remnant will form depends on the initial mass of the star. Evolution of stars depends on their mass (at start of fusion only- Zero Main Sequence) with a tiny bit of dependence on chemical composition. (why ?)- Type I(young-our Sun) and type II (old) stars

MOLECULAR CLOUDS - STAR NURSERIES - ORION

H II Regions 4 UV STARS Dark Regions Star Nurseries Need IR to see Space Telescope - Visible

IR picture Space Telescope – Molecular Clouds in ORION

Eagle Nebula

Winds from Protostars

SHELL BURNING RED GIANT

SUPER-GIANT ORION CONSTELLATION

STAR BECOMES A COSMIC OGNION STAYS IN ASYMPTOTIC GIANT BRANCH NUCLEOSYNTHESIS Shell Burning

Neutron Star – Neutron Degeneracy Pressure

SN 1987

DEGENERACY PRESSURE Heisenberg’s Uncertainty Principle Upper limit for  v=c P D < mc 2 /(  x) 3