slide 1 stellar evolution m ~4 p r o t o s t a r m a i n s e q u e n c e d g i a n t planetary...
TRANSCRIPT
Slide 1
Stellar EvolutionStellar Evolution
M<0.08 .08<M<0.4 0.4<M<1.4 1.4<M<~4 M>~4
P R O T O S T A R M a i n S e q u e n c e
D G I A N T
Planetary Supernova Nebula
W h i t e D w a r f
B r o w n D w a r f Neutron Star OR
Black Hole
M A I N S E Q U E N C ER E D G I A N T
W H I T E D W A R F
B R O W N D W A R F
M is mass of the star in units of mass of the Sun M
Slide 2
Protostar
• Gravitational contraction of space matter.
• Source of energy is gravity.
• Starts typically with a size of several light years. (1 ly ~ 1013 km.)
• Many gravitational contraction points
• When protostar core gets hot enough to start nuclear fusion, a normal star is born.
Slide 3
Main Sequence Stars
• Source of energy is nuclear fusion
• 4 H He + energy as helium mass is less than 4H by 0.7%.
• Star very stable with gravity pulling in and heat energy pushing out.
• The more massive the star, the faster it uses hydrogen.
Slide 4
Red Giant Stars
• After core hydrogen is depleted, core contracts, heats up more and when temperature reaches 100,000,000ºK, 3He C + energy fusion starts.
• Outside of the core the temperature is now over 1,000,000ºK and there is plenty of hydrogen and 4HHe + energy production starts.
• Now more energy is produced, so star expands to about 100 times original size.
• Sun will become a red giant in about 5 billion years, swell about 100 times in diameter and absorb Mercury, Venus and Earth.
Slide 8
Death of Stars
• Depends on mass.
• For stars < 4M after all nuclear fusion has stopped, the star collapses into white dwarf, the size of Earth.
• If mass > 1.4 M during collapse the outer layers are expelled and become planetary nebula (nothing to do with planets).
Slide 15
Supernova
• For Red Giants with mass > 4 M becomes iron. Iron cannot fuse to higher mass elements and fusion stops and star starts collapsing.
• During the collapse all the outer layers become extremely hot and nuclear fusion starts everywhere except in the core.
• The star explodes into a supernova and the core squeezes into a neutron star or black hole.
• During supernova the star brightens 1010 to 1011 times. Often outshines the whole galaxy.
Slide 19 Fig. 13-13, p.268
Tarantula Nebula in Large Magellanic Cloud (a neighboring galaxy)and 1987A supernova
Before and after February 24, 1987
Slide 20
Supernova• Rise in brightness very rapid ~ 1 day.• Drop in intensity ~ 1 year.• On the average 2 supernova per century per galaxy.• Last supernova observes in our galaxy was about 400
years ago.• Last supernova observed in “naked eye” was in 1987
in Large Magellanic Cloud galaxy.• Many supernovae are observed each year in far away
galaxies.
Slide 23
Supernova remnants
• 80% to 90% of the star blows out.• Core squeezes into a neutron star or black
hole.• Neutron star is the size of a city, spins very
rapidly and emits pulses that gave the original name of pulsars.
• If the mass of neutron star is too large, it becomes a black hole.
Slide 33 Fig. 13-26, p.275
Binary pulsarperihelionshift due togravity wavesas predictedby Einsteingeneral theoryof gravity
4º per year.