core he h burning shell main sequence evolution star brightens significantly (red giant)
TRANSCRIPT
Core
He
H burning shell
Main Sequence EvolutionHydrogen is depleted in the last fusion
zoneReaction rate fallsCore can no longer support its weight
core shrinksTemperature in the core increasesExtra energy produced to -
Begin fusion reaction in next core zoneBegin fusion reaction in next core zoneLift the envelopeStar brightens significantly (Red
Giant)
The Sun as a Red Giant
diameter = 1 AU
The Sun as a Main Sequence Star
diameter = 1/100 AU
H-R Diagram
Temperature
Lu
min
osi
ty
0.1R
1 R
10 R
100 R
ZAMS
Core is collapsing and heating up◦ He Fusion (Triple Alpha Process)
Threshold Temperature◦ 108 K = 100,000,000 K◦ Massive stars do this easily
Core is still ideal gas◦ Low mass stars (like the Sun) struggle
Core becomes degenerate
The ideal gas safety valve◦ Heat an ideal gas and it expands and cools◦ Cool an ideal gas and it contracts and heats up◦ Pressure Temperature
Degenerate electron gas◦ Electrons are forced to be very close together
and fill every energy state◦ Pressure and Temperature not related
Extra energy from He fusion causes the core to expand very little
Fusion energy raises the temperature of the core and takes place all over the core◦ He Flash◦ End of ascent up the Red Giant Branch
Eventually core does expand enough to become ideal again◦ Fusion now at much higher temperature
Star is quasi-stable◦ Envelope contracts (luminosity should )◦ Temperature increases (lum. should )◦ These two effects nearly offset
Horizontal Branch◦ RR Lyrae Variables
Periods of 0.05 to 1.2 days Amplitudes of 1 to 2 magnitude
All have M = -0.5 Measure m and calculate distance
Mag
nit
ud
e
Time
H-R Diagram
Temperature
Lu
min
osi
ty
ZAMS
Periods between 1 and 70 days Amplitudes of 0.1 to 2 mag
H burning shell
He burning shell
Carbon
Core
He is depleted in the last fusion zone Reaction rate falls Core can no longer support its weight
◦ core shrinks Temperature in the core increases
◦ Carbon fusion threshold 600 million K◦ Low Mass stars cannot reach this temperature
Envelope expands to supergiant
H-R Diagram
Temperature
Lu
min
osi
ty
ZAMS
Periods several hundred days Amplitudes several magnitudes
Mag
nit
ud
e
Time
Core is once again degenerate◦ He fusion in the shell becomes explosive
Send shocks of energy into the expanded envelope Recombination energy also drives envelope
out
The Ring Nebula
The Helix Nebula
Wings of a Butterfly Nebula
H-R Diagram
Temperature
Lu
min
osi
ty
ZAMS
Enhanced stellar wind in giant phases Planetary Nebula
Chandresakhar Limit◦ Maximum amount of mass that can be supported
by electron degeneracy◦ 1.4 M
Mass < 2.5 M
◦ He ignites in degenerate core (He flash)◦ Nuclear processing stops at He fusion
Mass between 2.5 and 8 M
◦ He ignites in a non-degenerate core No He flash required
◦ Nuclear processing stops at He fusion Mass between 8 and 10 M
◦ C fusion possible
Core was collapsing◦ Can never reach 600 million K for C fusion◦ Much of the original envelope has left in Planetary
Nebula◦ Material becomes degenerate◦ Electron Degeneracy Pressure halts collapse
Core must be < 1.4 M
Carbon
Thin atmosphere of H and He
Mass 1 M
Radius R
Sirius A◦ A1V, m = -1.46◦ T = 9550 K
Sirius B◦ m = 8.3◦ T = 25,000 K◦ gives R = 92%R
H-R Diagram
Temperature
Lu
min
osi
ty
ZAMS Animation