Download presentation
Presentation is loading. Please wait.
1
19. Main-Sequence Stars & Later
End of core hydrogen fusion creates a red giant Core helium fusion in red giants Star clusters & red giant evolution Star evolution produces two star populations Many mature stars pulsate Mass transfer can affect close binary stars
2
Core Hydrogen Fusion Termination
Critical concepts Zero-age main-sequence stars ZAMS On-going hydrogen fusion begins within the core Hydrostatic & thermal equilibrium are established Main-sequence lifetime The total time hydrogen fusion continues within the core Chemical changes in a star’s core Initial mass ~ 74% H ~ 25% He ~ 1% “metals” Atoms ~ 91 H ~ 8 He ~ 1 “metals” Final mass ~ 0% H ~ 99% He ~ 1% “metals” Atoms ~ 0 H ~ 25 He ~ 1 “metals” Physical changes in a star’s core Progressively fewer atoms as He replaces H Core diameter decreases & temperature increases Rate of hydrogen fusion gradually increases
3
Changes In the Sun Physical changes Chemical changes
The Sun is ~ 40% more luminous than at ZAMS The Sun is ~ 6% larger in diameter than at ZAMS The Sun is ~ 300 K hotter than at ZAMS Chemical changes The Sun’s core is already > 50% He Position on an H-R diagram Increased temperature moves it slightly to the left Increased luminosity moves it slightly upward
4
H & He In the Sun’s Interior
5
The Maturing Sun
6
Main-Sequence Lifetimes
Basic physical relationships Einstein’s famous equation… E = f . M . c2 …where f is the fraction of mass lost in fusion Definition of luminosity… L = E / t E = L . t Combining the two… L . t = f . M . c2 t µ M / L Considering the mass-luminosity relationship… L µ M+3.5 t µ M–2.5
7
Lifetimes of Main-Sequence Stars
8
Red Giant: Sun In 5 Billion Years
9
Changes As Core H Is Exhausted
Basic physical processes Core temperature drops as H fusion ends Core pressure decreases Gravity again dominates Core diameter decreases H just outside the old core compresses & heats H-shell fusion begins No core-He fusion as yet He core eventually reaches ~ 100,000,000 K He fusion into C & O begins & H-shell fusion continues Differences due to mass High- mass stars He fusion begins gradually Low- mass stars He fusion begins in a flash
10
Three Evolutionary Stages for Stars
11
The Pauli Exclusion Principle
Two different kinds of pressure Temperature- dependent pressure Ordinary gas pressure Ideal gas law Force resisting gravity is proportional to temperature Temperature- independent pressure Degenerate electron pressure Pauli exclusion principle Force resisting gravity is independent of temperature Pauli exclusion principle One expression of quantum mechanics Only effective when core gases become ionized Some electrons roam freely Such electrons may not get extremely close to each other Quantum exclusion keeps these electrons apart This exclusion is independent of temperature
12
Degenerate Electrons in Ordinary Metal
13
Star Clusters & Red Giant Evolution
The transition to core He fusion Marks the move into the Red Giant phase Details are determined entirely by mass Analysis of star clusters All a cluster’s stars formed at about the same time All a cluster’s stars have different masses High- mass stars evolve very quickly Some leave the main sequence before low-mass stars can form Low- mass stars evolve very slowly A cluster’s H-R diagram depends on cluster age Lower right band slowly approaches the main sequence Upper left band moves away from the main sequence The turn-off gives the cluster’s age
14
Mass Determines Every Star’s Evolution
The main sequence is a band
15
Main Sequence Turn-Off Points
16
Two Distinct Star Populations
Remnants of the Big Bang Very few atoms heavier than H & He formed Noticeable deficiency of “metals” The oldest stars contain little metal These are Population II stars Remnants of supernovae explosions Relative abundance of “metals” Some even as heavy as Uranium The newest stars contain abundant metal These are Population I stars
17
Metal-Poor & Metal-Rich Stars
Metal-poor Population II stars Metal-rich Population I stars “Metal” means any element heavier than helium
18
Many Mature Stars Pulsate
Critical differences Main sequence stars Characterized by hydrostatic & thermal equilibrium No significant change in diameter Pulsating stars Distinct lack of hydrostatic & thermal equilibrium Cyclical change in diameter Some examples of pulsating stars Long-period variables Cool red giants that vary in luminosity by a factor of ~ 100 Cepheid variables Vary over periods of ~ 1 to ~ 100 days RR Lyrae variables Vary over periods of < 1 day
19
Cepheid Variables As Standard Candles
Two types of Cepheid variables Type I Metal-rich Population I stars More luminous than Type II Cepheids Type II Metal-poor Population II stars Less luminous than Type I Cepheids Standard candles Basic properties Very bright objects of known luminosity Relatively abundant throughout galaxies Cepheids Luminosity is sufficient to be visible at millions of parsecs Luminosity is directly proportional to period
20
Variable Stars On An H-R Diagram
21
d Cephei: A Pulsating Star
22
Mass Transfer Affects Close Binaries
Critical concepts Binary star systems > 50% of all stars are in binary systems Roche lobes Three-dimensional surfaces mark gravitational domains Inner Lagrangian point The gravitational balance point between binary stars Types of binary star systems Detached Neither star fills Roche lobe Semi-detached One star fills Roche lobe Contact Both stars fill Roche lobes Over-contact Both stars over-fill Roche lobes
23
Roche Lobes of Close Binary Stars
24
3 Kinds of Eclipsing Binary Stars
…Semi-detached without mass transfer …with mass transfer Over-contact…
25
Important Concepts Termination of core hydrogen fusion
Zero-age main-sequence stars Main-sequence lifetime of stars Proportional to M2.5 Progressive increase in luminosity Number of atoms in core decreases 4 H atoms become 1 He atom Core contracts & heats Three evolutionary stages of stars Start of core-H fusion into He Birth of a ZAMS star End of core-H fusion into He Start of shell-H fusion Start of core-He fusion into C & O ~ 30% as long as core-H fusion Two kinds of pressure Ordinary gas pressure Degenerate e– pressure Does not depend on temperature Star cluster analysis Same birthday but different masses H-R turn-off gives cluster age Two distinct star populations Metal-poor Population II stars Formed soon after the Big Bang Metal-rich Population I stars Formed long after the Big Bang Variable stars Long-period variables Cepheid variables Used as standard candles RR Lyrae variables Binary star systems Detached Semi-detached Contact Over-contact Mass transfer
Similar presentations
