LIFECYCLES OF STARS
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Transcript of LIFECYCLES OF STARS
M.R. Burleigh 2601/Unit 5
DEPARTMENT OF PHYSICS AND ASTRONOMY
LIFECYCLES OF STARSLIFECYCLES OF STARS
Option 2601Option 2601
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Stellar PhysicsStellar Physics
Unit 1 - Observational properties of Unit 1 - Observational properties of starsstars
Unit 2 - Stellar SpectraUnit 2 - Stellar Spectra Unit 3 - The SunUnit 3 - The Sun Unit 4 - Stellar StructureUnit 4 - Stellar Structure Unit 5 - Stellar EvolutionUnit 5 - Stellar Evolution Unit 6 - Stars of particular interestUnit 6 - Stars of particular interest
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DEPARTMENT OF PHYSICS AND ASTRONOMY
Unit 5Unit 5
Stellar EvolutionStellar Evolution
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Stellar EvolutionStellar Evolution
Star formationStar formation Main sequenceMain sequence Stellar clusters (open, globular)Stellar clusters (open, globular) Population I & II starsPopulation I & II stars Red GiantsRed Giants Planetary NebulaePlanetary Nebulae White DwarfsWhite Dwarfs SupernovaeSupernovae Neutron StarsNeutron Stars
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SequenceSequence
ProtostarProtostar Pre-main Sequence (PMS)Pre-main Sequence (PMS) Main SequenceMain Sequence Post-main SequencePost-main Sequence
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ProtostarsProtostars
Stars born by gravitational contraction Stars born by gravitational contraction of interstellar clouds of gas and dustof interstellar clouds of gas and dust
Gravitation energy Gravitation energy 50% thermal & 50% thermal & 50% radiative50% radiative
Cloud is a Cloud is a ProtostarProtostar before hydrostatic before hydrostatic equilibrium is establishedequilibrium is established
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ProtostarsProtostars
Collapse starts in “free fall”Collapse starts in “free fall”– Particles do Particles do notnot collide during collapse collide during collapse– i.e. P=0, gravity is only force involvedi.e. P=0, gravity is only force involved
Collapse is unevenCollapse is uneven– Core collapses more rapidly forming a Core collapses more rapidly forming a
small central condensationsmall central condensation– Core then Core then accretes accretes materialmaterial
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ProtostarsProtostars
Low mass objects accrete all (most) of Low mass objects accrete all (most) of materialmaterial
High mass objects behave similarly, High mass objects behave similarly, butbut– Fusion begins before end of accretionFusion begins before end of accretion– Some material then blown away by Some material then blown away by
radiation pressureradiation pressure
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Effect of RotationEffect of Rotation
If angular momentum > 0If angular momentum > 0– Cloud flattens into a diskCloud flattens into a disk
In some cases several central blobs In some cases several central blobs form, which can coalesce into fewer…form, which can coalesce into fewer…
Multiple star systemsMultiple star systems
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Cloud CollapseCloud Collapse
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Star FormationStar Formation
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Star FormationStar Formation
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Star FormationStar Formation
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Pre-main sequence for a solar mass star
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Evolution of a high mass star
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Star Formation Star Formation
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Star FormationStar Formation
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Stellar LifecycleStellar Lifecycle
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The Main SequenceThe Main Sequence
Start of nuclear burning Start of nuclear burning zero-age zero-age main sequence main sequence
As H As H He composition ( He composition () changes, ) changes, structure changesstructure changes
Rates of evolution depend on two Rates of evolution depend on two thingsthings
1.1. Initial massInitial mass2.2. CompositionComposition
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The Main SequenceThe Main Sequence
High mass stars are hotter & more High mass stars are hotter & more luminousluminous
Use their energy faster, i.e. evolve Use their energy faster, i.e. evolve fasterfaster
Spend less time on the main sequenceSpend less time on the main sequence O & B stars evolve faster than M starsO & B stars evolve faster than M stars
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Mass-luminosity relation:
3.3
**
SunSun MM
LL
3.2
***
*
SunLLMM
Sun MM
tt
Sun
Sun
Giving star lifetime:
QuantitativelyQuantitatively
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Eagle NebulaEagle Nebula
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Eagle NebulaEagle Nebula
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Rosette NebulaRosette Nebula
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TT
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The PleiadesThe Pleiades
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Population I StarsPopulation I Stars
Accreting from the ISM now! (i.e. recent past)Accreting from the ISM now! (i.e. recent past) Typical stars are young, in galactic spiral Typical stars are young, in galactic spiral
arms where gas and dust foundarms where gas and dust found Typically reside in open star clustersTypically reside in open star clusters ~2% of mass elements heavier than H or He ~2% of mass elements heavier than H or He
(ISM enriched by supernovae)(ISM enriched by supernovae) If MIf M* * a little > Ma little > M energy generation is by CNO energy generation is by CNO
cyclecycle Sun is population ISun is population I
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Post main-sequence for a solar mass star
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Evolutionary phases of a solar mass star, post main-sequence
H-R positionH-R position StageStage Physical processesPhysical processes
33 ZAMSZAMS Core hydrogen burning beginsCore hydrogen burning begins
44 Evolution on main-Evolution on main-sequencesequence
Core hydrogen burning ceases; shell Core hydrogen burning ceases; shell hydrogen burning beginshydrogen burning begins
55 Evolution off main-Evolution off main-sequencesequence
Shell hydrogen burning continues; Shell hydrogen burning continues; convection dominates energy transportconvection dominates energy transport
66 Red giantRed giant Helium flash occurs; core helium burning Helium flash occurs; core helium burning beginsbegins
77 SubgiantSubgiant Core helium burning continues along with Core helium burning continues along with shell hydrogen burningshell hydrogen burning
Red giant againRed giant again Thermonuclear reactions then end; shell Thermonuclear reactions then end; shell helium and hydrogen burning continues helium and hydrogen burning continues
88 Planetary nebulaPlanetary nebula Star enters the planetary nebula stageStar enters the planetary nebula stage
99 White dwarfWhite dwarf All thermonuclear reactions stop; slow All thermonuclear reactions stop; slow coolingcooling
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End of Main SequenceEnd of Main Sequence
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Post main-sequence for a solar mass star
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Population II StarsPopulation II Stars
First stars to be formed in UniverseFirst stars to be formed in Universe Have only 0.01% heavy elementsHave only 0.01% heavy elements Typically found in galactic bulge and globular Typically found in galactic bulge and globular
clustersclusters Similar sequence of evolution but occupy Similar sequence of evolution but occupy
different region of H-R diagram during core different region of H-R diagram during core He burningHe burning
Significant temperature changes, heating and Significant temperature changes, heating and then coolingthen cooling
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Late in the life of a solar mass star
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Red Giant > PN Red Giant > PN
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Evolutionary phases of a solar mass star, post main-sequence
H-R positionH-R position StageStage Physical processesPhysical processes
33 ZAMSZAMS Core hydrogen burning beginsCore hydrogen burning begins
44 Evolution on main-Evolution on main-sequencesequence
Core hydrogen burning ceases; shell Core hydrogen burning ceases; shell hydrogen burning beginshydrogen burning begins
55 Evolution off main-Evolution off main-sequencesequence
Shell hydrogen burning continues; Shell hydrogen burning continues; convection dominates energy transportconvection dominates energy transport
66 Red giantRed giant Helium flash occurs; core helium burning Helium flash occurs; core helium burning beginsbegins
77 SubgiantSubgiant Core helium burning continues along with Core helium burning continues along with shell hydrogen burningshell hydrogen burning
Red giant againRed giant again Thermonuclear reactions then end; shell Thermonuclear reactions then end; shell helium and hydrogen burning continues helium and hydrogen burning continues
88 Planetary nebulaPlanetary nebula Star enters the planetary nebula stageStar enters the planetary nebula stage
99 White dwarfWhite dwarf All thermonuclear reactions stop; slow All thermonuclear reactions stop; slow coolingcooling
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Late in the life of a solar mass star
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PN > White DwarfPN > White Dwarf
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White DwarfsWhite Dwarfs
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For a perfect gas: nkTP TP From hydrostatic equilibrium:
31
1
MR Greater mass, smaller radius
White dwarfs form from stars with M 8MSun
Degenerate gas pressure prevents further gravitational contraction
Chrandrasekhar limit: degeneracy pressure can only support M 1.4MSun. Above this limit a neutron star is formed
For a degenerate gas (non-relativistic): 35
KP Constant
Chandrasekhar LimitChandrasekhar Limit
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White dwarf companions
e.g. Sirius – companion Sirius B (Alvan Clark, 1862)
Procyon – Procyon B (1882)
In binaries we can measure the companion’s mass from Kepler’s laws
MSirius B = 1.0MSun
TSirius A = 10,000K ; MV = -1.5
TSirius B = 25,000K ; MV = 8
From :
R 7 10-3RSun
= 3 109kg m-3
424 TRL Sun 3 10-3LSun
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Massive StarsMassive Stars
Stars with masses > 7 MStars with masses > 7 M
Masses greater than ~ 50 MMasses greater than ~ 50 M
– Affected by mass loss (i.e. winds)Affected by mass loss (i.e. winds)– As mass of star changes so does the As mass of star changes so does the
structure and luminositystructure and luminosity
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Evolution of a high mass star
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StageStage Physical processesPhysical processes
ProtostarProtostar Dust and gas cloud collapses rapidly, Dust and gas cloud collapses rapidly, accompanied by heating of the interior and accompanied by heating of the interior and ionisation of atomsionisation of atoms
PMSPMS Semihydrostatic equilibrium; contraction and Semihydrostatic equilibrium; contraction and heating continueheating continue
ZAMSZAMS Hydrogen burning commencesHydrogen burning commences
Initial evolution on the main Initial evolution on the main sequence sequence
Hydrogen consumed in the core; some Hydrogen consumed in the core; some contraction occurscontraction occurs
Evolution off the main sequenceEvolution off the main sequence Hydrogen depleted in the core, isothermal helium Hydrogen depleted in the core, isothermal helium core and hydrogen-burning establishedcore and hydrogen-burning established
Evolution to the right in the H-R Evolution to the right in the H-R diagramdiagram
Core rapidly contracts, envelope expands, Core rapidly contracts, envelope expands, hydrogen-burning shell narrowshydrogen-burning shell narrows
Red giantRed giant Energy output increases, convective envelope Energy output increases, convective envelope forms, helium burning beginsforms, helium burning begins
CepheidCepheid Convective shell contracts, core helium burning Convective shell contracts, core helium burning becomes the major energy sourcebecomes the major energy source
SupergiantSupergiant Helium-burning shell formsHelium-burning shell forms
Evolutionary phases of a massive star
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Evolution of a high mass star
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SupernovaeSupernovae
Absolute magnitudes from –16 to –20 Absolute magnitudes from –16 to –20 (energy ~10(energy ~104444J)J)– e.g. China, SN of 1054 reached me.g. China, SN of 1054 reached mVV=-6 =-6
(remnant is Crab Nebula)(remnant is Crab Nebula) Two types… Type I & Type IITwo types… Type I & Type II Both types eject a large fraction of Both types eject a large fraction of
original mass with v~5000-10000 km soriginal mass with v~5000-10000 km s-1-1
Explosion of stellar Explosion of stellar interiorinterior
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Type II SupernovaeType II Supernovae
Seen in spiral galaxies only, especially in Seen in spiral galaxies only, especially in spiral arms… Population I starsspiral arms… Population I stars
Explosions in cores of Blue/Red Supergiants Explosions in cores of Blue/Red Supergiants (10-100M(10-100M))
Implosion of stellar core to form neutron starImplosion of stellar core to form neutron star– Core reaches density > electron pressureCore reaches density > electron pressure
Violent rebound > explosion > ejects outer Violent rebound > explosion > ejects outer layerslayers
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Type II SupernovaeType II Supernovae
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SN 1987ASN 1987A
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Type I SupernovaeType I Supernovae
Seen in both elliptical and spiral Seen in both elliptical and spiral galaxies… Population II starsgalaxies… Population II stars
Progenitors are H-deficient, highly Progenitors are H-deficient, highly evolved starsevolved stars
Mechanism not well understoodMechanism not well understood– Accretion onto a WD increasing MAccretion onto a WD increasing MWDWD > >
Chandrasekhar limitChandrasekhar limit– Merger of two WDs to give M > 1.4MMerger of two WDs to give M > 1.4M
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Type Ia SupernovaeType Ia Supernovae
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Supernovae: Key PointsSupernovae: Key Points
SN responsible for nucleosynthesis of SN responsible for nucleosynthesis of element above element above 5656FeFe
Remnant neutron stars… sometimes Remnant neutron stars… sometimes revealed as pulsarsrevealed as pulsars
Shockwave heating of interstellar Shockwave heating of interstellar medium… medium… Supernova RemnantsSupernova Remnants
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Supernova RemnantsSupernova RemnantsVelaVela
Crab NebulaCrab Nebula
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Supernova RemnantsSupernova Remnants
Cassiopiea ACassiopiea A
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Supernova expansion
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Schematic H-R diagram showing the spectral classification of stars
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H-R diagram for stars near the Sun
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H-R diagram from Hipparcos data
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Cluster H-R DiagramsCluster H-R Diagrams
In a cluster, compared to evolutionary In a cluster, compared to evolutionary timescales, the stars are all (roughly) timescales, the stars are all (roughly) the same agethe same age
H-R Diagram can reveal the age of the H-R Diagram can reveal the age of the clustercluster
Need to identify the “turn-off”, mass Need to identify the “turn-off”, mass above which all stars have evolved above which all stars have evolved away from the main sequenceaway from the main sequence
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H-R diagram showing open cluster (pop I) ages
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Globular ClustersGlobular Clusters
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Globular Cluster AgesGlobular Cluster Ages
Population II stars, few heavy elementsPopulation II stars, few heavy elements Older than open clustersOlder than open clusters Also have different tracks due to Also have different tracks due to
composition differencescomposition differences
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H-R diagram for a globular cluster
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Stellar EvolutionStellar Evolution
Star formationStar formation Main sequenceMain sequence Stellar clusters (open, globular)Stellar clusters (open, globular) Population I & II starsPopulation I & II stars Red GiantsRed Giants Planetary NebulaePlanetary Nebulae White DwarfsWhite Dwarfs SupernovaeSupernovae Neutron StarsNeutron Stars
M.R. Burleigh 2601/Unit 5
DEPARTMENT OF PHYSICS AND ASTRONOMY
Unit 5Unit 5
Stellar EvolutionStellar Evolution
M.R. Burleigh 2601/Unit 5
Stellar PhysicsStellar Physics
Unit 1 - Observational properties of Unit 1 - Observational properties of starsstars
Unit 2 - Stellar SpectraUnit 2 - Stellar Spectra Unit 3 - The SunUnit 3 - The Sun Unit 4 - Stellar StructureUnit 4 - Stellar Structure Unit 5 - Stellar EvolutionUnit 5 - Stellar Evolution Unit 6 - Stars of particular interestUnit 6 - Stars of particular interest
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DEPARTMENT OF PHYSICS AND ASTRONOMY
STELLAR PHYSICSSTELLAR PHYSICS
Option 2607Option 2607
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Mass-radius relationship for white dwarfs
Marked is the best fitting mass and radius for V471 Tau, with 1 and 2 sigma uncertainty contours
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DA Hydrogen dominated Non-DA Helium dominated
PROGENITORS – SdB, SdOB, SdO, H-rich
PNN?
Hottest DO stars
DO pulsationsDO cooling
sequenceCoolest DO
stars
No known
PROGENITORS – He-rich SdO
and PNNLate helium thermal pulse
Settling of He and CNO
Dredge up of helium
Hottest DA stars
DA cooling sequence
DA pulsations
DO or DBs
DB pulsations
DB cooling sequence
70,000K
13,000K
10,000K
30,000K
45,000K
150,000K
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White Dwarf CoolingWhite Dwarf Cooling
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