the death of stars
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The Death of Stars. Parts of a MS star. What holds a star up while it is on the MS?. On the Main Sequence. How does energy get out?. Radiation & Convection May take a million years to reach the surface. The smallest stars. - PowerPoint PPT PresentationTRANSCRIPT
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On the Main Sequence
What holds a star up while it is on the MS?
Parts of a MS star
How does energy get out?
Radiation & Convection May take a million years to reach the surface.
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Brown Dwarfs : Stars with core mass < .08 Msun (failed stars).
Brown Dwarfs do not get hot enough to fuse H, but they do fuse Deuterium for a very short time. Deuterium is an isotope of H, with a neutron. About 1,000 Brown Dwarfs have been found. They radiate in the infrared wavelength.
The smallest stars
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Red Dwarfs : Stars with a core mass of .08 to 0.4 solar mass
Coolest and dimmest of all MS stars. They remain on MS hundreds of billions of years. When all the H is converted to He fusion ceases, they cool down, moving down and to the right in the H-R diagram.
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Red Dwarfs are very low mass stars with no more than 40% of the mass of the Sun and represent the majority of the stars.
. They have relatively low temperatures in their
cores; red dwarfs transport energy from the core to the surface by convection.
A low-mass main-sequence star of spectral classes M and L. Red dwarf stars range from about 0.6 solar mass at class M0 down to 0.08 solar mass in cool M
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Death of Low Mass Star
0.5 - 1.4 White Dwarf
Core Mass Final State
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Thermodynamics
When Fusion stops, core shrinks & temperature of core rises.
When the Envelope expands its temperature cools down.
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Main Sequence Phase
Energy Source: H fusion in the core
Using P-P cycle H fuses to He
Slowly builds up an inert He core
Evolution of Low-Mass Stars
0.5 - 1.4 Msun
He Fusing
Envelope
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When the H in the core is almost completely converted into He, H fusion stops in core. The left over H is pushed out into a shell ring around the He core. The core collapses & heats up.
Outer layer expands and cool forming a
Red Giant
The increasing temp will cause the H shell to fuse forming He that will join the core
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(On the H_R Diagram)
•
•The star gets brighter and redder, climbs up the Giant Branch. (Takes 1 Byr)
At the top of the Giant Branch, the star’s envelope is about the size of Venus’ orbit
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• The core will contract until it gets hot enough to fuse the He in the core into Carbon & Oxygen.
When the fusion begins, the burning occurs rapidly because of the H shell burning and the He burning in the core. This is called the “Helium Flash”. Some of the outer layers are blown outward causing the star to loose mass.
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The star gets hotter, and moves onto the
Horizontal Branch
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•C-O core collapses and heats up •He burning shell outside the C-O core •H burning shell outside the He burning shell
The core never gets hot enough to fuse the Carbon & Oxygen Outside: Envelope swells &cools because of H & He burningClimbs the Asymptotic Giant Branch
Once the He fuses and forms C & O, the core contracts.
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Climbs the Giant Branch again, slightly to the left , and higher, becoming a super red giant. .
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With weight of envelope taken off, core never reaches Carbon fusion temp of 600 Million K
Outer envelope gets slowly ejected . This is a non-violent ejection; a series of puffs or burps.Expanding envelope forms a ring nebula around the contracting C-O core.
Core and Envelope separate, takes ~100,000 yr
C-O core continues to contract:
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A Planetary Nebula forms
Hot C-O core is exposed, moves to the left Becomes a White Dwarf
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Planetary Nebulae
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Fig. 13.16cButterfly Nebula
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Outer shellsof red supergiant“puffed off”
Ejection not explosive
Nebula shell expands
Hot dwarf left behind
Cools down to form a WD
Planetary Nebula
The nebula is ionized, and heated by the. Ultra-violet radiation from the hot star
•After ~ 50,000 years, the nebula spreads so far that the nebulosity simply fades from view.
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White Dwarfs have a mass that is less than 1.4 MoThey will shine for a long time but no fusion is taking place.
Contraction of the core is stopped by electron degeneracy. The electrons repel each other as they are pressed closer together and a White Dwarf forms.
•One teaspoon weighs about 5 tons.
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Electron energy levels
• Only two electrons (one up, one down) can go into each energy level.
• In a degenerate gas, all low energy levels are filled.
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White Dwarf’s mass < than the White Dwarf’s mass < than the Chandrasekhar massChandrasekhar mass (1.4 Solar Mass)(1.4 Solar Mass)
Radius (a little smaller than Earth!)
Temp. – anywhere from 100,000 to 2500 K.
White dwarfs shine by leftover heat, no fusion.
WD will cool off and fade away slowly, becoming a "Black Dwarf“.
Takes ~10 Tyr to cool off , so none exists yet.
White Dwarfs are planetary in size, but have a stellar mass
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Sirius B
Sirius B Temp. 25,000 KSize: 92% Earth's diameterMass: 1.2 solar masses
Sirius B
The most famous W.D. is Sirius’ companion .
The mass of a star, in the size of a planet.
White Dwarfs are so small, that they can only be seen if close-by, or in a binary systems.
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A lone white dwarf is a cooling corpse but a white dwarf in a binary system can be revived
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There is more !! A White Dwarf in a binary system…
White DwarfEvolving (dying) star
Roche Lobes
Evolving (dying) starWhite Dwarf
Accretion Disk
Roche Lobe filled
Evolving (dying) star
I
II
III
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Type 1a
super NOVA!!
W.D. can take on material but, if the W.D. exceeds 1.4 solar masses (Chandrasekar limit)powerful explosions take place and they could happen more than once. The star will get down below 1.4 solar mass.
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Since the Type 1a supernova is always a white dwarf they can be used to judge very great distances (using the inverse square law). Type Ia: No hydrogen lines in the spectrum
Type II: Hydrogen lines in the spectrum
There is a further subdivision of I into Ia, Ib, Ic
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Low Mass StarsSun
Core forms a White Dwarf
White Dwarf becomes a Black Dwarf (dead star)
If the White Dwarf is a binary star, a Supernova type 1a can form, if its mass becomes greater than 1 ¼ solar masses
Envelope separates from core and forms a planetary nebulaRed Giant
Becomes Red Giant when H is almost gone
Only H , He in shells, C & O in core left C & O do not fuse
Orbit out to almost Venus
Becomes a Red Super Giant
Red Super Giant
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Of course you know the relationship is just going to end in a Type 1a supernovae...but I suppose its better to have transferred mass and exploded than to have never transferred mass at all...
Wanted
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Crab NebulaSupernovaRemnantStellar Graveyard
High Mass Stars
1.4 < M < 3.0 Neutron Star
Final Core Mass Final State
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massive stars evolve more rapidly due to rapid nuclear burning, and massive stars produce heavier elements
Massive stars have the same internal changes as we saw in low mass stars ,
Evolution of Massive Stars
except :
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Evolution of High-Mass Stars High-Mass Stars
O & B Stars core mass >1.4 and <3 Msun •Burn Hot •Live Fast •Die Young
Main Sequence Phase:
•Burn H to He in core using the CNO cycle
•Build up a He core, like low-mass stars
•But this lasts for only ~ 10 Myr
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Red Supergiant Phase
After H core exhaustion: •Inert He core contracts & heats up the H burning in a shell .• Envelope expands due to the burning H shell and cools•Envelope ~ size of orbit of Jupiter
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Moves horizontally across the H-R diagram, becoming a Red Supergiant star
Takes about 1 Myr to cross the H-R diagram.
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Core Temperature reaches 170 Million K
Helium Flash : Helium ignites
This Helium flash is not as explosive as the one for low mass stars.
Helium Fusion produces C & O in core:
Star heats up and becomes a Yellow Supergiant.
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Star becomes a Yellow Supergiant.
Yellow
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When He exhausted in core
•Inert C-O core collapses & heats up the H & He burning in shells. Star expands and becomes a Red Supergiant again
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C-O Core collapses until: Tcore> 600 MillionK • Carbon in the Core ignites.
C fuses to form : Ne , and O
•Core at the end of • Carbon Burning •Phase:
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1. Hydrogen burning: 10 Myr2. Helium burning: 1 Myr3. Carbon burning: 1000 years4. Neon burning: ~10 years5. Oxygen burning: ~1 year6. Silicon burning: ~1 day Finally builds up an inert Iron core
Nuclear burning continues past HeliumThings happen fast!
End of the line!!
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Massive star at the end of Silicon Burning: Onion Skin of nested nuclear burning shells
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Protons & electrons form neutrons & neutrinos. Collapse is final.
At the start of Iron Core collapse:
•Radius ~ 6000 km (~Rearth)
•Density ~ 108 g/cc
A second later!! , the properties are:
•Radius ~50 km
•Density ~1014 g/cc
•Collapse Speed ~0.25 c !
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Supernova explosionNeutron degeneracy pressure halts the collapse
Material falling inwards rebounds.
Outer layers of the atmosphere, including shells, are blown off in a violent explosion called a supernova.
The star will outshine all the other stars in the galaxy combined.
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The ejected material often attain speeds of 100,000 km/sec.
Elements heavier than Lead are produced in the explosion and ejected into space. Stars do recycle.
Close to 150 supernova remnants have been detected in the Milky Way.
There are smaller numbers of massive stars and so smaller amount of explosions.
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The Famous Supernova
Before
At maximum
type II Supernova
SN 1987A
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Supernova remnants
Cas A in x-rays (Chandra)
Vela
SN1998bu
Remnant of SN386, with central pulsar (Chandra)
Cygnus Loop (HST): green=H, red=S+, blue=O++
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The rings of
SN 1987A
are from previous
mass loss
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1a is binary with a White DwarfType II : Hydrogen lines in the spectrum
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Supernova explosion
1, The iron core collapses
2. Neutrons stop the collapse
3. The rebound of the core sends shock waves causing an explosion that blows the outer atmosphere into space as a super nova
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• The Crab Nebula.
• A supernova that, according to the Chinese, exploded in 1054.
• Despite a distance of ~ 7,000 light-years, the supernova was brighter than Venus for weeks before fading from view after nearly two years.
•Even today, the nebula
• is still expanding at
• more than 3 million
•miles per hour.
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Structure of a Neutron Star
•Diameter~ 12 km in diameter
•Mass -about 1.4 times that of our Sun.
•One teaspoonful of material would weigh a billion tons! Rotation Rate: 1 to 100 rotations/sec
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The magnetic axis is miss-aligned with the rotation axis of the neutron star .The star's rotation sweeps the beams outward as it rotates.If we are in the sight path, will see regular, sharp pulses of light (optical, radio, X-ray.)
Lighthouse Model:
field generates a
Spinning magnetic
a strong electric field.
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Pulsars: emitted sharp, 1 millisecond-long pulses every second at an extremely repeatable rate.
A typical pulsar signal, received with a radio telescope
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The connection between pulsars and neutron stars was the discovery of a pulsar in the crab nebula.
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Iron
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Proto-stars (born in cool gas GMC)
Main Sequence Stars (H Fusion)
Core Mass (CM) > 1.4 MO
Red Super Giant
Red Super Giant
Yellow Super Giant
Supernova (Type II)
Neutron Star Black Hole
CM > 1.4 & < 3 CM > 3
Black Dwarf
Red Giant
Red Super Giant
Planetary Nebula
White Dwarf
Binary can produce Type ia supernova
Brown
Dwarf
CM<0,08
Core Mass (CM) 0.5- 1.4 MO
Red Dwarf 0.08 - 0 .5 MO
CM 0.5 – 1.4 MO
White Dwarf
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Neutron Star
High
Mass
Very High M
ass
Black Hole
Supernova
Massive Stars
Outer layers of the atmosphere, including shells, are blown off in a violent explosion called a supernova
Red Supergiant
Red Supergiant
Massive star
Becomes Yellow Supergiant when He exhausted
Orbit size of Jupiter
Becomes Red Supergiant
Yellow Supergiant
Becomes a Red Supergiant when H exhausted
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Black Holes
We know of no mechanism to halt the collapse of a compact object with mass > 3 Msun.
It will collapse into a single point – a singularity:
=> Becoming a Black Hole!
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Honeycutt H
Has He
Caused C
No Ne
Oxford O
Student Si
Injury (Iron) Fe
To memorize this sequence, use this :
Massive stars form the following:H, He, C, Ne, O, Si, Fe . Iron will not fuse. Low mass stars form only H, He, C, O
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Thanks to the following for allowing me to use information from their web site :
Nick Stobel
Bill Keel
Richard Pogge
NASA