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Our Sun’s Story …and that of heavy stars. mass of a star determines its core pressure and temperature: our sun’s low mass cooler core and slower fusion rate lower internal temperature, and external (yellow) smaller luminosity longer lifetime (10 B y) - PowerPoint PPT Presentation
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Our Sun’s Story…and that of heavy stars
mass of a star determines its core pressure and temperature:
our sun’s low mass cooler core and slower fusion ratelower internal temperature, and external (yellow)smaller luminositylonger lifetime (10 B y)
high mass stars (> 8 msun) have higher core temperaturemore luminous and higher external temperature (blue)more rapid fusion
shorter-lived (30 M y)
High-Mass Stars
> 8 MSun
Low-Mass Stars< 2 MSun
Intermediate-Mass Stars
Brown Dwarfs
famous Herztsprung- Russell diagram
sun is stable…
as long as it has hydrogen in its core to fuse into helium
Thought Question
What happens when a star no longer has enough hydrogen in its core to fuse to helium?
i.e. after 10 B years
A. Core cools offB. Core shrinks and heats upC. Core expands and heats upD. Helium fusion immediately begins
Thought Question
What happens when a star can no longer fuse hydrogen to helium in its core?
A. Core cools offB. Core shrinks and heats upC. Core expands and heats upD. Helium fusion immediately begins
Life Track after Main Sequence
Observations of stars in clusters, all born at the same time, show that a star becomes larger, redder, and more luminous after fusing all the H in its core
as inert He core contracts, H in a shell around the He core begins burning
luminosity increases 1,000 x too hot for life on
Earth radius grows 100 x,
out to Earthincreased fusion rate in the
H shell does not stop He core from contracting
H shell burns for ~1 B years
luminosity of a sun? same as for any black body…
L Area T4 Stefan-Boltzman law
even though T down 2, A up (100)2 for red giant,
Helium fusion does not begin until heated by collapse requires 100 MK since charge (+2)2 leads to 4 x greater repulsion than with 2 protons
Fusion of 2 helium nuclei doesn’t work (8Be unstable), helium fusion must combine 3 He nuclei to make carbon
Thought Question
What happens in a low-mass star when core temperature rises enough for helium fusion to begin?
A. Helium fusion slowly starts upB. Hydrogen fusion stopsC. Helium fusion (triple alpha) starts very sharply
Hint: this is a strong reaction (no neutrinos)once the temperature is hot enough to overcome Coulomb barrier
Thought Question
What happens in a low-mass star when core temperature rises enough for helium fusion to begin?
A. Helium fusion slowly starts upB. Hydrogen fusion stopsC. Helium fusion rises very sharply
Helium Flash
Core temperature rises rapidly when helium fusion begins
Helium fusion rate skyrockets until thermal pressure takes over and expands core again
Helium burning stars neither shrink nor grow, core He burns to C for 100 M years, then expand again in a second red giant phase
Thought Question
What happens when the star’s core runs out of helium?
A. The star explodesB. Carbon fusion beginsC. The core cools offD. Helium fuses to C in a shell around a heavier carbon core
Thought Question
What happens when the star’s core runs out of helium?
A. The star explodesB. Carbon fusion beginsC. The core cools offD. Helium fuses in a shell around the core
Double Shell BurningAfter core helium used up,
He fuses into carbon in a shell around the inert carbon coreH fuses to He in a shell around the fusing helium layer
double-shell burning stage never reaches equilibrium—fusion rate periodically spikes upward in a series of thermal pulses
With each spike, convection dredges carbon up from core and transports it to surface
Our Sun’s Dregs: a Planetary Nebula
after few M years,double-shell burning ends in a pulse, ejecting H, He, C out into space a planetary nebula (but nothing to do with planets)
white dwarf, carbon core left behind
…two example pix from Hubble
for our sun, C is the end of the fusion trail
fusion progresses no further in a low-mass star mass too small for gravity to collapse it further,
and heat it up even more
electron degeneracy pressure supports white dwarf against gravity
(e-’s approach speed c if m > 1.4 msolar )
temperature never grows hot enough (400 M K) for fusion to heavier elements e.g. for He to fuse with C to make oxygen
Life stages of a low-mass star like the Sun
Life Path of a Sun-Like Star
How different are life stages of high-mass (e.g. 25 m๏) star?
similar to those of low-mass stars, like our sun, but each is faster
Hydrogen core fusion, ~ M years
not pp, but much faster CNO cycle, higher luminosity making N and O as well as He
becomes a red supergiant when core H exhausted
Hydrogen shell burning around a He core
Helium core fusion to carbon, lasting ~ 100,000 years
Carbon burning (0.6 B ºK) for ~ 100 years
CNO CycleHigh-mass fuse H to He at a higher rate using carbon catalyst, CNO cycle
Greater core temperature heavy nuclei overcome greater Coulomb repulsion
What are the life stages of a high-mass star?
How do high-mass stars make the elements necessary for life?
Big Bang made 75% H, 25% He – stars make everything else
3 Helium fusion makes carbon in low-mass stars
CNO cycle changes C into N and O
Helium Capture by O and Ne
higher core temperatures from successive gravitational collapses gives helium the energy to thwart ever stronger Coulomb barriers (zZ) of heavier elements
Advanced Nuclear Burning
• Core temperatures in stars with >8MSun
allow fusion of elements as heavy as iron
Multiple Shell Burning• Advanced nuclear
burning proceeds in a series of nested shells
Iron = dead end for fusion
nuclear reactions of iron release no energy
Fe has lowest mass per nucleon
signature of helium capturenucleosysthesis:
highest abundances are elements with
even numbers of protons
Iron builds up in core until degeneracy pressure can no longer resist gravity
Core then suddenly collapses, creating supernova explosion
Energy and neutrons released in supernova explosion enable elements heavier than iron to form, including Au and U
What causes a supernova collapse?
Core degeneracy pressure disappearselectrons combine with protons,
making neutrons and neutrinos
kT + me + mp > mn
kT + 0.5 + 938.3 > 939.6 MeV
Ethermal = kT @ 10 BK = 1 MeV,k = Boltzman’s constant
Neutrons collapse to the center, forming a much smaller (~10km~Boston)
neutron star (me/mn ~ 1/2000)
… then collapsing to a black hole if 12 msun
Supernova Remnant
energy released by core collapse drives outer layers into space
Crab Nebula the remnant of supernova of AD 1054
…and its neutron star
our picture of a pulsar (neutron star)
during collapse…
angular momentum conserved big spin up
magnetic fields pinched very strong
but in chaos of explosion, magnetic rotational axis
beams of radiation escape along magnetic axis
“lighthouse” beam sweeps periodically past earth…spinning so fast it can only be from a compact source, r ~
10 km
Supernova 1987A
closest supernova in the last four centuries