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Transcript
Guiding Questions The Deaths of Stars 1 Pathways of Stellar Evolution GOOD TO KNOW 1. What kinds of nuclear reactions occur within a star like the Sun as it ages? 2. Where did the carbon atoms in our bodies come from? 3. What is a planetary nebula, and what does it have to do with planets? 4. What is a white dwarf star? 5. Why do high-mass stars go through more evolutionary stages than low-mass stars? 6. What happens within a high-mass star to turn it into a supernova? 7. Why was SN 1987A an unusual supernova? 8. What was learned by detecting neutrinos from SN 1987A? 9. How can a white dwarf star give rise to a type of supernova? 10.What remains after a supernova explosion? 2 Low-mass stars go through two distinct red-giant stages 3 5 • A low-mass star becomes – a red giant when shell hydrogen fusion begins – a horizontal-branch star when core helium fusion begins – an asymptotic giant branch (AGB) star when the helium in the core is exhausted and shell helium fusion 4 begins 6 1 Bringing the products of nuclear fusion to a giant star’s surface • As a low-mass star ages, convection occurs over a larger portion of its volume • This takes heavy elements formed in the star’s interior and distributes them throughout the star 7 8 9 10 11 12 Low-mass stars die by gently ejecting their outer layers, creating planetary nebulae • Helium shell flashes in an old, low-mass star produce thermal pulses during which more than half the star’s mass may be ejected into space • This exposes the hot carbon-oxygen core of the star • Ultraviolet radiation from the exposed core ionizes and excites the ejected gases, producing a planetary nebula 2 Why do planetary nebulae look so different from one another? 13 14 The burned-out core of a low-mass star cools and contracts until it becomes a white dwarf • No further nuclear reactions take place within the exposed core • Instead, it becomes a degenerate, dense sphere about the size of the Earth and is called a white dwarf • It glows from thermal radiation; as the sphere cools, it becomes dimmer 15 16 17 18 3 High-mass stars create heavy elements in their cores • Unlike a low-mass star, a high mass star undergoes an extended sequence of thermonuclear reactions in its core and shells • These include carbon fusion, neon fusion, oxygen fusion, and silicon fusion 19 20 High-mass stars violently blow apart in supernova explosions • In the last stages of its life, a high-mass star has an iron-rich core surrounded by concentric shells hosting the various thermonuclear reactions • The sequence of thermonuclear reactions stops here, because the formation of elements heavier than iron requires an input of 21 energy rather than causing energy to be released 23 • A high-mass star dies in a violent cataclysm in which its core collapses and most of its matter is ejected into space at high speeds • The luminosity of the star increases suddenly by a factor of around 108 during this explosion, producing a supernova • The matter ejected from the supernova, moving at supersonic speeds through interstellar gases and dust, glows as a nebula called a supernova remnant 22 24 4 In 1987 a nearby supernova gave us a close-up look at the death of a massive star 25 26 Neutrinos emanate from supernovae like SN 1987A 27 White dwarfs in close binary systems can also become supernovae • An accreting white dwarf in a close binary system may become a supernova when carbon fusion ignites explosively throughout the degenerate star 29 More than 99% of the energy from such a supernova is emitted 28 in the form of neutrinos from the collapsing core Type Ia supernovae are those produced by accreting white dwarfs in close binaries 30 5 Type Ib and Type Ic supernovae occur when the star has lost a substantial part of its outer layers before exploding 31 32 33 34 Type II supernovae are created by the deaths of massive stars Most supernovae occurring in our Galaxy are hidden from our view by interstellar dust and gases but a supernova remnant can be detected at many wavelengths for centuries after the explosion Jargon • asymptotic giant branch • asymptotic giant branch star(AGB star) • carbon fusion • carbon star • Cerenkov radiation • Chandrasekhar limit • core helium fusion • dredge-up • helium shell flash • horizontal branch • mass-radius relation • neon fusion • neutron capture • nuclear density • oxygen fusion 35 • • • • • • • • • • • • • • • • photodisintegration planetary nebula progenitor star red-giant branch shell helium fusion silicon fusion supergiant supernova (plural supernovae) supernova remnant thermal pulse Type I supernova Type Ia supernova Type Ib supernova Type Ic supernova Type II supernova white dwarf 36 6