How do stars form? The Nebular Hypothesis. Observations Stars can be seen in various stages of...
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![Page 1: How do stars form? The Nebular Hypothesis. Observations Stars can be seen in various stages of formation. Stars seem to have been forming continuously.](https://reader035.fdocuments.net/reader035/viewer/2022072006/56649d0e5503460f949e3c81/html5/thumbnails/1.jpg)
How do stars form?
The Nebular Hypothesis
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Observations
• Stars can be seen in various stages of formation.
• Stars seem to have been forming continuously since the formation of the Universe.
• Star formation continues today.• Observations synthesized into the Nebular
Hypothesis.
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Our Sun: an exampleof stellar evolution
• Our Sun began as a nebula, approximately 5 billion years ago.
• A nebula is an enormous cloud of gasses (mainly Hydrogen) and dust
• Nebula may become disturbed by shock waves, for example from a nearby supernova.
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Example of a nebula
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Nebula begins to contract
• As the molecules of gas and dust move closer together, they experience stronger gravitational attraction.
• Newton’s Law of Universal Gravitation
• Fg = g(m1m2)/d2
• Most mass concentrates at the center as the nebula contracts.
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Nebula begins to take a more definite shape.
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Shape becomes spherical with equatorial disk
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Will a star form?
• If mass is sufficient, gravity at the center of the sphere may be great enough to “squash” atoms together.
• 4 H atoms are fused to form 1 He atom in a nuclear reaction (not chemical).
• Nuclear reaction is nuclear fusion, which releases tremendous energy.
• A star is born!
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Stable stars
• Radiant energy produced by fusion causes the star to expand.
• Gravity holds the star together.
• Gas pressure/radiant energy is balanced by gravity, so the star is stable.
• The Hertzsprung-Russell (H-R) Diagram shows these stars as the main sequence.
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The H-R Diagram
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Another version of the H-R Diagram
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H-R Diagram
• Shows relationships among size, temperature and brightness (luminosity or magnitude).
• Larger, stable stars are hotter and brighter.
• Large, hot stars burn out faster than smaller, cooler stars.
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Stellar Evolutionand the H-R Diagram
• What happens when a star exhausts its nuclear fuel?
• Depends on size• Star core collapses on itself, but heats the
outer envelope.• Result may be: White dwarf, white dwarf
with planetary nebula, red giant, neutron star or black hole.
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Stellar collapse
• May result in gravitational heating and eventual burnout.
• May result in renewed fusion (He is fused this time).
• Collapse may produce explosion (supernova).
• Remnant of supernova may be a neutron star or a black hole.
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Products of fusion
• H is fused to form He
• He is fused to form C and other, heavier chemical elements.
• Heavier elements are recycled into new nebulae, and/or new stars and planets.
• Implication?
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Heavy Elements
• Since all elements heavier than H are produced by fusion in stars,
• We are made of Stardust !!!
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Summary: Nebular Hypothesis
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So what happened to the disk?
• The disk that surrounds the central star may
• 1) be swallowed as the star initially expands.
• 2) remain as a disk or a series of rings
• 3) may form planets that orbit the central star.
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Our Solar System
• Sun began to radiate energy about 5 billion years ago.
• Surrounding disk condensed into 9 (possibly 8) planets and an asteroid belt.
• Earth is one of those nine planets.
• Earth condensed approximately 4.6 billion years ago.
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How do we know the timing?
• Age of Sun via chemical composition and known rate of fusion: about 5 Ga
• Oldest Earth rock: 3.98 Ga
• Age of oldest Moon Rocks: 4.2 Ga
• Age of Meteorites: 4.5 Ga
• Ga = Giga-annum = billion years