Textbook Chapters 24 - Stars Textbook Chapter 25 - Universe. Regents Earth Science with Ms. Connery
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1 Textbook Chapters 24 - Stars Textbook Chapter 25 - Universe Regents Earth Science with Ms. Connery
2 SPECTROSCOPY is the study of light. Read to learn - textbook pages STAR LIGHT gives us characteristics of stars & galaxies From VISIBLE LIGHT luminosity - brightness based on how much energy is being emitted from the star temperature - how fast the molecules are moving distance - how far away the star is size - how big the star is From SPECTRUM composition - what star is made of Doppler motion - if star is moving towards or away from observer
3 STARLIGHT spectroscopy nuclear fusion hydrogen helium self-illuminating emit light (emission) electromagnetic spectrum EM wavelengths star mass luminosity visible color & temperature spectrum & composition BIG BANG Doppler effect red shift (expanding universe) blue shift (collapsing universe) STELLAR EVOLUTION protostar main sequence star giant star supergiant star dwarf star nova supernova black hole
4 We see all these EM energy forms coming from stars. If we can read them we gain knowledge of things that are very distant both in space and time!
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7 Universe everything that exists Galaxy contains 100 x 10 9 solar systems Nebula where stars form Solar system star + its orbiting planets Star energy emitting mass of incandescent gas held together by gravity Natural satellites in orbit around a central body Planets (orbit stars like our sun) Moons (orbit planets) Human-made satellites
8 200 B stars Our solar system is 2/3 out from center
9 Orion Nebula star forming region
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11 How does nuclear fusion in the core of stars emit light and what does that light tell us? (text pgs689-90)
12 STARS HAVE DIFFERENT LAYERS Corona STARS are self-illuminating and give off their own light as long as there s nuclear fusion in the core!
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14 Energy production in stars by NUCLEAR FUSION Hydrogen IS TURNED INTO Helium fusion requires extremely high temperature (millions of degrees) and pressure fused nuclei RELEASE ENERGY (just like nuclear fusion weapons) Energy is released in all directions (sphere shape) Our eyes can only see the visible light
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18 How does a matrix of star size, color, temperature, and luminosity show us the life cycle of stars?
19 Star Anatomy (text pg ) Hertzprung Russell Diagram (ESRT graph) of Star Characteristics (text pg ) Stellar Evolution (text pg )
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21 In order to see the characteristics of stars and how they group out, data for hundreds of thousands of stars were graphed. You ll just do a few to get the idea (and appreciate the work it takes to see these patterns!
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24 MAIN SEQUENCE (young & stable) Temp range Color range Luminosity range Size range WHITE DWARF (old age & dying) Temp range Color range Luminosity range Size range GIANT (middle age and unstable) Temp range Color range Luminosity range Size range SUPERGIANT (middle age & unstable) Temp range Color range Luminosity range Size range
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33 Stars start as PROTOSTARS in the nebula. A star is STABLE on the MAIN SEQUENCE as long as the OUTWARD FORCE (RADIATING ENERGY) = INWARD FORCE (GRAVITY)
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35 When the star becomes UNSTABLE, and it MOVES OFF THE MAIN SEQUENCE, as it s characteristics change. It starts to DIE by expanding (GIANTS) and then collapsing (DWARFS and BLACK HOLES) LARGER stars are less stable, have shorter life spans, and go out with a bigger show!
36 All stars start main sequence and expand If low to mid-size star mass (like our sun) expands to red giant goes nova and blows off outer expansion zone and is left with core as a white dwarf black dwarf when no energy left so no illumination!
37 All stars start main sequence and expand If starts as, supergiant supernova neutron star (very dense)
38 All stars start main sequence and expand If very high mass star (>10x sun) supergiant supernova black hole (extremely high gravity field that attracts things to it)
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