ISU PHY 102 - Stars (4 pages)

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Lecture number:
Lecture Note
Illinois State University
Phy 102 - Atoms to Galaxies

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PHY 102 1st Edition Outline of Last Lecture I Einstein a Equation for spacetime II Shape of the Universe III Einstein GTR and the Universe a Einstein s equation of general relativity IV Friedmann s Universe a Total Energy b Einstein s Equations c E mc2 V VI Atomic Emission Spectra Hubble s Relationship a Distance of nebulas b Hubble s law for Galaxies VII Abbe Georges Lamaitre Outline of Current Lecture i Individual Star Organization ii Aging of Stars iii Variable Stars iv Clusters These notes represent a detailed interpretation of the professor s lecture GradeBuddy is best used as a supplement to your own notes not as a substitute v vi Nebulae SNR Neutron Stars Black Holes Current Lecture I Individual Stars are organized a By mass b By lifetime i Stars range in efficiency in use of gas can have the same amount of gas but use it in a different time period c Age II When stars age a They can literally explode b Some will become white dwarves neutron stars and others c Which one they will become is dependent on the mass III Binary Singular Stars a Both are equally as common b Two stars that orbit around each other instead of one being the center of a galaxy c Some people believe that our sun has a companion star that passes every 30 million years linked to extinction patterns IV Variable Stars a Large magellanic cloud b From the southern hemisphere the milky way looks like two chunks As the period of variability gets longer the brightness increases luminosity The difference between absolute brightness and apparent brightness has to do with distance Period of variability V Clusters two types a Open loose clusters of stars leftover from formation of clouds dust b Globular closely grouped stars gravitational pull is extremely strong i 13 8 billion years old cluster stars bright turnoff blue VI VII red ii Younger stars will be on the main sequenc iii Older the stars are the more likely they are to peel off of the curve c We know how much fuel they have and how fast they

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