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The Future of the Universe

by: Alyssa Karounos

The Future of the Universe Astr 1010-100

Marketplace > University of Washington > Astronomy > Astr 1010-100 > The Future of the Universe
Alyssa Karounos
GPA 3.9
Introductory Astronomy 1
Dr. Oliver Fraser

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About this Document

notes that explain: Predict the future size and expansion rate of the universe from measurement in the past
Introductory Astronomy 1
Dr. Oliver Fraser
Class Notes
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This 2 page Class Notes was uploaded by Alyssa Karounos on Friday March 13, 2015. The Class Notes belongs to Astr 1010-100 at University of Washington taught by Dr. Oliver Fraser in Winter2015. Since its upload, it has received 116 views. For similar materials see Introductory Astronomy 1 in Astronomy at University of Washington.


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Date Created: 03/13/15
3 1 115 1 Goals A Predict the future size and expansion rate of the universe from measurement in the past 11 Big Bang Problem 1 A The Cosmic Microwave Background is really smooth B how come any two opposite points in the sky have the same temperature without touching Why are they identical 111 Big Bang Problem 2 A Where do clumps come from B areas of one distances after the big bang C clumps make galaxies but where do they come from D hot spots are in contact with each other E not enough time before recombination for dark matter to clump up this way IV Big Bang Problem 3 A the universe appears to be at B we live exactly enough mass to never expand forever nor to collapse yet C what are the chances of that D if all possibilities are equally likely atness is unlikely V In ation A created to solve the Big Bang problems B spacetime is created time is moving forward C D space is expanding E stuff is created F very quickly the universe expands very quickly like hyper quickly and then goes back to normal expansion VI Fix 1 Horizon A the points were totally in contact before the Big Bang B they were touching in the compressed space C in ation pulled them apart really quickly D expansion of 1040 VII Fix 2 Clumps A Quantum Uncertainty 1 you can t identify a particles momentum and its position at the same time B because of this there will always be hot and cold spots at a subatomic level C then they were in ated to the size of galaxies during the hyper expansion VIII Fix 3 Flat A B The Future A B C IX G H What is Qmass A X P150 pm we don t know the geometry of the universe but if you in ate anything it looks at to us it will be perceived as at because we are in it but that doesn39t mean it is the Hubble plot is velocity to the same unknown place to gure out redshift distances is a challenge standard candle I know how bright it really is and how it appears now I know the distance Super Nova Type la 1 white dwarf sucking at red giant 2 collapses SN are about as bright as their Galaxies Once you get a spectra of a SN you are looking farther back in time than just the galaxy by plotting these supernovae we could out that l the universe is actually expanding faster not slower we have slower expansion in the past data all luminous matter is Qmass 002 since galaxies are 90 dark matter Qmass 02 add dark matter between galaxies Qmass 03 Qmassl is required to cause a at universe dark energy exists because we can see it affecting things but we can39t see it and we don t know much about it Qmass appears very low but we have a cosmological constant an accelerating universe can naturally out of general relativity 1 depends on the value of QA the cosmological constant 2 4 atoms 3 22 Dark Matter 4 74 Dark energy Qmass 25 and 9A 75


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