AaZaK[d 5666778? HH $ @d HHHHff@  d a Footnote TableFootnote**.\t.\t/ - :;,.!?14 `M  `UTOCHeading1Heading2  EquationVariables6 I Y M I J K L  <$lastpagenum> <$monthname> <$daynum>, <$year> "<$monthnum>/<$daynum>/<$shortyear> ;<$monthname> <$daynum>, <$year> <$hour>:<$minute00> <$ampm> "<$monthnum>/<$daynum>/<$shortyear> <$monthname> <$daynum>, <$year>> "<$monthnum>/<$daynum>/<$shortyear>  <$fullfilename>  <$filename>  <$paratext[Title]>  <$paratext[Heading1]>  <$curpagenum>  <$marker1>  <$marker2>  (Continued) + (Sheet <$tblsheetnum> of <$tblsheetcount>) Heading & Page <$paratext> on page<$pagenum> Pagepage<$pagenum>.\ See Heading & Page%See <$paratext> on page<$pagenum>.  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HH5HHl  Pwd5p9HH HH ` 8Is the Universe Flat? ;` :ve X h 1 $Define the following parameter: I  5;The universe is flat if  @W=1 5, i.e. the density of @ 5Mthe universe  @r=r ACRIT 5  @= (5 - 20 )10 B-27 @  5kg/m B3 ` :er p;` : X` =y ELocal group of galaxies:  Cr  =0. C610 D-27 = kg/m D3 pu` : ` C  EW 0.02  Fto  E0.2 ` :+  ` GMa However: ` :Mu% Too big a coincidence that  HW~1 ` :Ne$ Inflation argues that  HW 1 #` :& Galaxy rotations show dark matter @` :  ] ??  3We believe that in fact  ?W=1  3but there is lots of z@ 3dark matter in the universe. HH5HHl  8d5e :neheHH HHte densit ` 8 Creation of the Elements P` 1@; All the raw materials available at  9t  2 1  1sec  m` 5y !Protons, Neutrons, and Electrons ` :27 ` 1, Combine protons + neutrons to form nuclei Ā` 52 1First step is n @+ 5p @ B2 5H @+g e` 5 8But, you also get  @g+ B2 5H @ 5n @+ 5p ` I The deuterium bottleneck  h :la Quickly form  N3 1He and  N4 1He but thats the end \` 5*No stable nuclei with atomic mass  @= 5 y` C*  =Only hydrogen and helium are formed HH5HHl  sitd5Cr;HH ae HHOec!Protonnd ` 8 Particle Creation Epochs ; h : K o` :  OWhenWhatWhy 1Fi` :+>1  Hm :secProtons and <kT H  <m KH <c L2 ` :5 Neutrons @+%` : B` :um: =1 secondElectrons IkT C  Im Pe Ic D2 _` :  |` :& Q  R. . . QNeutronsToo many ` Qes decay hot photons ` : ` :icB 33 minutesn ?+ 3p ? S2 3H ?+g 3Cooler now so ` 3e 4etc... no  ?g+ S2 3H ? 3n ?+ 3p  ` :an e*` :5 210 N5 2  1yearsAtoms 9kT  2  1eV G` :  HH5HHl  Hd5 <HH HHlfic ` 8WPrimordial Abundances ;` 9 H&A major triumph of the Big Bang model X` : u` 5ut7  TYou 5 can calculate the helium mass fraction =1` U <+  :Wait until bottleneck breaks at  <t H 3  :min ` I Neutrons decay into protons! fPfP` Ues'+  :Assume N( L4 :He)=N(n) H/2 `  8) h C  =Find  L in6` :? SS` 9Co'Excellent agreement with observations! . p` :3 ?` :  ` 5 e4 Can also calculate other nuclei (but its harder) ` :  fP` : CMass fraction of  L2 :H H 10 L-4 H  :to H 10 L-5  ffP` :-Mass fraction of  L6 :Li H 10 L-10 *f` : Gf` 9 Agrees well with observation... df` 9(... but the observations are hard, too! HH5HHl   trd6?= THH tnHHpfP eneck br H ` 8Inflationary Cosmology int;` 9fP-A marriage of Particle Physics and Astronomy X` : u` 5 L)Conventional Cosmology: Nagging problems ` =re, Why is the universe so  Visotropic :? 3` = . Why is the universe so  Vhomogeneous :? ` =ut' Why is the universe so  Vflat :? ` =Ma6 Why is there only matter but  Vno antimatter :? ` :fP #` 5ct-The Grand Unification of Particle Physics: @` =$The three quantum mechanical forces ti]` :Electromagnetism hz` : h%Strong (i.e. holds protons together) ` :'Weak (i.e. allows for  Hb- :decay) fPfP =tr9are unified at  IE C 10 D16 = GeV where they fP@ =Tprefer matter over antimatter. fP` : fP` 1VAt  9t 2 10 N-35 2  1sec ( 9kT 2= 1  9E WGUT 1), the universe .fP 1,underwent a phase transition and expanded stKfP@ 1*quantum mechanically at a very high rate. hfP` Xin Inflation HH6BiHHl  o d6b y >t?HH lmaHHf`tt :fP   ` 8onFormation of the Galaxies ;` 9Th0A current hot topic of research and observation X` :ti hu` 5 h+Any model of galaxy formation must explain ` 5 (/ Morphology: Spirals, ellipticals, irregulars ` 5  Superclusters and voids ` 5fP! Connection with CMB anisotropy r` :fP ` :fP*True observational opportunities with HST #` : Look back in time: 1@ f`` :fPJHorizon H  :c H/ :H J0 H  :c  H 12  :Billion years af`` :me n~f` Cig0  =Try to match distributions and morphology f`@ =&of young galaxies to CMB anisotropy f`` : f` Q ,Computer models with General Relativity and y f`@ Qmass distributions f`` ?/  3Do you need Dark Matter to get it right? 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