Outline. I. The Why and What of Inflation II. Gauge fields and inflation, generic setup III. Models within Isotropic BG
|
|
- Emerald Turner
- 5 years ago
- Views:
Transcription
1
2 Outline I. The Why nd Wht of Infltion II. Guge fields nd infltion, generic setup III. Models within Isotropic BG Guge-fltion model Chromo-nturl model IV. Model within Anisotropic BG Infltion with nisotropic hir model Guge-fltion model V. Conclusion
3 Cosmic Microwve Bckground rdition CMB: blckbody rdition with Temperture T=.7 K. This relic rdition the 1 st snpshot of the universe, turns out to be gold mine of cosmologicl informtion!
4 In 199, the Cosmic Bckground Explorer COBE stellite detected cosmologicl fluctutions in the microwve bckground temperture: T 5 ~ 10 T
5
6 013 Plnck Plnck
7 Observtion Vs Vs Stndrd Model Model of of Cosmology Horizon Problem: or universe dominted by P w comoving horizon size is H 1 H w 1 3w w 0 0
8 Observtion Vs Vs Stndrd Model Model of of Cosmology Horizon Problem: or universe dominted by P w comoving horizon size is H 1 H w 0 1 3w w 0 0
9 Observtion Vs Stndrd Model of Cosmology ltness Problem: The RW geometry k 3H 1 k H H 1 H w
10 Observtion Vs Stndrd Model of Cosmology ltness Problem: The RW geometry 3H Now, ssuming d k d ln 1 k 0 k H 0 1 3w 0 H 1 H w Observtions of the CMB nd lrge-scle structure find tht ~ 0! k
11 How Infltion cn solve them? The issue in the stndrd big bng cosmology which leds to these problem is tht: lwys 0 H 1 lwys increses with time!
12 How Infltion cn solve them? The problems in the stndrd big bng cosmology Infltion Ide: 0 There is stge in the erly universe with n ccelerted expnsion: 0 H 1 decreses in the infltionry phse!
13 How Infltion cn solve them? The problems in the stndrd big bng cosmology Infltion Ide: 0 There is stge in the erly universe with n ccelerted expnsion: 0 H 1 decreses in the infltionry phse! Infltion must lst enough for end 0 e 60
14 Wht cuses Infltion? RW metric ds riedmnn equtions dt t dr 1 kr H r d d k 3P ccelertion requires: 3P 0!
15 Slow-roll Infltion In order to ensure enough # e-folds: The Hubble prmeter decreses slowly, nd the universe experiences n pproximtely exponentil infltion. To put this qulittively, we use slow-roll prmeters : H H nd H HH Slow-roll conditions
16 Slow-roll Infltion In order to ensure enough # e-folds: The Hubble prmeter decreses slowly, nd the universe experiences n pproximtely exponentil infltion. To put this qulittively, we use slow-roll prmeters : H H nd H HH Slow-roll conditions 1, 1
17 Meet with Observtions Observtions of CMB: t the time of decoupling, the universe ws very nerly homogeneous with smll inhomogeneties t the level. A nturl strtegy: for ll quntities metric nd mtter fields where Liner perturbtions round the homogeneous bckground: Cosmologicl Perturbtions 10 5
18 Meet with Observtions Observtions of CMB: t the time of decoupling, the universe ws very nerly 10 5 homogeneous with smll inhomogeneties t the level. A nturl strtegy: for ll quntities metric nd mtter fields A A A X t, x X t X t, x, where X A X A t, x A t X t, x Liner perturbtions round the homogeneous bckground: G T Cosmologicl Perturbtions
19 Cosmologicl Perturbtions symmetries of sptilly flt, homogeneous nd isotropic bckground llows for decomposition into sclr, divergence-less vector divergence & trce-less tensor g g S g V g T v T T S T V T T v The equtions of ech prt is independent of the other sectors.
20 Cosmologicl Perturbtions An importnt guge-invrint sclr quntity comoving curvture perturbtion H P Usully vector perturbtions re dmping modes nd unimportnt during infltion. R C 0 0 q h Tensor modes hs polriztions h & without ny prity violting term ij h h h
21 A crucil sttisticl mesure of primordil sclr fluctutions Power spectrum of R, The power spectrum of primordil tensor fluctutions 1 * * 3 s n R R R k k k A k P k k k R k t n t t h t k k k A k P k k * * 3 Sttistics of Cosmologicl Perturbtions
22 A crucil sttisticl mesure of primordil sclr fluctutions Power spectrum of R, The power spectrum of primordil tensor fluctutions 1 * * 3 s n R R R k k k A k P k k k R k t n t t h t k k k A k P k k * * 3 Sttistics of Cosmologicl Perturbtions k k r R t
23 CMB Observtions Current observtions of CMB provide vlues for power spectrum of R, spectrl tilt nd impose n upper bound on tensor to sclr rtio: P n r r R R no evidence of non-gussinity ,, 95%, no running 95%, including running P. A. R. Ade et l. Plnck Collbortion, ``Plnck 013 results. XVI. Cosmologicl prmeters, rxiv: [stro-ph.co].
24 Infltion hs mny reliztions. R. Bouchet: CMB nisotropies, Sttus & Properties
25 Guge ields nd Infltion the role nd consequences of guge fields, theoreticl nd observtionl during infltionry er within Einstein GR with minimlly coupled fields hving vector without the guge symmetry, we expect to hve ghost instbility, so we will NOT consider the vector infltion models. B. Himmetoglu, C. R. Contldi nd M. Peloso, Instbility of nisotropic cosmologicl solutions supported by vector fields, Phys. Rev. Lett
26 Guge ields nd Infltion ds Isotropic Bckground dt e t dx ij i dx j ds Anisotropic Bckground dt e e t ij dx i dx j
27 Guge ields nd Infltion ds Isotropic Bckground dt e t dx ij i dx Guge field vlue on BG j A 0 A 0 e t t Scle fctor
28 Guge ields nd Infltion ds Isotropic Bckground dt e t dx ij i dx Guge field vlue on BG j A 0 A 0 non-abelin Guge field in BG Inflton field e.g. guge-fltion Auxiliry field e.g. chromo-nturl
29 Guge ields in Infltion ds Isotropic Bckground dt e t dx ij i dx Guge field vlue on BG j A 0 A 0 Guge field t the perturbtion level
30 perturbtion level: Guge ields nd Infltion ds Isotropic Bckground dt e t dx ij i dx Guge field vlue on BG j A 0 A 0 g g S g V g T v A A S V A T A T T perfect fluid
31 perturbtion level: Guge ields nd Infltion ds Isotropic Bckground dt e t dx ij i dx Guge field vlue on BG j A 0 A 0 g g S g V g T v A A S V A T A T T perfect fluid
32 Guge ields nd Infltion ds Isotropic Bckground dt e t dx ij i dx j
33 Guge ields nd Infltion ds Anisotropic Bckground dt e e t ij dx i dx j e t t Scle fctor t e ij nisotropy fctor
34 Guge ields nd Infltion ds Anisotropic Bckground dt e e t ij dx i dx Guge field vlue on BG j T T perfect fluid A 0
35 Guge ields nd Infltion Anisotropic Bckground ds dt e e t ij dx i dx j Guge field vlue on BG T T perfect fluid A 0 Anisotropic inerti the metric,. ij is the source of the nisotropies of A. M. nd M. M. Sheikh-Jbbri, Revisiting Cosmic No-Hir Theorem for Infltionry Settings, Phys. Rev. D 85 01
36 Guge ields nd Infltion Anisotropic Bckground ds dt e e t ij dx i dx j Guge field vlue on BG T T perfect fluid A 0 Anisotropic inerti is the source of the nisotropies of the metric, ij. if 0, nisotropies of the metric re dmping exponentilly during slow-roll infltion. A. M. nd M. M. Sheikh-Jbbri, Revisiting Cosmic No-Hir Theorem for Infltionry Settings, Phys. Rev. D 85 01
37 Guge ields nd Infltion Anisotropic Bckground ds dt e e t ij dx i dx j Guge field vlue on BG T T perfect fluid A 0 If 0, then nisotropies cn grow during infltion. Infltion puts n upper bound on the vlue of nisotropy: ij H A. M. nd M. M. Sheikh-Jbbri, Revisiting Cosmic No-Hir Theorem for Infltionry Settings, Phys. Rev. D 85 01
38 Guge ields nd Infltion ds Isotropic Bckground dt e t dx ij i dx j ds Anisotropic Bckground dt e e t ij dx i dx j
39 Isotropic Models with Guge ields Isotropic nd homogenous RW bckground ds non-abelin guge field dt G is ny non-abelin compct group t dx ij i dx Lgrngin of the models 1 L R L m I, A A A gf bc A b T A b A c b where [ T, T b j T b G ] if bc T c
40 Isotropic Models with Guge ields Isotropic nd homogenous RW bckground ds dt Lgrngin of the models 1 L R L m I, t dx ij i dx j f bc bc
41 Isotropic Models with Guge ields In the isotropic nd homogenous RW bckground, with Lgrngin of the form L R L m I,, we hve homogenous nd isotropic solution: 1 A t 0 t i 0 i nd I t I A. M. nd M. M. Sheikh-Jbbri, Guge-fltion: Infltion rom Non-Abelin Guge ields, to pper in PRB, rxiv: [hep-ph]. A. M. nd M. M. Sheikh-Jbbri, Non-Abelin Guge ield Infltion, Phys. Rev. D 84, [rxiv: [hep-ph]].
42 Guge-fltion Model n pproprite choice for non-abelin guge field infltion S d 4 x R g Tr A is non-abelin SU guge field A. M. nd M. M. Sheikh-Jbbri, Guge-fltion: Infltion rom Non-Abelin Guge ields, rxiv: [hep-ph], to pper in PLB. A. M. nd M. M. Sheikh-Jbbri, Non-Abelin Guge ield Infltion, Phys. Rev. D 84, [rxiv: [hep-ph]].
43 Guge-fltion Model n pproprite choice for non-abelin guge field infltion S Yng-Mills term Tr d 4 x R g term 1 4 YM 3P YM P 384 Tr YM YM
44 Guge-fltion Model n pproprite choice for non-abelin guge field infltion homogenous nd isotropic nstz reduced Lgrngin density R g x d S H g g H red L i t t i 0 0 A
45 Guge-fltion Model n pproprite choice for non-abelin guge field infltion homogenous nd isotropic nstz reduced Lgrngin density Slow-roll prmeters R g x d S i t t i 0 0 A H g g H red L 1 H g
46 Guge-fltion Model reduced Lgrngin density Lred H g g H is the effective inflton field which evolves slowly during infltion nd fter the end of infltion, it strts oscillting. 1 g H , i i 10, g.510, A. M. nd M. M. Sheikh-Jbbri, Non-Abelin Guge ield Infltion, Phys. Rev. D 84, [rxiv: [hep-ph]].
47 Guge-fltion Model vs. stndrd single sclr model A. M. nd M. M. Sheikh-Jbbri, Non-Abelin Guge ield Infltion, Phys. Rev. D 84, [rxiv: [hep-ph]].
48 Guge-fltion nd Prity Violtion of Grvittionl Wves e P P R R PL P L g H A. M. nd M. M. Sheikh-Jbbri, Non-Abelin Guge ield Infltion, Phys. Rev. D 84, [rxiv: [hep-ph]].
49 Guge-fltion Model & WMAP results A. M. nd M. M. Sheikh-Jbbri, Non-Abelin Guge ield Infltion, Phys. Rev. D 84, [rxiv: [hep-ph]].
50 Guge-fltion Model & Plnck results 95%, no running P. A. R. Ade et l. Plnck Collbortion, ``Plnck 013 results. XVI. Cosmologicl prmeters, rxiv: [stro-ph.co].
51 Guge-fltion Model & Plnck results 95%, including running P. A. R. Ade et l. Plnck Collbortion, ``Plnck 013 results. XVI. Cosmologicl prmeters, rxiv: [stro-ph.co].
52 Chromo-nturl Model Lgrngin density of the Chromo-nturl model: S d x R g cos f 8 f 4 A is n xion field 0, f is non-abelin SU guge field P. Adshed, M. Wymn, Chromo-Nturl Infltion, Phys. Rev. Lett. 108, M. M. Sheikh-Jbbri, Guge-fltion Vs Chromo-Nturl Infltion, Phys. Lett. B P. Adshed, M. Wymn, Guge-fltion trjectories in Chromo-Nturl Infltion, rxiv: [hep-th].
53 Chromo-nturl Model Lgrngin density of the Chromo-nturl model: S d x A R g 1 4 is n xion field cos 0, f is non-abelin SU guge field f 8 f 4 Tr topologicl term P. Adshed, M. Wymn, Chromo-Nturl Infltion, Phys. Rev. Lett. 108, M. M. Sheikh-Jbbri, Guge-fltion Vs Chromo-Nturl Infltion, Phys. Lett. B P. Adshed, M. Wymn, Guge-fltion trjectories in Chromo-Nturl Infltion, rxiv: [hep-th].
54 Chromo-nturl Model Lgrngin density of the Chromo-nturl model: S d x R g 1 4 Yng-Mills term Axion field term cos f 8 f 4 YM 3P YM P 3 YM YM 4 V 1 cos, f YM
55 Lgrngin density of the Chromo-nturl model: Inserting the isotropic nd homogenous nstz The reduced effective ction Chromo-nturl Model 8 cos f f R g x d S i t t i 0 0 A 3 cos H f g f g H red L
56 Chromo-nturl Model L The reduced effective ction: red g H g 1 cos f f H During the slow-roll infltion: H cos 3 f nd is the inflton field, while infltion possible. 3 4 sin 3gH f mkes the slow-roll
57 Chromo-nturl Model 6 4 The clssicl trjectories with g 10, 400, 710,, f 10 strted from different xion initil vlues, χ0. In both pnels, the solid ornge lines, the dshed red lines nd the dotted brown lines correspond to χ0/f vlues equl to 3π/4, π/ nd 0.01, respectively.
58 Guge ields nd Infltion ds Isotropic Bckground dt e t dx ij i dx j ds Anisotropic Bckground dt e e t ij dx i dx j
59 Anisotropic Infltion Model Anisotropic Bckground Lgrngin density of the Anisotropic Infltion model: is n sclr field is n Abelin U1 guge field V f R g x d S A 4 dz dy e dx e e dt ds t t t / c f e
60 Anisotropic Infltion Model H H the time evlution of nisotropy for vrious c with respect to number of e-folds is shown. M. A. Wtnbe, S. Knno nd J. Sod, Infltionry Universe with Anisotropic Hir, Phys. Rev. Lett. 10, [rxiv: [hep-th]].
61 Summry nd Outlook It is possible to hve non-abelin guge fields in the RW bckground s the inflton field or n uxiliry field Guge fields leds to very rich cosmic perturbtion theory e.g. chirl GW nd non-zero power spectrum for sclr nisotropic inerti Anisotropic infltion nd the growth of nisotropies during infltion violtion of cosmic no-hir conjecture
62
4 The dynamical FRW universe
4 The dynmicl FRW universe 4.1 The Einstein equtions Einstein s equtions G µν = T µν (7) relte the expnsion rte (t) to energy distribution in the universe. On the left hnd side is the Einstein tensor which
More information4- Cosmology - II. introduc)on to Astrophysics, C. Bertulani, Texas A&M-Commerce 1
4- Cosmology - II introduc)on to Astrophysics, C. Bertulni, Texs A&M-Commerce 1 4.1 - Solutions of Friedmnn Eqution As shown in Lecture 3, Friedmnn eqution is given by! H 2 = # " & % 2 = 8πG 3 ρ k 2 +
More informationBig Bang/Inflationary Picture
Big Bng/Infltionry Picture big bng infltionry epoch rdition epoch mtter epoch drk energy epoch DISJOINT Gret explntory power: horizon fltness monopoles entropy Gret predictive power: Ω totl = 1 nerly scle-invrint
More informationYou may not start to read the questions printed on the subsequent pages until instructed to do so by the Invigilator.
MATHEMATICAL TRIPOS Prt III Mondy 12 June, 2006 9 to 11 PAPER 55 ADVANCED COSMOLOGY Attempt TWO questions. There re THREE questions in totl. The questions crry equl weight. STATIONERY REQUIREMENTS Cover
More informationListening for primordial gravitational waves
Listening for primordil grvittionl wves V(φ) Vlerie Domcke PC Pris Rencontres de Moriond 4.03.016 bsed on rxiv:1603.0187 with Pierre Binétruy Muro Pieroni neutrinos grvittionl wves photons Primordil vcuum
More informationA5682: Introduction to Cosmology Course Notes. 4. Cosmic Dynamics: The Friedmann Equation. = GM s
4. Cosmic Dynmics: The Friedmnn Eqution Reding: Chpter 4 Newtonin Derivtion of the Friedmnn Eqution Consider n isolted sphere of rdius R s nd mss M s, in uniform, isotropic expnsion (Hubble flow). The
More information-S634- Journl of the Koren Physicl Society, Vol. 35, August 999 structure with two degrees of freedom. The three types of structures re relted to the
Journl of the Koren Physicl Society, Vol. 35, August 999, pp. S633S637 Conserved Quntities in the Perturbed riedmnn World Model Ji-chn Hwng Deprtment of Astronomy nd Atmospheric Sciences, Kyungpook Ntionl
More information+ x 2 dω 2 = c 2 dt 2 +a(t) [ 2 dr 2 + S 1 κx 2 /R0
Notes for Cosmology course, fll 2005 Cosmic Dynmics Prelude [ ds 2 = c 2 dt 2 +(t) 2 dx 2 ] + x 2 dω 2 = c 2 dt 2 +(t) [ 2 dr 2 + S 1 κx 2 /R0 2 κ (r) 2 dω 2] nd x = S κ (r) = r, R 0 sin(r/r 0 ), R 0 sinh(r/r
More informationWMAP satellite. 16 Feb Feb Feb 2012
16 Feb 2012 21 Feb 2012 23 Feb 2012 è Announcements è Problem 5 (Hrtle 18.3). Assume V * is nonreltivistic. The reltivistic cse requires more complicted functions. è Outline è WMAP stellite è Dipole nisotropy
More informationThe Cosmology of the Nonsymmetric Theory of Gravitation (NGT)
The Cosmology of the Nonsymmetric Theory of Grvittion () By Tomislv Proopec Bsed on stro-ph/050389 nd on unpublished wor with Wessel Vlenburg (mster s student) Bonn, 8 Aug 005 Introduction: Historicl remrs
More informationSummer School on Cosmology July Inflation - Lecture 1. M. Sasaki Yukawa Institute, Kyoto
354-1 Summer School on Cosmology 16-7 July 01 Infltion - Lecture 1 M. Ssi Yuw Institute, Kyoto Summer school on cosmology ICT, 16-18 July 01 Miso Ssi Yuw Institute for Theoreticl hysics Kyoto University
More informationDiluting the inflationary axion fluctuation by stronger QCD in the early Universe
Diluting the infltionry xion fluctution by stronger QCD in the erly Universe K. Choi, E. J. Chun, S. H. Im, KSJ rxiv: 1505.00306 Kwng Sik JEONG Pusn Ntionl University CosKASI Drk Mtter Workshop 2015 9-11
More informationInflation Cosmology. Ch 06 - Initial Conditions. Korea University Eunil Won. Korea U/Dept. Physics, Prof. Eunil Won (All rights are reserved)
Infltion Cosmology Ch 6 - Initil Conditions Kore University Eunil Won 1 The Einstein-Boltzmnn Equtions t Erly Times For nine first-order differentil equtions for the nine perturbtion vribles, we need initil
More informationNonlocal Gravity and Structure in the Universe
Nonlocl rvity nd Structure in the Universe Sohyun Prk Penn Stte University Co-uthor: Scott Dodelson Bsed on PRD 87 (013) 04003, 109.0836, PRD 90 (014) 000000, 1310.439 August 5, 014 Chicgo, IL Cosmo 014
More informationDomain Wall Start to Inflation with Contributions to Off Diagonal GR Stress Energy Tensor Terms
Domin Wll Strt to Infltion with Contributions to Off Digonl GR Stress Energy Tensor Terms Andrew Beckwith Chongqing University Deprtment of Physics; e mil: beckwith@uh.edu Chongqing, PRC, 000 Abstrct We
More informationImproper Integrals, and Differential Equations
Improper Integrls, nd Differentil Equtions October 22, 204 5.3 Improper Integrls Previously, we discussed how integrls correspond to res. More specificlly, we sid tht for function f(x), the region creted
More informationarxiv:astro-ph/ v1 5 Apr 2005
Slinky Infltion Griel Brenoim Deprtment de Físic Teòric, Universitt de Vlènci, Crrer Dr. Moliner 50, E-4600 Burjssot (Vlènci), Spin Joseph Lykken Theoreticl Physics Deprtment, Fermi Ntionl Accelertor Lortory,
More information1.1. Linear Constant Coefficient Equations. Remark: A differential equation is an equation
1 1.1. Liner Constnt Coefficient Equtions Section Objective(s): Overview of Differentil Equtions. Liner Differentil Equtions. Solving Liner Differentil Equtions. The Initil Vlue Problem. 1.1.1. Overview
More informationToday in Astronomy 142: general relativity and the Universe
Tody in Astronomy 14: generl reltivity nd the Universe The Robertson- Wlker metric nd its use. The Friedmnn eqution nd its solutions. The ges nd ftes of flt universes The cosmologicl constnt. Glxy cluster
More informationAstro 4PT Lecture Notes Set 1. Wayne Hu
Astro 4PT Lecture Notes Set 1 Wyne Hu References Reltivistic Cosmologicl Perturbtion Theory Infltion Drk Energy Modified Grvity Cosmic Microwve Bckground Lrge Scle Structure Brdeen (1980), PRD 22 1882
More informationMassachusetts Institute of Technology Quantum Mechanics I (8.04) Spring 2005 Solutions to Problem Set 6
Msschusetts Institute of Technology Quntum Mechnics I (8.) Spring 5 Solutions to Problem Set 6 By Kit Mtn. Prctice with delt functions ( points) The Dirc delt function my be defined s such tht () (b) 3
More informationP 3 (x) = f(0) + f (0)x + f (0) 2. x 2 + f (0) . In the problem set, you are asked to show, in general, the n th order term is a n = f (n) (0)
1 Tylor polynomils In Section 3.5, we discussed how to pproximte function f(x) round point in terms of its first derivtive f (x) evluted t, tht is using the liner pproximtion f() + f ()(x ). We clled this
More informationThe Power Spectrum for a Multi-Component Inflaton to Second-Order Corrections in the Slow-Roll Expansion
KAIST-TH 00/01 The Power Spectrum for Multi-Component Inflton to Second-Order Corrections in the Slow-Roll Expnsion Jin-Ook Gong Ewn D. Stewrt Deprtment of Physics, KAIST, Dejeon 05-701, South Kore Februry
More informationData Assimilation. Alan O Neill Data Assimilation Research Centre University of Reading
Dt Assimiltion Aln O Neill Dt Assimiltion Reserch Centre University of Reding Contents Motivtion Univrite sclr dt ssimiltion Multivrite vector dt ssimiltion Optiml Interpoltion BLUE 3d-Vritionl Method
More informationM.Gasperini. Dipartimento di Fisica Teorica, Via P.Giuria 1, Turin, Italy, and INFN, Sezione di Torino, Turin, Italy. and. G.
CERN-TH.778/94 Dilton Production in String Cosmology M.Gsperini Diprtimento di Fisic Teoric, Vi P.Giuri, 05 Turin, Itly, nd INFN, Sezione di Torino, Turin, Itly nd G.Venezino Theory Division, CERN, Genev,
More informationarxiv:gr-qc/ v1 14 Mar 2000
The binry blck-hole dynmics t the third post-newtonin order in the orbitl motion Piotr Jrnowski Institute of Theoreticl Physics, University of Bi lystok, Lipow 1, 15-2 Bi lystok, Polnd Gerhrd Schäfer Theoretisch-Physiklisches
More informationarxiv: v1 [gr-qc] 8 Apr 2009
On the Stbility of Sttic Ghost Cosmologies rxiv:0904.1340v1 [gr-qc] 8 Apr 2009 John D. Brrow 1 nd Christos G. Tsgs 2 1 DAMTP, Centre for Mthemticl Sciences University of Cmbridge, Wilberforce Rod, Cmbridge
More informationGauge Invariance and. Frame Independence in Cosmology
Guge Invrince nd Frme Independence in Cosmology Cover design by Mrten vn Gent ISBN: 978-90-8891-693-9 Printed by: Proefschriftmken.nl Uitgeverij BOXPress Published by: Uitgeverij BOXPress, s-hertogenbosch
More informationState space systems analysis (continued) Stability. A. Definitions A system is said to be Asymptotically Stable (AS) when it satisfies
Stte spce systems nlysis (continued) Stbility A. Definitions A system is sid to be Asymptoticlly Stble (AS) when it stisfies ut () = 0, t > 0 lim xt () 0. t A system is AS if nd only if the impulse response
More information1B40 Practical Skills
B40 Prcticl Skills Comining uncertinties from severl quntities error propgtion We usully encounter situtions where the result of n experiment is given in terms of two (or more) quntities. We then need
More informationSUMMER KNOWHOW STUDY AND LEARNING CENTRE
SUMMER KNOWHOW STUDY AND LEARNING CENTRE Indices & Logrithms 2 Contents Indices.2 Frctionl Indices.4 Logrithms 6 Exponentil equtions. Simplifying Surds 13 Opertions on Surds..16 Scientific Nottion..18
More information. Double-angle formulas. Your answer should involve trig functions of θ, and not of 2θ. sin 2 (θ) =
Review of some needed Trig. Identities for Integrtion. Your nswers should be n ngle in RADIANS. rccos( 1 ) = π rccos( - 1 ) = 2π 2 3 2 3 rcsin( 1 ) = π rcsin( - 1 ) = -π 2 6 2 6 Cn you do similr problems?
More informationClassical Mechanics. From Molecular to Con/nuum Physics I WS 11/12 Emiliano Ippoli/ October, 2011
Clssicl Mechnics From Moleculr to Con/nuum Physics I WS 11/12 Emilino Ippoli/ October, 2011 Wednesdy, October 12, 2011 Review Mthemtics... Physics Bsic thermodynmics Temperture, idel gs, kinetic gs theory,
More informationHigher Checklist (Unit 3) Higher Checklist (Unit 3) Vectors
Vectors Skill Achieved? Know tht sclr is quntity tht hs only size (no direction) Identify rel-life exmples of sclrs such s, temperture, mss, distnce, time, speed, energy nd electric chrge Know tht vector
More informationSection 4.8. D v(t j 1 ) t. (4.8.1) j=1
Difference Equtions to Differentil Equtions Section.8 Distnce, Position, nd the Length of Curves Although we motivted the definition of the definite integrl with the notion of re, there re mny pplictions
More informationBypassing no-go theorems for consistent interactions in gauge theories
Bypssing no-go theorems for consistent interctions in guge theories Simon Lykhovich Tomsk Stte University Suzdl, 4 June 2014 The tlk is bsed on the rticles D.S. Kprulin, S.L.Lykhovich nd A.A.Shrpov, Consistent
More informationarxiv: v1 [astro-ph.co] 16 Feb 2010
Collpse of Smll-Scle Density Perturbtions during Preheting in Single Field Infltion Krsten Jedmzi Lbortoire de Physique Théorique et Astroprticules, UMR 507-CNRS, Université de Montpellier II, F-34095
More informationDepartment of Physical Sciences Embry-Riddle Aeronautical University 600 S. Clyde Morris Boulevard Daytona Beach, FL 32114, USA
Journl of Applied Mthemtics nd Computtion (JAMC), 017, 1(1), 1-7 http://www.hillpublisher.org/journl/jmc ISSN Online:576-0645 ISSN Print:576-0653 Using Hubble Prmeter Mesurements to Find Constrints on
More informationMath 360: A primitive integral and elementary functions
Mth 360: A primitive integrl nd elementry functions D. DeTurck University of Pennsylvni October 16, 2017 D. DeTurck Mth 360 001 2017C: Integrl/functions 1 / 32 Setup for the integrl prtitions Definition:
More informationProperties of Integrals, Indefinite Integrals. Goals: Definition of the Definite Integral Integral Calculations using Antiderivatives
Block #6: Properties of Integrls, Indefinite Integrls Gols: Definition of the Definite Integrl Integrl Clcultions using Antiderivtives Properties of Integrls The Indefinite Integrl 1 Riemnn Sums - 1 Riemnn
More informationPh2b Quiz - 1. Instructions
Ph2b Winter 217-18 Quiz - 1 Due Dte: Mondy, Jn 29, 218 t 4pm Ph2b Quiz - 1 Instructions 1. Your solutions re due by Mondy, Jnury 29th, 218 t 4pm in the quiz box outside 21 E. Bridge. 2. Lte quizzes will
More informationA027 Uncertainties in Local Anisotropy Estimation from Multi-offset VSP Data
A07 Uncertinties in Locl Anisotropy Estimtion from Multi-offset VSP Dt M. Asghrzdeh* (Curtin University), A. Bon (Curtin University), R. Pevzner (Curtin University), M. Urosevic (Curtin University) & B.
More informationPhysics 201 Lab 3: Measurement of Earth s local gravitational field I Data Acquisition and Preliminary Analysis Dr. Timothy C. Black Summer I, 2018
Physics 201 Lb 3: Mesurement of Erth s locl grvittionl field I Dt Acquisition nd Preliminry Anlysis Dr. Timothy C. Blck Summer I, 2018 Theoreticl Discussion Grvity is one of the four known fundmentl forces.
More information5.7 Improper Integrals
458 pplictions of definite integrls 5.7 Improper Integrls In Section 5.4, we computed the work required to lift pylod of mss m from the surfce of moon of mss nd rdius R to height H bove the surfce of the
More informationWe partition C into n small arcs by forming a partition of [a, b] by picking s i as follows: a = s 0 < s 1 < < s n = b.
Mth 255 - Vector lculus II Notes 4.2 Pth nd Line Integrls We begin with discussion of pth integrls (the book clls them sclr line integrls). We will do this for function of two vribles, but these ides cn
More informationMath 1B, lecture 4: Error bounds for numerical methods
Mth B, lecture 4: Error bounds for numericl methods Nthn Pflueger 4 September 0 Introduction The five numericl methods descried in the previous lecture ll operte by the sme principle: they pproximte the
More informationRecitation 3: More Applications of the Derivative
Mth 1c TA: Pdric Brtlett Recittion 3: More Applictions of the Derivtive Week 3 Cltech 2012 1 Rndom Question Question 1 A grph consists of the following: A set V of vertices. A set E of edges where ech
More information4 7x =250; 5 3x =500; Read section 3.3, 3.4 Announcements: Bell Ringer: Use your calculator to solve
Dte: 3/14/13 Objective: SWBAT pply properties of exponentil functions nd will pply properties of rithms. Bell Ringer: Use your clcultor to solve 4 7x =250; 5 3x =500; HW Requests: Properties of Log Equtions
More informationarxiv:astro-ph/ v4 7 Jul 2006
Cosmologicl models with Gurzdyn-Xue drk energy rxiv:stro-ph/0601073v4 7 Jul 2006 G. V. Vereshchgin nd G. Yegorin ICRANet P.le dell Repubblic 10 I65100 Pescr Itly nd ICRA Dip. Fisic Univ. L Spienz P.le
More informationA 3D Brans-Dicke Theory Model
Interntionl Journl of Physics 06 Vol 4 No 3 64-68 Avilble online t http://pubssciepubcom/ijp/4/3/4 Science nd Eduction Publishing DOI:069/ijp-4-3-4 A 3D Brns-Dicke Theory Model T G do Prdo * E F Reis M
More informationTHERMAL EXPANSION COEFFICIENT OF WATER FOR VOLUMETRIC CALIBRATION
XX IMEKO World Congress Metrology for Green Growth September 9,, Busn, Republic of Kore THERMAL EXPANSION COEFFICIENT OF WATER FOR OLUMETRIC CALIBRATION Nieves Medin Hed of Mss Division, CEM, Spin, mnmedin@mityc.es
More informationTerminal Velocity and Raindrop Growth
Terminl Velocity nd Rindrop Growth Terminl velocity for rindrop represents blnce in which weight mss times grvity is equl to drg force. F 3 π3 ρ L g in which is drop rdius, g is grvittionl ccelertion,
More informationMath 100 Review Sheet
Mth 100 Review Sheet Joseph H. Silvermn December 2010 This outline of Mth 100 is summry of the mteril covered in the course. It is designed to be study id, but it is only n outline nd should be used s
More informationMAT187H1F Lec0101 Burbulla
Chpter 6 Lecture Notes Review nd Two New Sections Sprint 17 Net Distnce nd Totl Distnce Trvelled Suppose s is the position of prticle t time t for t [, b]. Then v dt = s (t) dt = s(b) s(). s(b) s() is
More informationarxiv:astro-ph/ v2 16 May 2005
Growth of perturbtions in drk mtter coupled with quintessence Tomi Koivisto Helsinki Institute of Physics,FIN-4 Helsinki, Finlnd nd Deprtment of Physics, University of Oslo, N-36 Oslo, Norwy (Dted: September,
More informationu( t) + K 2 ( ) = 1 t > 0 Analyzing Damped Oscillations Problem (Meador, example 2-18, pp 44-48): Determine the equation of the following graph.
nlyzing Dmped Oscilltions Prolem (Medor, exmple 2-18, pp 44-48): Determine the eqution of the following grph. The eqution is ssumed to e of the following form f ( t) = K 1 u( t) + K 2 e!"t sin (#t + $
More informationMath 42 Chapter 7 Practice Problems Set B
Mth 42 Chpter 7 Prctice Problems Set B 1. Which of the following functions is solution of the differentil eqution dy dx = 4xy? () y = e 4x (c) y = e 2x2 (e) y = e 2x (g) y = 4e2x2 (b) y = 4x (d) y = 4x
More informationFundamental Cosmology with EUCLID
Fundmentl Cosmology with EUCLID Rphel, Euclid, The School of Athens, Rome Luc Amendol University of Heidelberg nd ESTEC INAF/Rom 009 The reconstruction of spce-time geometry with Euclid Drk mtter nd infltion
More informationThe Fundamental Theorem of Calculus, Particle Motion, and Average Value
The Fundmentl Theorem of Clculus, Prticle Motion, nd Averge Vlue b Three Things to Alwys Keep In Mind: (1) v( dt p( b) p( ), where v( represents the velocity nd p( represents the position. b (2) v ( dt
More informationThe Periodically Forced Harmonic Oscillator
The Periodiclly Forced Hrmonic Oscilltor S. F. Ellermeyer Kennesw Stte University July 15, 003 Abstrct We study the differentil eqution dt + pdy + qy = A cos (t θ) dt which models periodiclly forced hrmonic
More informationFactors affecting the phonation threshold pressure and frequency
3SC Fctors ffecting the phontion threshold pressure nd frequency Zhoyn Zhng School of Medicine, University of Cliforni Los Angeles, CA, USA My, 9 57 th ASA Meeting, Portlnd, Oregon Acknowledgment: Reserch
More informationRead section 3.3, 3.4 Announcements:
Dte: 3/1/13 Objective: SWBAT pply properties of exponentil functions nd will pply properties of rithms. Bell Ringer: 1. f x = 3x 6, find the inverse, f 1 x., Using your grphing clcultor, Grph 1. f x,f
More informationHow can we approximate the area of a region in the plane? What is an interpretation of the area under the graph of a velocity function?
Mth 125 Summry Here re some thoughts I ws hving while considering wht to put on the first midterm. The core of your studying should be the ssigned homework problems: mke sure you relly understnd those
More informationLECTURE 14. Dr. Teresa D. Golden University of North Texas Department of Chemistry
LECTURE 14 Dr. Teres D. Golden University of North Texs Deprtment of Chemistry Quntittive Methods A. Quntittive Phse Anlysis Qulittive D phses by comprison with stndrd ptterns. Estimte of proportions of
More informationThe Active Universe. 1 Active Motion
The Active Universe Alexnder Glück, Helmuth Hüffel, Sš Ilijić, Gerld Kelnhofer Fculty of Physics, University of Vienn helmuth.hueffel@univie.c.t Deprtment of Physics, FER, University of Zgreb ss.ilijic@fer.hr
More informationLecture 21: Order statistics
Lecture : Order sttistics Suppose we hve N mesurements of sclr, x i =, N Tke ll mesurements nd sort them into scending order x x x 3 x N Define the mesured running integrl S N (x) = 0 for x < x = i/n for
More informationarxiv: v1 [astro-ph.co] 20 Dec 2018
Preprint 24 December 28 Compiled using MNRAS LATEX style file v3. A new method to probe the mss density nd the cosmologicl constnt using configurtion entropy Biswjit Pndey nd Biswjit Ds Deprtment of Physics,
More informationVorticity. curvature: shear: fluid elements moving in a straight line but at different speeds. t 1 t 2. ATM60, Shu-Hua Chen
Vorticity We hve previously discussed the ngulr velocity s mesure of rottion of body. This is suitble quntity for body tht retins its shpe but fluid cn distort nd we must consider two components to rottion:
More informationA. Limits - L Hopital s Rule ( ) How to find it: Try and find limits by traditional methods (plugging in). If you get 0 0 or!!, apply C.! 1 6 C.
A. Limits - L Hopitl s Rule Wht you re finding: L Hopitl s Rule is used to find limits of the form f ( x) lim where lim f x x! c g x ( ) = or lim f ( x) = limg( x) = ". ( ) x! c limg( x) = 0 x! c x! c
More informationf(x) dx, If one of these two conditions is not met, we call the integral improper. Our usual definition for the value for the definite integral
Improper Integrls Every time tht we hve evluted definite integrl such s f(x) dx, we hve mde two implicit ssumptions bout the integrl:. The intervl [, b] is finite, nd. f(x) is continuous on [, b]. If one
More informationUNIT 1 FUNCTIONS AND THEIR INVERSES Lesson 1.4: Logarithmic Functions as Inverses Instruction
Lesson : Logrithmic Functions s Inverses Prerequisite Skills This lesson requires the use of the following skills: determining the dependent nd independent vribles in n exponentil function bsed on dt from
More information1 1D heat and wave equations on a finite interval
1 1D het nd wve equtions on finite intervl In this section we consider generl method of seprtion of vribles nd its pplictions to solving het eqution nd wve eqution on finite intervl ( 1, 2. Since by trnsltion
More informationPhys 6321 Final Exam - Solutions May 3, 2013
Phys 6321 Finl Exm - Solutions My 3, 2013 You my NOT use ny book or notes other thn tht supplied with this test. You will hve 3 hours to finish. DO YOUR OWN WORK. Express your nswers clerly nd concisely
More informationJack Simons, Henry Eyring Scientist and Professor Chemistry Department University of Utah
1. Born-Oppenheimer pprox.- energy surfces 2. Men-field (Hrtree-Fock) theory- orbitls 3. Pros nd cons of HF- RHF, UHF 4. Beyond HF- why? 5. First, one usully does HF-how? 6. Bsis sets nd nottions 7. MPn,
More informationFINALTERM EXAMINATION 2011 Calculus &. Analytical Geometry-I
FINALTERM EXAMINATION 011 Clculus &. Anlyticl Geometry-I Question No: 1 { Mrks: 1 ) - Plese choose one If f is twice differentible function t sttionry point x 0 x 0 nd f ''(x 0 ) > 0 then f hs reltive...
More informationSufficient condition on noise correlations for scalable quantum computing
Sufficient condition on noise correltions for sclble quntum computing John Presill, 2 Februry 202 Is quntum computing sclble? The ccurcy threshold theorem for quntum computtion estblishes tht sclbility
More informationRiemann Sums and Riemann Integrals
Riemnn Sums nd Riemnn Integrls Jmes K. Peterson Deprtment of Biologicl Sciences nd Deprtment of Mthemticl Sciences Clemson University August 26, 2013 Outline 1 Riemnn Sums 2 Riemnn Integrls 3 Properties
More informationNon-Linear & Logistic Regression
Non-Liner & Logistic Regression If the sttistics re boring, then you've got the wrong numbers. Edwrd R. Tufte (Sttistics Professor, Yle University) Regression Anlyses When do we use these? PART 1: find
More information( dg. ) 2 dt. + dt. dt j + dh. + dt. r(t) dt. Comparing this equation with the one listed above for the length of see that
Arc Length of Curves in Three Dimensionl Spce If the vector function r(t) f(t) i + g(t) j + h(t) k trces out the curve C s t vries, we cn mesure distnces long C using formul nerly identicl to one tht we
More information1.2. Linear Variable Coefficient Equations. y + b "! = a y + b " Remark: The case b = 0 and a non-constant can be solved with the same idea as above.
1 12 Liner Vrible Coefficient Equtions Section Objective(s): Review: Constnt Coefficient Equtions Solving Vrible Coefficient Equtions The Integrting Fctor Method The Bernoulli Eqution 121 Review: Constnt
More informationMath 8 Winter 2015 Applications of Integration
Mth 8 Winter 205 Applictions of Integrtion Here re few importnt pplictions of integrtion. The pplictions you my see on n exm in this course include only the Net Chnge Theorem (which is relly just the Fundmentl
More informationScientific notation is a way of expressing really big numbers or really small numbers.
Scientific Nottion (Stndrd form) Scientific nottion is wy of expressing relly big numbers or relly smll numbers. It is most often used in scientific clcultions where the nlysis must be very precise. Scientific
More informationThermodynamics of the early universe, v.4
Thermodynmics of the erly universe, v.4 A physicl description of the universe is possible when it is ssumed to be filled with mtter nd rdition which follows the known lws of physics. So fr there is no
More informationRiemann Sums and Riemann Integrals
Riemnn Sums nd Riemnn Integrls Jmes K. Peterson Deprtment of Biologicl Sciences nd Deprtment of Mthemticl Sciences Clemson University August 26, 203 Outline Riemnn Sums Riemnn Integrls Properties Abstrct
More informationThe 5D Standing Wave Braneworld With Real Scalar Field
The 5D Stnding Wve Brneworld With Rel Sclr Field rxiv:0.9v [hep-th] 0 Dec 0 Merb Gogbershvili Andronikshvili Institute of Physics, 6 Tmrshvili Street, Tbilisi 077, Georgi nd Jvkhishvili Stte University,
More informationInterpreting Integrals and the Fundamental Theorem
Interpreting Integrls nd the Fundmentl Theorem Tody, we go further in interpreting the mening of the definite integrl. Using Units to Aid Interprettion We lredy know tht if f(t) is the rte of chnge of
More informationON INFLATION AND TORSION IN COSMOLOGY
Vol. 36 (005) ACTA PHYSICA POLONICA B No 10 ON INFLATION AND TORSION IN COSMOLOGY Christin G. Böhmer The Erwin Schrödinger Interntionl Institute for Mthemticl Physics Boltzmnngsse 9, A-1090 Wien, Austri
More informationMath 116 Final Exam April 26, 2013
Mth 6 Finl Exm April 26, 23 Nme: EXAM SOLUTIONS Instructor: Section:. Do not open this exm until you re told to do so. 2. This exm hs 5 pges including this cover. There re problems. Note tht the problems
More informationName Solutions to Test 3 November 8, 2017
Nme Solutions to Test 3 November 8, 07 This test consists of three prts. Plese note tht in prts II nd III, you cn skip one question of those offered. Some possibly useful formuls cn be found below. Brrier
More informationInflation Cosmology. Ch 02 - The smooth, expanding universe. Korea University Eunil Won
Infltion Cosmology Ch 02 - The smooth, expnding universe Kore University Eunil Won From now on, we use = c = k B = The metric Generl Reltivity - in 2-dimensionl plne, the invrint distnce squred is (dx)
More informationDisclaimer: This Final Exam Study Guide is meant to help you start studying. It is not necessarily a complete list of everything you need to know.
Disclimer: This is ment to help you strt studying. It is not necessrily complete list of everything you need to know. The MTH 33 finl exm minly consists of stndrd response questions where students must
More informationLecture 5. Today: Motion in many dimensions: Circular motion. Uniform Circular Motion
Lecture 5 Physics 2A Olg Dudko UCSD Physics Tody: Motion in mny dimensions: Circulr motion. Newton s Lws of Motion. Lws tht nswer why questions bout motion. Forces. Inerti. Momentum. Uniform Circulr Motion
More information221B Lecture Notes WKB Method
Clssicl Limit B Lecture Notes WKB Method Hmilton Jcobi Eqution We strt from the Schrödinger eqution for single prticle in potentil i h t ψ x, t = [ ] h m + V x ψ x, t. We cn rewrite this eqution by using
More informationStuff You Need to Know From Calculus
Stuff You Need to Know From Clculus For the first time in the semester, the stuff we re doing is finlly going to look like clculus (with vector slnt, of course). This mens tht in order to succeed, you
More informationA REVIEW OF CALCULUS CONCEPTS FOR JDEP 384H. Thomas Shores Department of Mathematics University of Nebraska Spring 2007
A REVIEW OF CALCULUS CONCEPTS FOR JDEP 384H Thoms Shores Deprtment of Mthemtics University of Nebrsk Spring 2007 Contents Rtes of Chnge nd Derivtives 1 Dierentils 4 Are nd Integrls 5 Multivrite Clculus
More informationarxiv:hep-th/ v1 1 Oct 2002
rxiv:hep-th/0210004v1 1 Oct 2002 EXACT STANDARD MODEL STRUCTURES FROM INTERSECTING BRANES C. KOKORELIS Deprtmento de Físic Teóric C-XI nd Instituto de Físic Teóric C-XVI Universidd Autónom de Mdrid, Cntoblnco,
More informationREGULARITY OF NONLOCAL MINIMAL CONES IN DIMENSION 2
EGULAITY OF NONLOCAL MINIMAL CONES IN DIMENSION 2 OVIDIU SAVIN AND ENICO VALDINOCI Abstrct. We show tht the only nonlocl s-miniml cones in 2 re the trivil ones for ll s 0, 1). As consequence we obtin tht
More informationESCI 343 Atmospheric Dynamics II Lesson 14 Inertial/slantwise Instability
ESCI 343 Atmospheric Dynmics II Lesson 14 Inertil/slntwise Instbility Reference: An Introduction to Dynmic Meteorology (3 rd edition), J.R. Holton Atmosphere-Ocen Dynmics, A.E. Gill Mesoscle Meteorology
More informationChapter 7 Notes, Stewart 8e. 7.1 Integration by Parts Trigonometric Integrals Evaluating sin m x cos n (x) dx...
Contents 7.1 Integrtion by Prts................................... 2 7.2 Trigonometric Integrls.................................. 8 7.2.1 Evluting sin m x cos n (x)......................... 8 7.2.2 Evluting
More informationJ. Ruz, J. K. Vogel, M. J. Pivovaroff, G. Brown, D. Smith, H. Hudson, B. Grefenstette, L. Glesener and H. Iain
J. Ruz, J. K. Vogel, M. J. Pivovroff, G. Brown, D. Smith, H. Hudson, B. Grefenstette, L. Glesener nd H. Iin August 10 th 2017 Columbus, OH LLNL-PRES-736641 This work ws performed under the uspices of the
More information