![Page 1: Ay 127, Winter 2017: The Early Universegeorge/ay127/Ay127_SGD_Lec05.pdf · • MaFer-an5maFer asymmetry: probes the baryogenesis era, t ~ 10-6 sec, z ~ 1012, but only in sugges5ng](https://reader036.vdocuments.us/reader036/viewer/2022081406/5f0fd4d47e708231d4461975/html5/thumbnails/1.jpg)
Ay 127, Winter 2017: The Early Universe
![Page 2: Ay 127, Winter 2017: The Early Universegeorge/ay127/Ay127_SGD_Lec05.pdf · • MaFer-an5maFer asymmetry: probes the baryogenesis era, t ~ 10-6 sec, z ~ 1012, but only in sugges5ng](https://reader036.vdocuments.us/reader036/viewer/2022081406/5f0fd4d47e708231d4461975/html5/thumbnails/2.jpg)
TheKeyIdeas• Pushingbackwardin5metowardstheBigBang,theuniversewas
ho<eranddenserinafairlypredictablemanner(asidefromsurprising“glitches”suchastheinfla5on…)
• Atanygiven5me,thetemperaturetranslatesintoacharacteris5cmassofpar5cles,whichdominatethatepoch:theUniverseastheul5mateaccelerator?
• Astheenergiesincrease,differentphysicalregimesanddifferentfundamentalinterac5onscomeintoplay
• ThecloserwegettotheBigBang(i.e.,furtherawayfromtheexperimentallyprobedregime),thelesscertainthephysics:theearlyUniverseasthelaboratoryofphysicsbeyondthestandardmodel?
• Ourextrapola5onsmustbreakdownbytheepochof~10-43sec~Plack5me,wherequantumgravitymustbeimportant
![Page 3: Ay 127, Winter 2017: The Early Universegeorge/ay127/Ay127_SGD_Lec05.pdf · • MaFer-an5maFer asymmetry: probes the baryogenesis era, t ~ 10-6 sec, z ~ 1012, but only in sugges5ng](https://reader036.vdocuments.us/reader036/viewer/2022081406/5f0fd4d47e708231d4461975/html5/thumbnails/3.jpg)
TheCosmicThermalHistory
(from M. Turner)
The Planck Era
… on a logarithmic time axis - a theorist’s delight!
![Page 4: Ay 127, Winter 2017: The Early Universegeorge/ay127/Ay127_SGD_Lec05.pdf · • MaFer-an5maFer asymmetry: probes the baryogenesis era, t ~ 10-6 sec, z ~ 1012, but only in sugges5ng](https://reader036.vdocuments.us/reader036/viewer/2022081406/5f0fd4d47e708231d4461975/html5/thumbnails/4.jpg)
AnotherSchema5cOutline:
![Page 5: Ay 127, Winter 2017: The Early Universegeorge/ay127/Ay127_SGD_Lec05.pdf · • MaFer-an5maFer asymmetry: probes the baryogenesis era, t ~ 10-6 sec, z ~ 1012, but only in sugges5ng](https://reader036.vdocuments.us/reader036/viewer/2022081406/5f0fd4d47e708231d4461975/html5/thumbnails/5.jpg)
SomeKeyMomentsintheThermalHistoryoftheUniverse:
• Planckera,t~10-43sec:quantumgravity,…???…• Infla5on,t~10-33sec:vacuumphasetransi5on,exponen5al
expansion• GrandUnifica5on,t~10-32sec:strongandelectroweak
interac5onssplit• Baryogenesis,t~10-6sec:quark-hadrontransi5on• Nucleosynthesis,t~1msto3min:D,He,Li,Beform• Radia5ontomaFerdominancetransi5on,t~105yr:structure
beginstoform• Recombina5on,t~380,000yr:hydrogenbecomesneutral,
CMBRreleased,darkagesbegin• Reioniza5on,t~0.3-1Gyr:firstgalaxiesandQSOsreionizethe
universe,thecosmicrenaissance
![Page 6: Ay 127, Winter 2017: The Early Universegeorge/ay127/Ay127_SGD_Lec05.pdf · • MaFer-an5maFer asymmetry: probes the baryogenesis era, t ~ 10-6 sec, z ~ 1012, but only in sugges5ng](https://reader036.vdocuments.us/reader036/viewer/2022081406/5f0fd4d47e708231d4461975/html5/thumbnails/6.jpg)
t < 10-10 s T > 1015 K GUT
10-10 < t <10-4 s 1015>T>1012K e+, e-,quarks,γ,ν
t ~ 10-4 s T ~ 1012K Quarks-> n, p µ+µ−> νµ,νµ
10-10 < t <10-4 s 1012>T>1010K e+, e-, n, p, γ,νe
t ~ 0.01 s T ~ 1011K assymetry in n, p
t ~ 4 s T ~ 5x109K e+, e-−> νe,ν
e n->p+e-+νe
t ~ 100 s T ~ 104K nucleosynthesis
t ~ 1011 s T ~ 16 500 K Matter domination
t ~ 1013 s T ~ 3000 K Decoupling
ThermalHistoryoftheEarlyUniverseAge Temperature Processes
![Page 7: Ay 127, Winter 2017: The Early Universegeorge/ay127/Ay127_SGD_Lec05.pdf · • MaFer-an5maFer asymmetry: probes the baryogenesis era, t ~ 10-6 sec, z ~ 1012, but only in sugges5ng](https://reader036.vdocuments.us/reader036/viewer/2022081406/5f0fd4d47e708231d4461975/html5/thumbnails/7.jpg)
EmpiricalEvidence• TheCMBR:probestherecombina5onera,t~105yr,z~1100,
basedonawellunderstoodatomicandmacroscopicphysics
• Nucleosynthesis:probesthet~10-3-102secera,z~109,comparethemodelpredic5onswithobservedabundancesofthelightestelements,basedonawellunderstoodnuclearphysics
• MaFer-an5maFerasymmetry:probesthebaryogenesisera,t~10-6sec,z~1012,butonlyinsugges5ngthatsomesymmetrybreakingdidoccur
• Predic5onsoftheinfla5onaryscenario:flatness,uniformityofCMBR,absenceofmonopoles,therighttypeofdensityfluctua5onspectrum-itallsupportstheideathatinfla5ondidhappen,butdoesnotsayalotaboutitsdetailedphysics
• Cosmologicalobserva5onscanindicateorconstrainphysicswelloutsidethereachoflaboratoryexperiments
![Page 8: Ay 127, Winter 2017: The Early Universegeorge/ay127/Ay127_SGD_Lec05.pdf · • MaFer-an5maFer asymmetry: probes the baryogenesis era, t ~ 10-6 sec, z ~ 1012, but only in sugges5ng](https://reader036.vdocuments.us/reader036/viewer/2022081406/5f0fd4d47e708231d4461975/html5/thumbnails/8.jpg)
CMBRandtheRecombina5onEraPrediction of CMB is trivial in Hot Big Bang model: • Hot, ionised initial state should produce thermal radiation • Photons decouple when universe stops being ionised (last
scattering) • Expansion by factor a cools a
blackbody spectrum from T to T/a • Therefore we should now see
a cool blackbody background – Alpher and Herman, 1949,
“A temperature now of the order of 5 K”
– Dicke et al., 1965, “<40 K” • note that the Gamow, Alpher
& Herman prediction had been nearly forgotten at this time!
![Page 9: Ay 127, Winter 2017: The Early Universegeorge/ay127/Ay127_SGD_Lec05.pdf · • MaFer-an5maFer asymmetry: probes the baryogenesis era, t ~ 10-6 sec, z ~ 1012, but only in sugges5ng](https://reader036.vdocuments.us/reader036/viewer/2022081406/5f0fd4d47e708231d4461975/html5/thumbnails/9.jpg)
TheCMBRDisoveries
CH
CN
Firstseenin1941(yes,1941!)
• Linesseeninstellarspectraiden5fiedasinterstellarCHandCN(AndrewMcKellar,theory;WalterAdams,spectroscopy)
• Comparisonoflinesfromdifferentrota5onalstatesgave“rota5onaltemperature”of2-3K
• Unfortunately Gamow et al. did not have known about this • Hoyle made the connection in 1950:
"[the Big Bang model] would lead to a temperature of the radiation at present maintained throughout the whole of space much greater than McKellar's determination for some regions within the Galaxy."
• So, Penzias & Wilson made the recognized discovery in 1964
![Page 10: Ay 127, Winter 2017: The Early Universegeorge/ay127/Ay127_SGD_Lec05.pdf · • MaFer-an5maFer asymmetry: probes the baryogenesis era, t ~ 10-6 sec, z ~ 1012, but only in sugges5ng](https://reader036.vdocuments.us/reader036/viewer/2022081406/5f0fd4d47e708231d4461975/html5/thumbnails/10.jpg)
DiscoveryoftheCosmicMicrowaveBackground(CMBR):ADirectEvidence
fortheBigBang
Arno Penzias & Robert Wilson (1965)
Nobel Prize, 1978
![Page 11: Ay 127, Winter 2017: The Early Universegeorge/ay127/Ay127_SGD_Lec05.pdf · • MaFer-an5maFer asymmetry: probes the baryogenesis era, t ~ 10-6 sec, z ~ 1012, but only in sugges5ng](https://reader036.vdocuments.us/reader036/viewer/2022081406/5f0fd4d47e708231d4461975/html5/thumbnails/11.jpg)
TheCMBRSpectrum:ANearlyPerfectBlackbody Residuals from the BB
strongly limit possible energy injection (e.g., from hypothetical decaying DM particles) during and after the recombination - no new physics here…
![Page 12: Ay 127, Winter 2017: The Early Universegeorge/ay127/Ay127_SGD_Lec05.pdf · • MaFer-an5maFer asymmetry: probes the baryogenesis era, t ~ 10-6 sec, z ~ 1012, but only in sugges5ng](https://reader036.vdocuments.us/reader036/viewer/2022081406/5f0fd4d47e708231d4461975/html5/thumbnails/12.jpg)
TemperatureofRecombina5onMean photon energy: TkE B3~
Ionisation energy of H: eV 6.13=E
Photoionisation Temperature: K500003
eV 6.13==
BkT
But there are many more photons than H ions: pnn 910≈γ
!"#$
%&−∝> TkEEn
Bexp)(γBoltzmann distribution:
( )K2500
10ln93eV 6.13
==Bk
T
Thus, the T can be lower and have enough photons with high enough energies to ionize H!
So the actual T of recombination is:
And thus, zrec ~ 1100
![Page 13: Ay 127, Winter 2017: The Early Universegeorge/ay127/Ay127_SGD_Lec05.pdf · • MaFer-an5maFer asymmetry: probes the baryogenesis era, t ~ 10-6 sec, z ~ 1012, but only in sugges5ng](https://reader036.vdocuments.us/reader036/viewer/2022081406/5f0fd4d47e708231d4461975/html5/thumbnails/13.jpg)
TheExtentofRecombina5onThis phase transition (ionized to neutral gas) has a finite thickness: most of the plasma recombines before the last scattering, which is the CMBR photosphere we see
![Page 14: Ay 127, Winter 2017: The Early Universegeorge/ay127/Ay127_SGD_Lec05.pdf · • MaFer-an5maFer asymmetry: probes the baryogenesis era, t ~ 10-6 sec, z ~ 1012, but only in sugges5ng](https://reader036.vdocuments.us/reader036/viewer/2022081406/5f0fd4d47e708231d4461975/html5/thumbnails/14.jpg)
IntotheNucleosynthesisEra• Inthepre-nucleosynthesisuniverse,theradia5onproduces
pairsofelectronsandpositrons,aswellasprotonsandan5protons,neutronsandan5neutrons,andtheycanannihilate;e+e-reac5onsproduceelectronneutrinos(νe)andan5neutrinos:
e-+e+←→νe+νee-+p←→n+νe,νe+p←→n+e+n←→p+e-+νee-+e+←→γ+γ
• Thisoccursun5lthetemperaturedropstoT~1010K,t~1sec• Inequilibriumtherewillslightlymoreprotonsthanneutrons
sincetheneutronmassisslightly(1.293MeV)larger• Thisleadstoanasymmetrybetweenprotonsandneutrons…
![Page 15: Ay 127, Winter 2017: The Early Universegeorge/ay127/Ay127_SGD_Lec05.pdf · • MaFer-an5maFer asymmetry: probes the baryogenesis era, t ~ 10-6 sec, z ~ 1012, but only in sugges5ng](https://reader036.vdocuments.us/reader036/viewer/2022081406/5f0fd4d47e708231d4461975/html5/thumbnails/15.jpg)
AsymmetryinNeutron/ProtonRa5oMass difference between n and p causes an asymmetry via reactions:
It is slightly easier (requires less energy) to produce p than n:
Thus, once e+, e- annihilation occurs only neutrons can decay
−+↔+ epn eν
epen ν+↔+ +
eepn ν++→ −
eenp ν++→ +
⎟⎠
⎞⎜⎝
⎛−+
=s1013
exp16.0~ tNN
NXpn
nn
at T~ 1012 K, n/p = 0.985
We can calculate the equilibrium ratio of n to p via the Boltzmann equation,
The n/p ratio is “frozen” at the value it had at when T= 1010 K , n/p = 0.223, i.e., for every 1000 protons, there are 223 neutrons
![Page 16: Ay 127, Winter 2017: The Early Universegeorge/ay127/Ay127_SGD_Lec05.pdf · • MaFer-an5maFer asymmetry: probes the baryogenesis era, t ~ 10-6 sec, z ~ 1012, but only in sugges5ng](https://reader036.vdocuments.us/reader036/viewer/2022081406/5f0fd4d47e708231d4461975/html5/thumbnails/16.jpg)
BigBangNucleosynthesis(BBNS)Free neutrons are unstable to beta decay, with mean lifetime = 886 sec, n → p + e- + νe . This destroys ~ 25% of them, before they can combine with the protons
γ+↔+ Hpn 2
nHeHH +↔+ 322
pHnHe +↔+ 33
nHeHH +↔+ 423
When the temperature drops to ~ 109 K (t=230s), neutrons and protons combine to form deuterium, and then helium: Note that these are not the same reactions as in stars (the pp chain)!
Photons break the newly created nuclei, but as the temperature drops, the photodissociation stops
At t ~ 103 sec and T < 3Í108 K, the density also becomes too low for fusion, and BBN ends. This is another “freeze-out”, as no new nuclei are created and none are destroyed
![Page 17: Ay 127, Winter 2017: The Early Universegeorge/ay127/Ay127_SGD_Lec05.pdf · • MaFer-an5maFer asymmetry: probes the baryogenesis era, t ~ 10-6 sec, z ~ 1012, but only in sugges5ng](https://reader036.vdocuments.us/reader036/viewer/2022081406/5f0fd4d47e708231d4461975/html5/thumbnails/17.jpg)
The actual reactions network is a tad more complicated… But the simplified version is pretty close, and conveys the important parts of the story
![Page 18: Ay 127, Winter 2017: The Early Universegeorge/ay127/Ay127_SGD_Lec05.pdf · • MaFer-an5maFer asymmetry: probes the baryogenesis era, t ~ 10-6 sec, z ~ 1012, but only in sugges5ng](https://reader036.vdocuments.us/reader036/viewer/2022081406/5f0fd4d47e708231d4461975/html5/thumbnails/18.jpg)
StableMassGapsinthePeriodicTable
1H
2H
3He
4He
6Li
7Li
9Be
No stable nuclei
Since there are no stable mass-5 nuclides, combining He and tritium to get Li requires overcoming the Coulomb repulsion. So almost all of the neutrons end up in He instead!
There is another gap at mass-8, so BBN ends with Li, with only trace amounts of Be produced
![Page 19: Ay 127, Winter 2017: The Early Universegeorge/ay127/Ay127_SGD_Lec05.pdf · • MaFer-an5maFer asymmetry: probes the baryogenesis era, t ~ 10-6 sec, z ~ 1012, but only in sugges5ng](https://reader036.vdocuments.us/reader036/viewer/2022081406/5f0fd4d47e708231d4461975/html5/thumbnails/19.jpg)
TheEvolu5onofAbundancesinBBNS
![Page 20: Ay 127, Winter 2017: The Early Universegeorge/ay127/Ay127_SGD_Lec05.pdf · • MaFer-an5maFer asymmetry: probes the baryogenesis era, t ~ 10-6 sec, z ~ 1012, but only in sugges5ng](https://reader036.vdocuments.us/reader036/viewer/2022081406/5f0fd4d47e708231d4461975/html5/thumbnails/20.jpg)
BigBangNucleosynthesisEnd
Thus neutron/proton asymmetry caused by their mass difference and the beta decay of neutrons determines primordial abundance of He and other light elements
At this point n/p ratio has dropped to ~ 0.14. The excess protons account for about 75% of the total mass, and since essentially all neutrons are incorporated into He nuclei, the predicted primordial He abundance is ~ 25% - about as measured
Because all the neutrons are tied up in He, its abundance is not sensitive to the matter density. In contrast, the abundances of other elements produces in the early universe, D, 3He, and 7Li are dependent on the amount of baryonic matter in the universe
The universe expanded to rapidly to build up heavier elements!
![Page 21: Ay 127, Winter 2017: The Early Universegeorge/ay127/Ay127_SGD_Lec05.pdf · • MaFer-an5maFer asymmetry: probes the baryogenesis era, t ~ 10-6 sec, z ~ 1012, but only in sugges5ng](https://reader036.vdocuments.us/reader036/viewer/2022081406/5f0fd4d47e708231d4461975/html5/thumbnails/21.jpg)
BBNSPredic5ons• TheBBNSmakesdetailedpredic5onsoftheabundancesof
lightelements:2D,3He,4He,7Li,8Be
• Thesearegenerallygivenasafunc5onofthebaryontophotonra5oη=nn/nγ,usuallydefinedinunitsof1010,anddirectlyrelatedtothebaryondensityΩb:η10=1010(nn/nγ)=274Ωbh2
• Astheuniverseevolvesηispreserved,sothatwhatweobservetodayshouldreflectthecondi5onsintheearlyuniverse
• Comparisonwithobserva5ons(consistentamongthedifferentelements)gives:
• ThisisinaspectacularlygoodagreementwiththevaluefromtheCMBfluctua5ons:
€
Ωbaryonsh2 = 0.021→ 0.025
€
Ωbaryonsh2 = 0.024 ± 0.001
![Page 22: Ay 127, Winter 2017: The Early Universegeorge/ay127/Ay127_SGD_Lec05.pdf · • MaFer-an5maFer asymmetry: probes the baryogenesis era, t ~ 10-6 sec, z ~ 1012, but only in sugges5ng](https://reader036.vdocuments.us/reader036/viewer/2022081406/5f0fd4d47e708231d4461975/html5/thumbnails/22.jpg)
BBNSPredic5ons4He: the higher the density, the more of it is made ➙
2D, 3He: easily burned into 4He, so abundances are lower at higher densities ➙
7Li: … complicated ➙
Boxes indicate observed values
![Page 23: Ay 127, Winter 2017: The Early Universegeorge/ay127/Ay127_SGD_Lec05.pdf · • MaFer-an5maFer asymmetry: probes the baryogenesis era, t ~ 10-6 sec, z ~ 1012, but only in sugges5ng](https://reader036.vdocuments.us/reader036/viewer/2022081406/5f0fd4d47e708231d4461975/html5/thumbnails/23.jpg)
Helium-4Measurements• Heisalsoproducedin
stars,butthis“secondary”abundanceisexpectedtocorrelatewithabundancesofothernucleosynthe5cproducts,e.g.,oxygen
• Observe 4He from recombination lines in extragalactic HII regions in low-metallicity starforming galaxies
• The intercept at the zero oxygen abundance should represent the primordial (BBNS) value
• The result is: YBBNS = 0.238 +/- 0.005
![Page 24: Ay 127, Winter 2017: The Early Universegeorge/ay127/Ay127_SGD_Lec05.pdf · • MaFer-an5maFer asymmetry: probes the baryogenesis era, t ~ 10-6 sec, z ~ 1012, but only in sugges5ng](https://reader036.vdocuments.us/reader036/viewer/2022081406/5f0fd4d47e708231d4461975/html5/thumbnails/24.jpg)
DeuteriumMeasurements
€
DH
= 2.74 ×10−5
Deuterium is easily destroyed in stars, and there is no known astrophysical process where it can be created in large amounts after the BBNS
Thus, we need to measure it in a “pristine” environment, e.g., in QSO absorption line systems
It is a tricky measurement and it requires high resolution spectra from 8-10 m class telescopes
The result is:
![Page 25: Ay 127, Winter 2017: The Early Universegeorge/ay127/Ay127_SGD_Lec05.pdf · • MaFer-an5maFer asymmetry: probes the baryogenesis era, t ~ 10-6 sec, z ~ 1012, but only in sugges5ng](https://reader036.vdocuments.us/reader036/viewer/2022081406/5f0fd4d47e708231d4461975/html5/thumbnails/25.jpg)
BBNSandPar5clePhysicsBBNS predictions also depend on the number of lepton
(neutrino) families. Indeed, only 3 are allowed:
![Page 26: Ay 127, Winter 2017: The Early Universegeorge/ay127/Ay127_SGD_Lec05.pdf · • MaFer-an5maFer asymmetry: probes the baryogenesis era, t ~ 10-6 sec, z ~ 1012, but only in sugges5ng](https://reader036.vdocuments.us/reader036/viewer/2022081406/5f0fd4d47e708231d4461975/html5/thumbnails/26.jpg)
TheIdeaofInfla5on• AlanGuth(1980);precursors:D.Kazanas,A.Starobinsky• Explainsanumberoffundamentalcosmologicalproblems:
flatness,horizon,originofstructure,absenceoftopologicaldefects…
A. Guth A. Linde A. Starobinsky
• Developed further by P. Steinhardt, A. Albrecht, A. Linde, and many others
A page from Guth’s notebook
![Page 27: Ay 127, Winter 2017: The Early Universegeorge/ay127/Ay127_SGD_Lec05.pdf · • MaFer-an5maFer asymmetry: probes the baryogenesis era, t ~ 10-6 sec, z ~ 1012, but only in sugges5ng](https://reader036.vdocuments.us/reader036/viewer/2022081406/5f0fd4d47e708231d4461975/html5/thumbnails/27.jpg)
TheInfla5onaryScenarioItsolves3keyproblemsoftheBigBangcosmology:1. Theflatnessproblem:whyistheuniversesocloseto
beingflattoday?2. Thehorizonproblem:howcomestheCMBRisso
uniform?3. Themonopoleproblem:wherearethecopious
amountsofmagne5cmonopolespredictedtoexistintheBBcosmology?
…ItalsoaccountsnaturallyfortheobservedpowerspectrumoftheiniCaldensityperturbaCons
…Itpredictsasimilar,scale-invariantspectrumforthecosmicgravita5onalwavebackground
…Anditimpliesamuch,much(!)biggeruniversethantheobservableone
![Page 28: Ay 127, Winter 2017: The Early Universegeorge/ay127/Ay127_SGD_Lec05.pdf · • MaFer-an5maFer asymmetry: probes the baryogenesis era, t ~ 10-6 sec, z ~ 1012, but only in sugges5ng](https://reader036.vdocuments.us/reader036/viewer/2022081406/5f0fd4d47e708231d4461975/html5/thumbnails/28.jpg)
TheFlatnessProblem( )
)()(1
)()()(1 22
020
20
22
2
tatHH
RtatHkct Ω−
=−=Ω−
3m0
4r0
2
0
)(aaH
tH Ω+
Ω=⎟⎟
⎠
⎞⎜⎜⎝
⎛
The expanding universe evolves away from Ωtot = 1:
This creates an enormous fine-tuning problem: the early universe must have been remarkably close to Ωtot = 1 in order to have Ωtot ~ 1 today !
(from N. Wright)
![Page 29: Ay 127, Winter 2017: The Early Universegeorge/ay127/Ay127_SGD_Lec05.pdf · • MaFer-an5maFer asymmetry: probes the baryogenesis era, t ~ 10-6 sec, z ~ 1012, but only in sugges5ng](https://reader036.vdocuments.us/reader036/viewer/2022081406/5f0fd4d47e708231d4461975/html5/thumbnails/29.jpg)
TheHorizonProblemConsiderma<er-onlyuniverse:• HorizondistancedH(t)=3ct• Scalefactora(t)=(t/t0)2/3
• Thereforehorizonexpandsfasterthantheuniverse,sonew”objectsareconstantlycomingintoview
ConsiderCMBR:• Itdecouplesat1+z~1000• i.e.,tCMB=t0/104.5
• ThendH(tCMB)=3ct0/104.5
• Nowthishasexpandedbyafactorof1000to3ct0/101.5
• Buthorizondistancenowis3ct0• Soanglesubtendedonskybyone
CMBhorizondistanceisonly~2°
➙ Patches of CMB sky > 2° apart should not be causally connected!
0
0.5
1
1.5
2
2.5
3
3.5
0 0.25 0.5 0.75 1
t/t0
d/ct horizon
distance
distance to object at dhor for a =0.1
distance to object at dhor for a =1.0
![Page 30: Ay 127, Winter 2017: The Early Universegeorge/ay127/Ay127_SGD_Lec05.pdf · • MaFer-an5maFer asymmetry: probes the baryogenesis era, t ~ 10-6 sec, z ~ 1012, but only in sugges5ng](https://reader036.vdocuments.us/reader036/viewer/2022081406/5f0fd4d47e708231d4461975/html5/thumbnails/30.jpg)
CMBRisUniformto∆T/T~10-6Yettheprojectedsizeofthepar5clehorizonatthedecouplingwas~2°-theseregionswerecausallydisconnected-sohowcome?
![Page 31: Ay 127, Winter 2017: The Early Universegeorge/ay127/Ay127_SGD_Lec05.pdf · • MaFer-an5maFer asymmetry: probes the baryogenesis era, t ~ 10-6 sec, z ~ 1012, but only in sugges5ng](https://reader036.vdocuments.us/reader036/viewer/2022081406/5f0fd4d47e708231d4461975/html5/thumbnails/31.jpg)
TheMonopoleProblem• Magne5cmonopolesarebelievedtobeaninevitableconsequenceofGrandUnifica5onTheories(GUTs)– Point-liketopologicaldefectsarisingduringthephasetransi5onwhenthestrongandtheelectroweakforcesdecouple
• Expectenormousnumbersofthem– Mass~1016mp;dominateallotherma<erdensitybyafactorof~1012andthusclosetheuniverseanddriveittoaBigCrunchalong5meago…
• Notobserved!So,wherearethey?
![Page 32: Ay 127, Winter 2017: The Early Universegeorge/ay127/Ay127_SGD_Lec05.pdf · • MaFer-an5maFer asymmetry: probes the baryogenesis era, t ~ 10-6 sec, z ~ 1012, but only in sugges5ng](https://reader036.vdocuments.us/reader036/viewer/2022081406/5f0fd4d47e708231d4461975/html5/thumbnails/32.jpg)
Infla5onaryUniverseScenario• IfthereisaTheoryofEverything(TOE)thatunifiesallfourforces
itwillbreakspontaneouslyatthePlanck5me(t~10-43sec)intothegravita5onandaunifiedversionofthemagne5c,electroweak,andstrongforces–aGrandUnifiedTheory(GUT)
• TheGUTwillholdun5lT~1028K,ort~10-34sec.Atthispointtheuniverseenteredaperiodof“falsevacuum”:theenergylevelhigherthanthelowest,“ground”state
• SymmetrybreakinginGUTtheoriesisassociatedwithmassiveHiggsbosons,whicharequantaofascalarfieldthathasanassociatedpoten5alwhichdescribestheenergyofthefield
• Thefalsevacuumisametastablestate,withit’svacuumenergyac5ngasa“nega5vepressure”causingtheuniversetoexpandexponen5allyasit“rollsdownthescalarfield”
![Page 33: Ay 127, Winter 2017: The Early Universegeorge/ay127/Ay127_SGD_Lec05.pdf · • MaFer-an5maFer asymmetry: probes the baryogenesis era, t ~ 10-6 sec, z ~ 1012, but only in sugges5ng](https://reader036.vdocuments.us/reader036/viewer/2022081406/5f0fd4d47e708231d4461975/html5/thumbnails/33.jpg)
Infla5onWithaScalarField• Needpoten5alUwithbroadnearlyflatplateaunearφ=0• Thisisthemetastablefalsevacuum
U
ö
Potential U(φ) of a scalar field φ
φ < = <=
Inflation Reheating
• Inflation occurs as φ moves slowly away from 0
• It stops at drop to minimum U - the true vacuum
• Decay of inflaton field φ at this point reheats universe, producing photons, quarks, etc. - all of the matter/energy content of the universe is created in this process
• This is equivalent to latent heat of a phase transition
False vacuum
True vacuum
![Page 34: Ay 127, Winter 2017: The Early Universegeorge/ay127/Ay127_SGD_Lec05.pdf · • MaFer-an5maFer asymmetry: probes the baryogenesis era, t ~ 10-6 sec, z ~ 1012, but only in sugges5ng](https://reader036.vdocuments.us/reader036/viewer/2022081406/5f0fd4d47e708231d4461975/html5/thumbnails/34.jpg)
TheCosmicInfla5onRecall that the energy density of the physical vacuum is described as the cosmological constant. If this is the dominant density term, the Friedmann Eqn. is:
The solution is obviously:
In the model where the GUT phase transition drives the inflation, the net expansion factor is:
The density parameter evolves as:
Thus:
![Page 35: Ay 127, Winter 2017: The Early Universegeorge/ay127/Ay127_SGD_Lec05.pdf · • MaFer-an5maFer asymmetry: probes the baryogenesis era, t ~ 10-6 sec, z ~ 1012, but only in sugges5ng](https://reader036.vdocuments.us/reader036/viewer/2022081406/5f0fd4d47e708231d4461975/html5/thumbnails/35.jpg)
TheInfla5onaryScenario
Standard Big Bang
Inflationary Period
The universe inflates by > 40 orders of magnitude!
… and then the standard expansion resumes
![Page 36: Ay 127, Winter 2017: The Early Universegeorge/ay127/Ay127_SGD_Lec05.pdf · • MaFer-an5maFer asymmetry: probes the baryogenesis era, t ~ 10-6 sec, z ~ 1012, but only in sugges5ng](https://reader036.vdocuments.us/reader036/viewer/2022081406/5f0fd4d47e708231d4461975/html5/thumbnails/36.jpg)
Infla5onSolvestheFlatnessProblem
As the universe inflates, the local curvature effects become negligible in comparison to the vastly increased “global” radius of curvature: the universe becomes extremely close to flat locally (which is the observable region now). Thus, at the end of the inflation, Ω = 1 ± ε
![Page 37: Ay 127, Winter 2017: The Early Universegeorge/ay127/Ay127_SGD_Lec05.pdf · • MaFer-an5maFer asymmetry: probes the baryogenesis era, t ~ 10-6 sec, z ~ 1012, but only in sugges5ng](https://reader036.vdocuments.us/reader036/viewer/2022081406/5f0fd4d47e708231d4461975/html5/thumbnails/37.jpg)
Infla5onSolvestheHorizonProblemRegions of the universe which were causally disconnected at the end of the inflation used to be connected before the inflation - and thus in a thermal equilibrium
Note that the inflationary expansion is superluminal: the space can expand much faster than c
![Page 38: Ay 127, Winter 2017: The Early Universegeorge/ay127/Ay127_SGD_Lec05.pdf · • MaFer-an5maFer asymmetry: probes the baryogenesis era, t ~ 10-6 sec, z ~ 1012, but only in sugges5ng](https://reader036.vdocuments.us/reader036/viewer/2022081406/5f0fd4d47e708231d4461975/html5/thumbnails/38.jpg)
Infla5onandStructureForma5on• UncertaintyPrinciplemeansthatinquantummechanics
vacuumconstantlyproducestemporarypar5cle-an5par5clepairs– Thiscreatesminutedensityfluctua5ons
– Infla5onblowstheseuptomacroscopicsize
– Theybecometheseedsforstructureforma5on
• Expectthemassspectrumofthesedensityfluctua5onstobeapproximatelyscaleinvariant
– Thisisindeedasobserved!– Nota“proof”ofinfla5on,butawelcomeconsistencytest
![Page 39: Ay 127, Winter 2017: The Early Universegeorge/ay127/Ay127_SGD_Lec05.pdf · • MaFer-an5maFer asymmetry: probes the baryogenesis era, t ~ 10-6 sec, z ~ 1012, but only in sugges5ng](https://reader036.vdocuments.us/reader036/viewer/2022081406/5f0fd4d47e708231d4461975/html5/thumbnails/39.jpg)
TheInfla5onasaPhaseTransi5onThe universe undergoes a phase transition from a state of a false vacuum, to a ground state; this releases enormous amounts of energy (“latent heat”) which drives an exponential expansion
Regions of non-inflating universe are created through the nucleation of bubbles of true vacuum. When two such bubbles collide, the vast energy of the bubble walls is converted into the particles. This process is called reheating
![Page 40: Ay 127, Winter 2017: The Early Universegeorge/ay127/Ay127_SGD_Lec05.pdf · • MaFer-an5maFer asymmetry: probes the baryogenesis era, t ~ 10-6 sec, z ~ 1012, but only in sugges5ng](https://reader036.vdocuments.us/reader036/viewer/2022081406/5f0fd4d47e708231d4461975/html5/thumbnails/40.jpg)
PhysicalInterac5onsintheEarlyUniverseAswegetclosertot→0andT→∞,weprobephysicalregimesinwhichdifferentfundamentalinterac5onsdominate.Theirstrengthisafunc5onofenergy,andatsufficientlyhighenergiestheybecomeunified
![Page 41: Ay 127, Winter 2017: The Early Universegeorge/ay127/Ay127_SGD_Lec05.pdf · • MaFer-an5maFer asymmetry: probes the baryogenesis era, t ~ 10-6 sec, z ~ 1012, but only in sugges5ng](https://reader036.vdocuments.us/reader036/viewer/2022081406/5f0fd4d47e708231d4461975/html5/thumbnails/41.jpg)
TheElectroweakEra:upto10-10sec• AtT~1028K,threedis5nctforcesintheuniverse:Gravity,
Strong,andElectroweak:unifiedElectromagne5smandWeaknuclearforce
• AtT<1015K,Electromagne5smandWeaknuclearforcesplit;thisistheElectroweakphasetransi5on
• Limitofwhatwecantestinpar5cleaccelerators
• AtT>1029K,electroweakforceandstrongnuclearforcejointoformtheGUT(grandunifiedtheory)interac5on
• Rela5velysolidtheore5calframework(butmaybewrong),butnotdirectlytestableinexperiments
• ThisGUTphasetransi5onmaybedrivingtheInfla5on(butthereareothercandidates)
TheGUTEra:upto10-35sec
![Page 42: Ay 127, Winter 2017: The Early Universegeorge/ay127/Ay127_SGD_Lec05.pdf · • MaFer-an5maFer asymmetry: probes the baryogenesis era, t ~ 10-6 sec, z ~ 1012, but only in sugges5ng](https://reader036.vdocuments.us/reader036/viewer/2022081406/5f0fd4d47e708231d4461975/html5/thumbnails/42.jpg)
Ma<er-An5ma<erAsymmetry
q q They basically have all annihilated away
except a tiny difference between them
Matter Particles
10,000,000,001
Antimatter Particles
10,000,000,000
Thisprocessleadstothepreponderanceofphotonsoverthelezoverbaryonstodaybythesamefactor…
Wheredoesitcomefrom?
![Page 43: Ay 127, Winter 2017: The Early Universegeorge/ay127/Ay127_SGD_Lec05.pdf · • MaFer-an5maFer asymmetry: probes the baryogenesis era, t ~ 10-6 sec, z ~ 1012, but only in sugges5ng](https://reader036.vdocuments.us/reader036/viewer/2022081406/5f0fd4d47e708231d4461975/html5/thumbnails/43.jpg)
TheCosmicBaryogenesis• Thecondi5onsrequiredforthecrea5onofmorema<erthan
an5-ma<erwerefirstderivedbyA.Sakharovin1967:1. Baryonnumberviola5on
• Otherwisehavesameno.ofpar5clesandan5par5cles• Neverbeenobserved• PredictedtooccurinseveralGUTtheories
2. CandCPviola5on• Parityofan5par5clesisoppositetothatofpar5cles• CPviola5ondiscoveredin1964(CroninandFitch)
3. Departurefromnon-thermalequilibrium• Otherwiseallreac5onsgobothways• Providedbytheexpansionoftheuniverse
• Nowbelievedtobethemechanismresponsibleforthema<er-an5ma<erasymmetry
![Page 44: Ay 127, Winter 2017: The Early Universegeorge/ay127/Ay127_SGD_Lec05.pdf · • MaFer-an5maFer asymmetry: probes the baryogenesis era, t ~ 10-6 sec, z ~ 1012, but only in sugges5ng](https://reader036.vdocuments.us/reader036/viewer/2022081406/5f0fd4d47e708231d4461975/html5/thumbnails/44.jpg)
PlanckUnitsProposedin1899byM.Planck,asthe“natural”systemofunits
basedonthephysicalconstants:
Theymaybeindica5veofthephysicalparametersandcondi5onsattheerawhengravityisunifiedwithotherforces…assumingthatG,c,andhdonotchange…andthattherearenootherequallyfundamentalconstants
![Page 45: Ay 127, Winter 2017: The Early Universegeorge/ay127/Ay127_SGD_Lec05.pdf · • MaFer-an5maFer asymmetry: probes the baryogenesis era, t ~ 10-6 sec, z ~ 1012, but only in sugges5ng](https://reader036.vdocuments.us/reader036/viewer/2022081406/5f0fd4d47e708231d4461975/html5/thumbnails/45.jpg)
“Derived”PlanckUnits