Lecture35 Hot Big Bangpeople.virginia.edu/~cls7i/Classes/astr2120/Lecture35_Hot_Big_Bang.pdfBang!...
Transcript of Lecture35 Hot Big Bangpeople.virginia.edu/~cls7i/Classes/astr2120/Lecture35_Hot_Big_Bang.pdfBang!...
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The Hot Big BangASTR 2120
Sarazin
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Final ExamThursday, May 7, start anytime before 8
pm4 hoursYou may not consult the text, your notes,
or any other materials or any personYou can use three of 3x5 cards (both
sides) or 6x5 paper (one side) with equations only
Have pencils, paper, calculator
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Final Exam~2/3 Quantitative Problems (like homework
problems)~1/3 Qualitative Questions
Multiple Choice, Short Answer, Fill In the Blank
Test done with Collab Tests & Quizzes ToolQuantitative Problems:
Do work on work sheetsType Answers in Answer Boxes in Collab
Scan/photo worksheets and equation sheets, either upload at Collab Assignments “Final Exam Work Sheets” tool or email to me [email protected]
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Final Exam (Cont.)
Material:Final exam will cover the entire semester
Chapters (5), (7), 13-24Stars, Sun ® Cosmology
Extra emphasis on material not on first two testsExtragalactic Distances, Clusters of Galaxies
(problems), AGNs, CosmologyChapters 21, 23, 24Homeworks 9-11
Know pc, AU, Msolar, Lsolar, Rsolar, H0, TCMB
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Final Exam ReviewReading DayWednesday, May 610 am – noon
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The Hot Big BangASTR 2120
Sarazin
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Hot Big Bang
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€
particle + antiparticle ↔ 2γExample : p + p ↔ 2γN particles ≈ Nantiparticles ≈ Nγ
Bubbling sea of particles and antiparticlesp, p ,n,n ,e− ,e+ ,γ,ν,ν ,π,Ω− , . . . etc.
Thermal History of Universe
t ≲ 10-6 sec, T ≳ 1013 K
Tγ ≈1010 K t−1/2 (t in sec)for Tγ >10, 000 K
10-5 sec ≲ t ≲ 1 sec, 1013 K > T ≳ 1010 KCan’t make most particlesa) Unstable particles decay
Exception: neutron, t1/2 = 11 minutes
€
p, p ,n,n ,e− ,e+ ,γ,νe,ν e,νµ ,ν µ ,ντ ,ν τ ,(dark matter particles)
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Thermal History of Universe10-5 sec ≲ t ≲ 1 sec, 1013 K > T ≳ 1010 K
b) Antimatter annihilates
If matter/antimatter symmetric, this is very efficientNp/Ng ≲ 10-18, not 10-9 as observed (homework)
If pure matter, Np ~ Ng initially, would still be trueNeed small, but non-zero asymmetry
€
p + p → 2γ (no reverse)n + n → 2γ
€
N p − N p
N p
~10−9
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Thermal History of Universe10-5 sec ≲ t ≲ 1 sec, 1013 K > T ≳ 1010 K
Existence of matter today requires Universe had a small matter/antimatter asymmetry by 1 sec
€
N p − N p
N p
~10−9
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Thermal History of Universe10-5 sec ≲ t ≲ 1 sec, 1013 K > T ≳ 1010 K
c) Electrons and neutrinos still producedkT >> mec2
d) Protons and neutrons in equilibrium
View p+ & n as different states (isotopic spin) of same particle
€
e−,e+ ,νe,ν e
€
p+ + e− ↔ n+νep+ +ν e ↔ n+ e+ , etc.
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Thermal History of Universe10-5 sec ≲ t ≲ 1 sec, 1013 K > T ≳ 1010 K
View p+ & n as different states (isotopic spin) of same particle
€
Nn
Np
= e−ΔE /kT = e−Δmc2 /kT = e−(mn −mp )c
2 /kT
n
p
ΔE=(mn−mp) c2
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Thermal History of Universe
1 sec ≲ t ≲ 103 sec, 1010 K > T ≳ 3 x 108 K(mn-mp)c2/k ~ 1010 K
Nn/Np decreasesAfter a few seconds, T < mec2/k ~ 6 x 109 K, can’t
make electrons anymore
Reactions between n, p stop
€
Nn
Np
= e−ΔE /kT = e−Δmc2 /kT = e−(mn −mp )c
2 /kT
€
e+ + e− → 2γ (no reverse)
€
n+ e+ ↔ p+ +ν e, etc. stop
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Thermal History of Universe
1 sec ≲ t ≲ 103 sec, 1010 K > T ≳ 3 x 108 KNeutron to proton ratio freezes out at
What happens to neutrons?
If nothing else happened, neutrons would decay away
€
Nn
Np
= e−ΔE /kT = e−Δmc2 /kT = e−(mn −mp )c
2 /kT
€
n→ p+ + e− +ν e, beta decay, t1/2 =11 minutes€
Nn ≈ Np / 8
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Fusion During Big Bang1 sec ≲ t ≲ 103 sec, 1010 K > T ≳ 3 x 108 K
rbaryons ≲ 10-2 gm/cm3
Hotter, lower density than center of star, but not completely dissimilar
Differences from star:a) Very little time (minutes)
No weak reactionsNo pp reaction (1010 years in Sun)
b) Free neutronsNever true in stars except during SN, only
last 11 minutes
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Fusion During Big Bang
Tritium
p+ n→ 2H+γ2H+ n→ 3H+γ2H+ p→ 3He+γ3He+ n→ 4He+γ3H+ p→ 4He+γ 3 H→ 3 He+ e− +νe
t1/2 =12 years
All tritium è Helium-3
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Fusion During Big Bang
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Fusion During Big Bang
and similar
No significant reactions beyond 4HeIn stars, requires Triple-Alpha reaction, very slow,
not enough time in Big BangLose energy between 4He and 12C, only reaction is
3 4He ® 12C
€
p+ n→ 2H+γ2H + p→ 3He+γ3He +n→ 4He+γ
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Fusion During Big Bang
3a reaction
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Fusion During Big Bang
and similar
No significant reactions beyond 4HeIn stars, requires Triple-Alpha reaction, very slow,
not enough time in Big BangLose energy between 4He and 12C, only reaction is
3 4He ® 12C
€
p+ n→ 2H+γ2H + p→ 3He+γ3He +n→ 4He+γ
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Fusion During Big Bang
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Fusion During Big BangFusion in Big Bang makes
H & 4HeTraces of 2H & 3HeTiny bits of 6Li, 7Li, 7Be
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Fusion During Big BangHow much helium?
Fusion reactions up to helium very efficientAll neutrons ® heliumInitially, Nn ~ Np / 8Do arithmetic (homework problem), findY = 0.22 (mass fraction of helium)X = 0.78 (mass fraction of hydrogen)
Agree with values in oldest stars
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Fusion During Big BangHow much 2H (deuterium), 3He (helium-3), Li?
Fusion reaction rate depends on density of baryonsrbaryons
High density = less 2H, 3He, more LiLow density = more 2H, 3He, less Li
€
p+ n→ 2H+γ2H + p→ 3He+γ3He +n→ 4He+γ
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Fusion During Big Bang
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Fusion During Big BangGives rbaryons at t = 1 sec, T = 1010 K
rbaryons (today) = rbaryons (1 sec) x (r / ro)3
= rbaryons (1 sec) x (1 + z)-3
T (1 sec) = T (today) x (1 + z)(1 + z ) = 1010 K / 2.725 Krbaryons (1 sec) gives rbaryons (today)!!
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Fusion During Big Bang
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Fusion During Big BangGives rbaryons at t = 1 sec, T = 1010 K
rbaryons (today) = rbaryons (1 sec) x (r / ro)3
= rbaryons (1 sec) x (1 + z)-3
T (1 sec) = T (today) x (1 + z)(1 + z ) = 1010 K / 2.725 Krbaryons (1 sec) gives rbaryons (today)!!rbaryons (today) = 3.5 x 10-31 gm/cm3
W (baryons) = rbaryons / rcrit = Wb = 0.046
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Fusion During Big BangWb = 0.046 << WM
Dark Matter not anything which was ordinary matter at t = 1 second
Not planets, brown dwarfs (MACHOs)Not black holes from stars or collapse of matter
Dark Matter = weakly interacting particles made in Big Bang!
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Cosmological NeutrinosIn early Universe
Decouple at t ~ 1 sec
Nn ~ Ng Tn = (4/11)1/3 TCMB = 1.95 KNeutrinos stable (except for oscillations), still
aroundCosmological background of neutrinosIf mass = 0, just like photons
€
2γ ↔ e+ + e− ↔νe +ν e (etc.)
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Neutrino Dark Matter?Oscillations of neutrinos ® must have massIf mn > 10 eV, could be Dark MatterTritium decay, cosmology, particle experiments ®
mn < 1 eVProbably not dark matter, but example of potential weakly
interacting dark matter particles from Big Bang
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Made in Big Bang• Hot Dark Matter
• kT >> mc2 when decoupled ® v ~ c when formed• mc2 ~ eV• Example: neutrinos• Problem: hard to get to cluster, form superclusters ®
clusters ® galaxies ® stars• But, galaxies old, structure appears to grow small to large
Probably NOT Hot Dark Matter
Particle Dark Matter
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• Cold Dark Matter• kT << mc2 when decoupled ® v << c when formed• mc2 ~ 1-1000 GeV = 1 – 1000 mpc2
• Exception: axion• Examples:
• WIMPs = Weakly Interacting Massive Particles• lightest supersymetric particle (gravitino,
neutralino)• axions
• Structure grows hierarchically, small to largeCurrently the favored form of DM
Particle Dark Matter
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Leading candidate is lightest supersymmetricparticleSupersymmetry (SUSY):
Every boson (integer spin) has a fermion (half integral spin) supersymmetric partner
Example: photon (spin 1) / photino (spin ½)Every fermion has a boson supersymmetricpartner
Example: electron (spin ½) / selectron (spin 0)
WIMPs
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Supersymmetry particles only decay into supersymmetric particlesè Lightest supersymmetric particle is stable, could
be Dark Matter
Leading candidates:gravitino = SUSY partner of graviton, carrier of
gravity forceneutralino = SUSY partner of W0,Z, B, Higgs
WIMPs
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Another particle outside of the standard model is the axionAssociated with symmetry which keeps the strong interaction
from violating CP invarianceWeakly interacting, light (10-6 to 1 eV), produced in Big BangCandidate Dark Matter particlesCan be detected due to effect on photons in a strong
magnetic fieldAlso, super-partners (axino, saxino) might be LSP, also Dark
Matter candidates
Axions
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• Warm Dark Matter• mc2 ~ keV• Examples: Sterile neutrino
Normal Neutrinos: left handedSterile Neutrinos : right handed
Only left handed neutrinos interact with matter
Particle Dark Matter
Sterile neutrino Normal neutrino
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Later Thermal Historyt ~ 50,000 years, z ~ 3600, T ~ 10,000 K
End of radiation-dominated era
t = 370,000 years, z =1100 , T = 3000 KRecombinationPrior to this, matter is mainly p+ & e-
At recombination, p+ + e-® H (hydrogen atoms)
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Recombination
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Recombinationt = 370,000 years, z =1100 , T = 3000 K
Prior to recombination, p+ & e-
Matter and radiation tightly coupled by electron scattering
e-photon
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Recombinationt = 370,000 years, z =1100,
T = 3000 KMatter and radiation decoupled
Matter can separate from radiation, form structures (galaxies, clusters, etc.)
CMB photons all come directly from recombination era, “last scattering surface”
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Epoch of ReionizationIntergalactic medium today is completely ionized
againWhen did this happen?
WMAP: started at z ~ 20Quasar spectra: complete by z ~ 6
Due to UV from:stars in newly formed galaxies?quasars from supermassive BHs in centers of newly
formed galaxies?
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Epoch of Reionization21 cm line from hydrogen
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CHIME Radio Telescope
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Later Thermal Historyt ~ 50,000 years, z ~ 3600, T ~ 10,000t = 370,000 years, z =1100 , T = 3000 K
RecombinationT = 9 billion years, z ~ 1, T ~ 6 K
Epoch of Dark Energy Accelerated Expansion
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Dark Energy – Accelerated Expansion
tor / ro
t
deceleration
acceleration
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Large Scale Structure
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13.7 billion years ago
How does the Universe go from looking like this...To looking like this….?
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13.7 billion years ago13.5 billion years ago12.7 billion years ago
Millennium Simulation
9 billion years agoNOW
The Universe Evolves
Gravity Rules
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Structure FormationNeed fluctuations in density of 10-5 at recombination to
make all the galaxies and clusters of galaxies todayPrediction confirmed by WMAP and Planck
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13.7 billion years ago13.5 billion years ago12.7 billion years ago
Millennium Simulation (Springel et al. 2005)
9 billion years agoNOW
Millennium Simulation Sample