Particles and fields The standard model
Transcript of Particles and fields The standard model
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Particles and fields –The standard model
Edvard Mörtsell
Cosmology and Astroparticle Physics FK7050
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Standard models of Particle physics and Cosmology
Particle Physics Cosmology
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How many atoms are there in a carrot?
106
1016
1025
1050
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Particles and fields - QuarksEdvard Mörtsell
Cosmology and Astroparticle Physics FK7050
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Quarks and colour
• To each quark (u) comes an anti-quark (u̅)
• Each (anti-)quark comes in three (anti-)colours: red, blue and green
• Quarks combine to give colour-less particles: hadrons
• Red + blue + green (baryon)
• Colour + anti-colour (meson)
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What are the charges of the particles below?
+1 and +1
-1 and +1
+1 and -1
-1 and -1
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Which are the particles below?
A neutron and a proton
A lepton and a gluino
A proton and a pion
A kaon and a D meson
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The strong force
• Force mediators are bosons
• Baryons and mesons are kept together by the strong force
• The strong force is mediated by gluons
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How could you make a neutron out of u and d-quarks?
𝑢, 𝑢 and 𝑑
𝑢, 𝑑 and 𝑑
𝑢, ത𝑢 and 𝑑
𝑢, ҧ𝑑 and 𝑑
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Particles and fields - LeptonsEdvard Mörtsell
Cosmology and Astroparticle Physics FK7050
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The electromagnetic force
• Atoms are held together by the electromagnetic (EM) force
• The electromagnetic force is mediated by photons
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Leptons
To each family, there are also two leptons (and anti-leptons):
• One with zero charge
• One with charge –e = -1
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Neutrinos and the weak force
• Neutrinos do not have strong or electromagnetic interactions
• They interact with the weak force
• The weak force is mediated by Z and W bosons
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Which is heaviest, the Z or W boson?
The Z boson
The W boson
They have the same mass
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Higgs (Englert) boson
• Physics describe particles and their interactions throughforces (carried by other particles)
• This can be described by fields and their interactions
• Excitation of the scalar Higgs field: Spin 0
• Gives mass to standard model particles
• Predicted in 1964, found in 2012
• Mass 125 GeV (a proton is 1 GeV)
• Weak and gravitational interactions
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Particles and fields –Quantum numbers
Edvard Mörtsell
Cosmology and Astroparticle Physics FK7050
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Quantum numbers
Conserved quantities (momentum, angular momentum) arerelated to symmetries (translations, rotations)
• Electric charge
• Spin
• Baryon number (?)
• Lepton number?
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What quantum number conservation is violated in the process below?
𝑏 → ҧ𝑠 + 𝑠 + 𝑑 + 𝑒− + ҧ𝜈𝑒
Lepton number conservation
Baryon number conservation
Charge conservation
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Force Force mediator
Interactionlength
Particles
Strong Gluon 10-15 metres Quarks, hadrons
Weak W and Z 10-17 metres Fermions, Higgs
Electromagnetic Photon Infinite Charged particles
Gravity Graviton? Infinite All particles
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Grand Unified Theory (GUT) and Theory of Everything (TOE)
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Particles and fields - StatesEdvard Mörtsell
Cosmology and Astroparticle Physics FK7050
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Spin states
• Two particles with spin s can be in different states depending on the spin direction, e.g., projected on the z-axis
• The projection on the direction of propagation, is denoted helicity
• For massive particles, helicity is not unambigous when changingframe (but the related chirality is)
• Massive particles have 2s+1 possible helicity states
• Massless spin-1 particles have only 2 possible helicity states, ±1
• Neutrinos only have helicity -1; they are left-handed
• Anti-neutrinos have helicity +1; they are right-handed
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What is the helicity of a particle?
The spin of a particle projected on its direction of motion
The spin of a particle in units of ℏ
The angular momentum squared of a particle
The inverse mass of a particle
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States in the Standard Model
• 12 quarks in 3 colours with 2 spin states = 72
• 6 charged leptons with 2 spin states = 12
• 6 neutrinos
• 90 fermion states
• 8 gluons with 2 spin states = 16
• 1 photon with 2 spin states = 2
• W± and Z with 3 spin states = 9
• Higgs = 1
• In total: 118 states
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How many boson states are there in the particle standard model?
28
90
None
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Word list
• Quark (Spin ½, all fundamental interactions, fractional EM charge)
• Lepton (Spin ½, no strong interactions, integer EM charge)
• Fermion (Any half-integer spin particle, including composite ones)
• Boson (Any integer spin particle, including composite ones)• Fundamental bosons: spin 0 = Higgs, spin 1 = force carriers, spin 2: graviton?
• Baryon (Particle made up of three quarks)
• Meson (Particle made up of a quark and an anti-quark)
• Hadron (Baryon or meson)
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A proton is a (multiple answers possible)
Quark
Lepton
Fermion
Boson
Baryon
Meson
Hadron
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Particles and fields –Cross-sections
Edvard Mörtsell
Cosmology and Astroparticle Physics FK7050
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Feynman diagrams
Time →
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Feynman rules
• The Feynman rules are a prescription for calculating the amplitude for a diagram
• The cross-section is given by the squared amplitude
• Each vertex (where lines meet) gives a factor given by the coupling strength, 𝑔
• Each internal line corresponds to a factor of the virtual particle's propagator
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Interaction strengths
• The electromagnetic coupling is 𝑔EM = 𝑄𝑒, where the fine structure constant is given by
𝛼EM ≡𝑒2
4𝜋≈
1
137
• The weak coupling constant is
𝑔weak =𝑒
sin 𝜃wwhere the Weinberg angle is sin2 𝜃w ≈ 0.23
• The strong coupling constant, 𝑔s, is given by (at a few GeV)
𝛼s ≡𝑔s2
4𝜋≈ 0.3
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The propagator and phase space factors
The propagator factor is given by
𝑃 𝑠 =1
𝑠 − 𝑚𝑖2
where 𝑚𝑖 is the (real) mass of the propagator particle and 𝑠 its virtual mass squared, 𝑠 = 𝑝1 + 𝑝2
2.
For fermion propagators, 𝑃 ∝ 𝑚−1 at low energies.
The phase space factor 𝜙 , multiplying the cross-section, takes into account that outgoing particles have many possible final states, e.g., different scattering angles.
In many cases, 𝜙 ∝ 𝑠 for large energies.
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Electromagnetic example
An electron and a positron annihilating and forming a muon and an anti-muon will have a cross-section
𝜎 ∼ 𝜙 ⋅𝑒4
𝑠2∼ 𝜙 ⋅
𝛼
𝑠
2
∼𝛼2
𝑠where the last approximation holds for large energies.
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Weak interaction example
An electron neutrino and a positron annihilating and forming a muon neutrino and an anti-muon will have a cross-section
𝜎 ∼ 𝜙 ⋅𝑒4
sin4 𝜃w (𝑠 − 𝑚w2 )2
∼ 𝜙 ⋅𝛼
𝑠 − 𝑚w2
2
∼𝑠𝛼2
𝑠 − 𝑚w2 2
being very small for 𝑠 ≪ 𝑚w2 .
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Particles and fields –The dark sectors
Edvard Mörtsell
Cosmology and Astroparticle Physics FK7050
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Vacuum energy density
• The energy of a massless scalar field is the sum of all possible ground state energies 𝐸0 = σ𝑖(ℏ𝜔𝑖)/2
• In a box with side 𝐿, we can fit harmonic oscillators with 𝜆𝑖 ⋅ 𝑛𝑖 = 𝐿
• In terms of the wave vector 𝑘𝑖 = (2𝜋)/𝜆𝑖 = 𝜔𝑖, 𝑛𝑖 = 𝐿 ⋅ 𝑘𝑖/(2𝜋)
• Summing the number of modes at each 𝑘, we obtain
𝐸0 =ℏ
2
𝐿3
2𝜋 3 ∫ 𝑘𝑑3𝑘 =ℏ
16𝜋2𝐿3𝑘max
4
• Putting the cut-off scale to the Planck energy, we obtain
𝜌vac =𝐸0𝐿3
∼ 1095 kg/m3
• The fact that this is a factor of 10122 too high is referred to as the cosmological constant problem
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Imagine we put the cut-off scale for our field theory treatmentof the vacuum energy to that of the W and Z bosons instead(that we know exist and we believe we understand well). What is the corresponding vacuum energy contribution?
𝜌vac∼ 1 kg/m3
𝜌vac∼ 1027 kg/m3
𝜌vac∼ 1078 kg/m3
𝜌vac∼ 10120 kg/m3
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dark matter?
graviton(s)
dark energy?
inflaton?