Neutrino Physics: Lecture 12
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1 Neutrino Physics: Lecture 12 Sterile neutrinos Amol Dighe Department of Theoretical Physics Tata Institute of Fundamental Research Apr 5, 2010
2 Outline 1 Short baseline experiments and LSND anomaly 2 Adding a fourth neutrino 3 Constraining the sterile neutrino 4 Sterile neutrino in astrophysics and cosmology
3 Outline 1 Short baseline experiments and LSND anomaly 2 Adding a fourth neutrino 3 Constraining the sterile neutrino 4 Sterile neutrino in astrophysics and cosmology
4 SBLs: When only one m 2 matters No CP violation, any number of neutrinos: P αβ = δ αβ i<j 4Re( αβij ) sin 2 ( ji ) αβij U αi U βj Uαj U βi Approximation of single mass-squared dominance All significant ji nearly equal, All other ji negligible, 0 P αα = 1 sin 2 2θ eff sin 2 ( ) P αβ = sin 2 2θ eff sin 2 ( ) (α β)
5 SBLs: When only one m 2 matters No CP violation, any number of neutrinos: P αβ = δ αβ i<j 4Re( αβij ) sin 2 ( ji ) αβij U αi U βj Uαj U βi Approximation of single mass-squared dominance All significant ji nearly equal, All other ji negligible, 0 P αα = 1 sin 2 2θ eff sin 2 ( ) P αβ = sin 2 2θ eff sin 2 ( ) (α β)
6 Equi-probabilty contours sin 2 2θ eff sin 2 ( ) = Constant
7 Short baseline and sensitivity to m 2 Nontrivial P αα or P αβ only when 1 Atmospheric neutrinos: E 1 GeV, L 10 3 km m ev 2 Reactor neutrinos: E 1 MeV, L 1 km m ev 2 Long baseline experiments: E 1 10 GeV, L km m ev 2 Accelerator (short baseline) experiments: E MeV, L 1 km m ev 2
8 Neutrino experiments with 2ν approximation
9 Solar and atmospheric experiments
10 Results from short baseline experiments
11 The LSND excess ν µ ν e oscillations! Excess = 87.9 ± 22.4 ± 6.0 events
12 L/E oscillations in LSND Oscillation probability ± ± m ev 2
13 The LSND parameter space hep-ex/
14 A fourth neutrino? Three independent m 2 : m ev 2 matm ev 2 m ev 2 Not possible with only three neutrino masses! A fourth neutrino species must be present
15 A fourth neutrino? Three independent m 2 : m ev 2 matm ev 2 m ev 2 Not possible with only three neutrino masses! A fourth neutrino species must be present
16 Outline 1 Short baseline experiments and LSND anomaly 2 Adding a fourth neutrino 3 Constraining the sterile neutrino 4 Sterile neutrino in astrophysics and cosmology
17 A fourth generation neutrino? LEP: e + e Z f f Effective number of neutrinos: N ν = ± Only three light neutrinos interact with Z The fourth neutrino has to be sterile!
18 What is a (light) sterile neutrino A fermion without electric charge Does not have electroweak interactions (Does not interact with W, Z, γ) Can have interactions beyond the Standard Model (BSM) Can mix with active neutrinos due to the BSM interactions NOT the right-handed partner of active neutrinos
19 What is a (light) sterile neutrino A fermion without electric charge Does not have electroweak interactions (Does not interact with W, Z, γ) Can have interactions beyond the Standard Model (BSM) Can mix with active neutrinos due to the BSM interactions NOT the right-handed partner of active neutrinos
20 What is a (light) sterile neutrino A fermion without electric charge Does not have electroweak interactions (Does not interact with W, Z, γ) Can have interactions beyond the Standard Model (BSM) Can mix with active neutrinos due to the BSM interactions NOT the right-handed partner of active neutrinos
21 What would the neutrino mass spectrum look like? Mixing matrix: 6 angles and 10 phases U = Φ(χ 1, χ 2, χ 3, χ 4 ) U 14 (θ 14, δ 14 ) U 34 (θ 34, 0) U 24 (θ 24, δ 24 ) U 23 (θ 23, 0) U 13 (θ 13, δ 13 ) U 12 (θ 12, 0) Φ(φ 1, φ 2, φ 3, 0)
22 Outline 1 Short baseline experiments and LSND anomaly 2 Adding a fourth neutrino 3 Constraining the sterile neutrino 4 Sterile neutrino in astrophysics and cosmology
23 Testing the LSND anomaly MiniBOONE: E 1 GeV, L 1 km ν µ as well as ν µ beams
24 Constraining sterile ν from appearance experiments
25 Constraints from disappearance experiments Solar neutrinos SNO indicates that most ν e go to ν µ or ν τ bound on ν e ν s mixing Atmospheric neutrinos Extra contribution to atmospheric oscillations: P µµ P µµ (3ν) 1 2 sin2 2θ µs bound on ν µ ν s mixing Reactor experiments mlsnd 2 would contribute to KamLAND, K2K, MINOS bound on ν e ν s and ν µ ν s mixing mlsnd 2 would contribute to CHOOZ bound on ν e ν s and ν µ ν s mixing
26 Constraints from disappearance experiments Solar neutrinos SNO indicates that most ν e go to ν µ or ν τ bound on ν e ν s mixing Atmospheric neutrinos Extra contribution to atmospheric oscillations: P µµ P µµ (3ν) 1 2 sin2 2θ µs bound on ν µ ν s mixing Reactor experiments mlsnd 2 would contribute to KamLAND, K2K, MINOS bound on ν e ν s and ν µ ν s mixing mlsnd 2 would contribute to CHOOZ bound on ν e ν s and ν µ ν s mixing
27 Constraints from disappearance experiments Solar neutrinos SNO indicates that most ν e go to ν µ or ν τ bound on ν e ν s mixing Atmospheric neutrinos Extra contribution to atmospheric oscillations: P µµ P µµ (3ν) 1 2 sin2 2θ µs bound on ν µ ν s mixing Reactor experiments mlsnd 2 would contribute to KamLAND, K2K, MINOS bound on ν e ν s and ν µ ν s mixing mlsnd 2 would contribute to CHOOZ bound on ν e ν s and ν µ ν s mixing
28 LSND parameter space ruled out ArXiv:
29 Can more than one sterile neutrinos help? Need 2 neutrinos of masses ev Constraints from cosmology
30 Outline 1 Short baseline experiments and LSND anomaly 2 Adding a fourth neutrino 3 Constraining the sterile neutrino 4 Sterile neutrino in astrophysics and cosmology
31 Sterile neutrinos in astrophysics Nucleosynthesis of heavy elements (r-process) Heavy elements need more neutrons ν e tend to reduce number of neutrons: ν e + n e + p ν e ν s conversion can allow heavy elements to be formed, if m ev 2 Supernova explosions Conversions to ν s carry away energy efficiently May affect explosion dynamics Can create large asymmetries in ν emission May explain large pulsar velocities
32 Sterile neutrinos in astrophysics Nucleosynthesis of heavy elements (r-process) Heavy elements need more neutrons ν e tend to reduce number of neutrons: ν e + n e + p ν e ν s conversion can allow heavy elements to be formed, if m ev 2 Supernova explosions Conversions to ν s carry away energy efficiently May affect explosion dynamics Can create large asymmetries in ν emission May explain large pulsar velocities
33 Sterile neutrinos in cosmology kev neutrinos are viable dark matter candidates Can help in producing supermassive black holes Predicted by some models (e.g. νmsm) that explain baryon asymmetry
34 (Not) the last word on sterile neutrinos ev-neutrinos not required for explaining oscillation data, Not ruled out either (only mixing constrained) Can help some astrophysical phenomena if m ev 2, very small mixing kev-neutrinos may play a role in cosmology, structure formation
35 (Not) the last word on sterile neutrinos ev-neutrinos not required for explaining oscillation data, Not ruled out either (only mixing constrained) Can help some astrophysical phenomena if m ev 2, very small mixing kev-neutrinos may play a role in cosmology, structure formation
36 (Not) the last word on sterile neutrinos ev-neutrinos not required for explaining oscillation data, Not ruled out either (only mixing constrained) Can help some astrophysical phenomena if m ev 2, very small mixing kev-neutrinos may play a role in cosmology, structure formation
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