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Non-Standard Interactions of neutrinos Yasaman Farzan IPM, Tehran
Non-Standard Interactions of neutrinos
Yasaman FarzanIPM, Tehran
Standard Neutrino interactions
´ Charged current coupling to electroweak gauge boson:
´ Neutral current coupling to electroweak gauge boson:
Broad meaning of NSI
´ Effective NSI with matter fields
´ New gauge interaction for neutrinos
´ Yukawa interaction
Effects of NSI on neutrinos
´ Neutral current Non-Standard Interaction (NSI): propagation of neutrinos in matter
´ Charged current Non-Standard Interaction (NSI): production and detection
Effects of NSI on neutrinos
´ Neutral current Non-Standard Interaction (NSI): propagation of neutrinos in matter
´ Charged current Non-Standard Interaction (NSI): production and detection
Focus of this talk
Non-standard neutral current interaction
Neutrino propagation:
Matter fieldProjectionmatrix
Standard Oscillation
In parenthesis
Non-Standard matter effects
Effects of NSI in long baseline experiments´ Renewed interest in NSI
´ NSI can fake CP-violation and lead to wrong determination of octant
Masud and Mehta, PRD 94(2016); Forero and Huber, PLB 117 (2016); Liao, Marfatia and Whistnant PRD 93 (2016); Agarwalla, Chatterjee and Palazzo, PLB 762 (2016)
Underlying models for NSI with light mediators
Y.F., PLB 748 (2015) 311; Y.F. and I. Shoemaker, JHEP 1607 (2016) 033; Y.F. and J.
Heeck, PRD94 (2016) no 5, 53010, Y.F. and M. Tortola, Front. In Phys 6 (2018) 10;
J. Heeck, M. Lindner, W. Rodejohann and Vogl, arXiv:1812.04067
LMA-Dark solution to the solar neutrino anomaly
´ LMA-Dark solution provides even a better fit. (suppression of low energy upturn)
Miranda, Tortola, Valle, JHEP 2004
Total solar neutrino flux measurement at SNO
´ Neutral current
´ Deuteron dissociation
´ Gamow-Teller transition
´ Sensitive only to axial-vector interaction
´ No effect from
Scattering experiments
NuTeV and CHARM rule out a large part (but not all) of parameter space of LMA-Dark solution.
Davidson, Pena-Garay, Rius, SantaMaria, JHEP 2003
Scattering experiments
NuTeV and CHARM rule out a large part (but not all of) parameter space of LMA-Dark solution.Davidson, Pena-Garay, Rius, SantaMaria, JHEP 2003
But not in the model that we shall present
Underlying theory for LMA-Dark?
Various model with heavy intermediate particleFor a review see:
Too small NSI
Suggestion
´ What if
YF, A model for large non-standard interactions leading to LMA-Dark solution,Phys. Lett. B748 (2015) 311-315; YF and J Heeck, Neutrinophilic nonstandard interactions,PRD 94 (2016) 53010; YF and I Shoemaker, lepton flavor violating NSI via light mediator,JHEP 1607 (2016) 33. YF and M Tortola, “neutrino oscillations and non-standard interactions” to appear in Frontiers in Physics; J. Heeck, M. Lindner, W. Rodejohann and Vogl, arXiv:1812.04067
Suggestion
´ What if
´ Bounds can be avoided not because the mass of the intermediate state is high
But because coupling is small!
Big Bang Nucleosynthesis
´ Huang, Ohlsson and Zhou, PRD 97 (2018) 75009
Bounds on Couplings of neutrinos
Barger et al, PRL 108 (2012);Laha et al, PRD 89 (2014);Pospelov, PRD 8 (2009)
Constraining secret gauge interactions of neutrinos by meson decay
Pouya Bakhti and YF, arXiv:1702.04187
Suppression of two-body decay versus enhancement of three body decay
NA62 bound
Lazzeroni et al [NA62 collaboration]PRD 79 (2009) 326
P Bakhti and YF, PRD 95 (2017) 095008
P Bakhti and YF, PRD 95 (2017) 095008
Artamonov et al., BNL-E494 collaboration, PRD 79 (2009) 092004
Coupling to quarks
´ Non-chiral couplings: No impact on total measurement at SNO
´ Flavor universal: Going to mass basis
Y.F. and J Heeck, PRD 94 (2016)053010
Coupling to fermion
Direct coupling to neutrinos
Gauge symmetry:
Coupling to neutrinos through mixing with :
Gauge symmetry:
Coupling to neutrinos
´ Direct coupling to neutrinos
Gauge symmetry:
Harnik, Kopp and Machado, JCAP 1207 (2012) 026
Anomaly cancelation:
Reproducing best fit
Anomaly free combinatons
J. Heeck, M. Lindner, W. Rodejohann and Vogl, arXiv:1812.04067
Anomaly cancelation
Adding a new generation of leptons (quarks)
Adding a pair of fermions with opposite hypercharges
Non-perturbative Yukawa coupling
Coupling to neutrinos
Direct coupling to neutrinos
Gauge symmetry:
Coupling to neutrinos through mixing with :
Gauge symmetry:
Coupling of neutrinos through mixing
Fernandez-Martinez et al., JHEP 08 (2016) 033
Coupling of neutrinos through mixing
Fernandez-Martinez et al., JHEP 08 (2016) 033
Neutrino scattering experiments
Suppression factor
Neutrino scattering experiments
Relaxing bounds from scattering experiments, NuTeV and CHARM
YF and J Heeck, PRD94 (2016) 053010
LUX-Zeplin SuperCDMS SNOLAB
COHERENT experiment
Neutrino source: Pion decay at rest
Coloma et al,JHEP 1704 (2017)116
COHERENT experiment
´ Akimov et al., “Observation of Coherent Elastic neutrino Nucleus Scattering,” science 357 (2017) No 6356, 1123
Freedman, PRD 9 (1974) 1389.
Set-up of the COHERENT experiment
´ Detector: 14.6 kg CsI scintillator
´ Source: Spallation Neutron Source (SNS) at Oak Ridge National Lab
Akimov et al., Science 357 (2017) No 6356, 1123
Akimov et al., Science 357 (2017) No 6356, 1123
P. Coloma, P. Denton, Gonzalez-Garcia,Maltoni and Schwetz, “curtailing the dark Side in non-standard neutrino interaction,”JHEP 1704 (2017) 116
JHEP 1704 (2017) 116
Esteban et al.,JHEP 1808 (2018)180
Standard coherent interaction
Liao and Marfatia, Phys Lett B775 (2017) 54
Coherent interaction with light mediator
Liao and Marfatia, Phys Lett B775 (2017) 54
Liao and Marfatia, Phys Lett B775 (2017) 54
LMA-Dark after COHERENT data
Denton, YF Shoemaker, JHEP 1807 (2018) 037 , arXiv:1804.03660
Denton, YF Shoemaker, JHEP 1807 (2018) 037, arXiv:1804.03660
Solar neutrino interaction at DM direct detection experiments
Y.F. and J. Heeck, PRD94 (2016);
Cerdeno et al,JHEP 05 (2016) 118
12/15/18Yasaman Farzan
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LMA-DARK solution
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Viable Z’ mass range
CONUS,COHERENTFuture solar
BBN+CMB
No Dip is cosmicneutrino spectrum
Summary
´ gauge boson with and can lead to sizeable NSI.
´ COHERENT has not ruled out LMA-Dark yet!
´ Upcoming CEνNS experiments can test this scenario
Yukawa interaction
12/15/18Yasaman Farzan
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Y. Farzan, M. Lindner, Rodejohann and X-J Xu,JHEP 1805 (2018) 066
Effects of LNV Yukawa on BBN
´ Heavy scalar decays to neutrinos before neutrino decoupling
´ Lighter ones can contribute to extra relativistic degrees of freedom.
12/15/18Yasaman Farzan
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Huang, Ohlsson and Zhou, PRD 97 (2018) 075009
12/15/18Yasaman Farzan
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LNC Yukawa and early universe
12/15/18Yasaman Farzan
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Effects in supernova evolution
´ Protoneutron star:
Inner core:
Outer core:
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µ⌫e ⌧ T<latexit sha1_base64="uJxVR3peFWiMHmWKv4nJVUJ1ArE=">AAAB+XicbVDLSsNAFL2pr1pfUZduhhbBVUnc6LLoxmWFvqAJYTKdtEMnkzCPQgkFP8SNC0Xc+ifu/Bunj4W2HrhwOOde7r0nzjlT2vO+ndLW9s7uXnm/cnB4dHzinp51VGYkoW2S8Uz2YqwoZ4K2NdOc9nJJcRpz2o3H93O/O6FSsUy09DSnYYqHgiWMYG2lyHWD1ERFIExEZwHnqBW5Na/uLYA2ib8itUY1qD4BQDNyv4JBRkxKhSYcK9X3vVyHBZaaEU5nlcAommMyxkPat1TglKqwWFw+Q5dWGaAkk7aERgv190SBU6WmaWw7U6xHat2bi/95faOT27BgIjeaCrJclBiOdIbmMaABk5RoPrUEE8nsrYiMsMRE27AqNgR//eVN0rmu+17df7Rp3MESZbiAKlyBDzfQgAdoQhsITOAZXuHNKZwX5935WLaWnNXMOfyB8/kDV2eU5w==</latexit><latexit sha1_base64="Ep7dpV5F0qAbMZHO1TqqKC99+8E=">AAAB+XicbVC7SgNBFL3rM8bXqqXNkCBYhV0bLYM2lhHygmxYZiezyZDZ2WUegbDkA/wCGxsLRWz9BP/ARvwbJ49CEw9cOJxzL/feE2WcKe15387a+sbm1nZhp7i7t39w6B4dN1VqJKENkvJUtiOsKGeCNjTTnLYzSXEScdqKhjdTvzWiUrFU1PU4o90E9wWLGcHaSqHrBokJ80CYkE4CzlE9dMtexZsBrRJ/QcrVUlC6f/j4qoXuZ9BLiUmo0IRjpTq+l+lujqVmhNNJMTCKZpgMcZ92LBU4oaqbzy6foDOr9FCcSltCo5n6eyLHiVLjJLKdCdYDtexNxf+8jtHxVTdnIjOaCjJfFBuOdIqmMaAek5RoPrYEE8nsrYgMsMRE27CKNgR/+eVV0ryo+F7Fv7NpXMMcBTiFEpyDD5dQhVuoQQMIjOARnuHFyZ0n59V5m7euOYuZE/gD5/0HUOKXIQ==</latexit><latexit sha1_base64="Ep7dpV5F0qAbMZHO1TqqKC99+8E=">AAAB+XicbVC7SgNBFL3rM8bXqqXNkCBYhV0bLYM2lhHygmxYZiezyZDZ2WUegbDkA/wCGxsLRWz9BP/ARvwbJ49CEw9cOJxzL/feE2WcKe15387a+sbm1nZhp7i7t39w6B4dN1VqJKENkvJUtiOsKGeCNjTTnLYzSXEScdqKhjdTvzWiUrFU1PU4o90E9wWLGcHaSqHrBokJ80CYkE4CzlE9dMtexZsBrRJ/QcrVUlC6f/j4qoXuZ9BLiUmo0IRjpTq+l+lujqVmhNNJMTCKZpgMcZ92LBU4oaqbzy6foDOr9FCcSltCo5n6eyLHiVLjJLKdCdYDtexNxf+8jtHxVTdnIjOaCjJfFBuOdIqmMaAek5RoPrYEE8nsrYgMsMRE27CKNgR/+eVV0ryo+F7Fv7NpXMMcBTiFEpyDD5dQhVuoQQMIjOARnuHFyZ0n59V5m7euOYuZE/gD5/0HUOKXIQ==</latexit><latexit sha1_base64="cYzbZ1Lvkw4ZNOQ6vIPLk3M3fM4=">AAAB+XicbVDLSsNAFL2pr1pfUZduBovgqiRudFl047JCX9CEMJlO2qGTSZhHoYT+iRsXirj1T9z5N07bLLT1wIXDOfdy7z1xzpnSnvftVLa2d3b3qvu1g8Oj4xP39KyrMiMJ7ZCMZ7IfY0U5E7Sjmea0n0uK05jTXjx5WPi9KZWKZaKtZzkNUzwSLGEEaytFrhukJioCYSI6DzhH7citew1vCbRJ/JLUoUQrcr+CYUZMSoUmHCs18L1chwWWmhFO57XAKJpjMsEjOrBU4JSqsFhePkdXVhmiJJO2hEZL9fdEgVOlZmlsO1Osx2rdW4j/eQOjk7uwYCI3mgqyWpQYjnSGFjGgIZOUaD6zBBPJ7K2IjLHERNuwajYEf/3lTdK9afhew3/y6s37Mo4qXMAlXIMPt9CER2hBBwhM4Rle4c0pnBfn3flYtVaccuYc/sD5/AF8CZOH</latexit>
Diffusing out
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Diffusion time:
Mean free path
Radius of the core
Carrying away binding energy of 10#$Ergs
Diffusing out
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Diffusion time:
Mean free path
Radius of the core
Carrying away binding energy of 10#$Ergs Consistent with 1987a
Effects of new light particles
´ Light mass<T=few 10 MeV
´ Energy loss: Upper and Lower bounds on coupling
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Below the upper bound production rate is too lowto affect energy loss rate.
Effects of new light particles
´ Light mass<T=few 10 MeV
´ Energy loss: Upper and Lower bounds on coupling
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Above the lower bound, the mean free path is too shortCompared to the core size: No effect on convection
Effects of new light particles
´ Light mass<T=few 10 MeV
´ Energy loss: Upper and Lower bounds on coupling
´ Shortening of mean free path Prolonging the diffusion time
´ Converting flavors: imprint in spectrum and maybe change of EoS
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Decay length of scalar
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✓10�5
y⌫
◆2E�
10 MeV
✓5 MeV
m�
◆2
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Coupling to both neutrino and baryons
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Change of EOS FOR LNV
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IMPACT ON NEUTRINO OSCILLATION?
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NO IMPACT ON NEUTRINO OSCILLATION
Neutrinoless double beta decay
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Gando et al. (KamLAND-ZEN), PRL 86 (2012) 021601
Experiments to test
Reactor experiments: CONUS
Solar neutrino interaction in dark matter detectors
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Coherent Elastic neutrino Nucleus scattering
COHERENT Source: Pion and Muon decay at rest
CONUS
´ Germanium detector 17 m away from reactor core
´ Thermal power of 3.9 GW in Brokdorf
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Recoil energy
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No interference
Coupling to nucleus
Y.F., M Lindner, W. Rodejohann and Xu,JHEP 1805 (2018) 066
Coupling to nucleus
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Belanger et al., Comput Phys Commun 180 (2009) 747
Crivellin et al, PRD89 (2014) 054021; Hoferichter et al, PRL 115 (2015)092301; Jonnarka and Walker-Loud, PRD 87 (2013) 114510
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Threshold on recoil energy:
Future of CONUS
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COHERENT
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COHERENT100: 10 times better statistical and systematic uncertainties
LNC case
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LNV case
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CONUS can help to probe new Yukawa couplings of neutrinos with light (MeVish) scalar that can lead to drastic change in supernova evolution
Thank you
"धन्यवाद्"
Backup slides
´Observational consequences
Emission in Supernova
´ Similar to
´ Reduced mean free path for
Kamada and Yu, arXiv:1504.00711
High energy cosmic neutrino
´ Kamada and Yu, arXiv:1504.00711
Background neutrino at rest
Dip or gap in ICECUBE spectrum
´ Theoretical prediction of dip in 400 TeV to PeV is robust!
´ Testing model
Maltoni and Gonzalez-Garcia, JHEP 2013
Kamada and Yu, 1504.00711
Yukawa coupling of neutrinos
Basis change:
Mix:
No mixing:
Majorana masses
If there is no Majorana mass for right-handed neutrinos:
1)
2) Smallness of neutrino mass
Majorana masses
Neutrino trident scattering
´ CCFR collaboration:
´ CHARM II collaboration
PRL66 (1991)
PLB 245 (1990)
Neutrino trident scattering
Altmannshofer et al., PRL113 (2014)
Davidson, Pena-Garay, Rius, SantaMaria, JHEP 2003
NuTeV: Muon neutrino energy~75 GeV
Davidson, Pena-Garay, Rius, SantaMaria, JHEP 2003
Standard coherent interaction
