non-standard interactions of...

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

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

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

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

LMA-DARK solution

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

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.

Huang, Ohlsson and Zhou, PRD 97 (2018) 075009

LNC Yukawa and early universe

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

Diffusion time:

Mean free path

Radius of the core

Carrying away binding energy of 10#$Ergs

Diffusing out

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

Below the upper bound production rate is too lowto affect energy loss rate.

Above the lower bound, the mean free path is too shortCompared to the core size: No effect on convection

´ Shortening of mean free path Prolonging the diffusion time

´ Converting flavors: imprint in spectrum and maybe change of EoS

Decay length of scalar

✓10�5

◆2E�

10 MeV

✓5 MeV

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Coupling to both neutrino and baryons

Change of EOS FOR LNV

IMPACT ON NEUTRINO OSCILLATION?

NO IMPACT ON NEUTRINO OSCILLATION

Neutrinoless double beta decay

Gando et al. (KamLAND-ZEN), PRL 86 (2012) 021601

Experiments to test

Reactor experiments: CONUS

Solar neutrino interaction in dark matter detectors

Coherent Elastic neutrino Nucleus scattering

COHERENT Source: Pion and Muon decay at rest

´ Germanium detector 17 m away from reactor core

´ Thermal power of 3.9 GW in Brokdorf

Recoil energy

No interference

Coupling to nucleus

Y.F., M Lindner, W. Rodejohann and Xu,JHEP 1805 (2018) 066

Coupling to nucleus

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

Threshold on recoil energy:

Future of CONUS

COHERENT

COHERENT100: 10 times better statistical and systematic uncertainties

LNC case

LNV case

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:

No mixing:

Majorana masses

If there is no Majorana mass for right-handed neutrinos:

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)

NuTeV: Muon neutrino energy~75 GeV

Standard coherent interaction

non-standard interactions of...

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