non-standard interaction of solar neutrinos in dark matter ... · dark matter detectors shu liao...
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![Page 1: Non-Standard Interaction of Solar Neutrinos in Dark Matter ... · Dark Matter Detectors Shu Liao Texas A&M University Collaboration with: J. Dent, B. Dutta, J. Newstead, L. Strigari](https://reader036.vdocuments.us/reader036/viewer/2022081613/5fba264de573210e290351f0/html5/thumbnails/1.jpg)
MotivationCombination of oscillation and CEnNS
Future work and conclusion
Non-Standard Interaction of Solar Neutrinos inDark Matter Detectors
Shu Liao
Texas A&M University
Collaboration with: J. Dent, B. Dutta, J. Newstead, L. Strigariand J. Walker
Shu Liao Non-Standard Interaction of Solar Neutrinos in Dark Matter Detectors
![Page 2: Non-Standard Interaction of Solar Neutrinos in Dark Matter ... · Dark Matter Detectors Shu Liao Texas A&M University Collaboration with: J. Dent, B. Dutta, J. Newstead, L. Strigari](https://reader036.vdocuments.us/reader036/viewer/2022081613/5fba264de573210e290351f0/html5/thumbnails/2.jpg)
MotivationCombination of oscillation and CEnNS
Future work and conclusion
Outline
1 MotivationNon-standard interactions of neutrinoTransition probability of solar neutrinoCurrent constrains
2 Combination of oscillation and CEnNSExpected number of events under NSIOscillation effects
3 Future work and conclusionResolving degeneraciesConclusion
Shu Liao Non-Standard Interaction of Solar Neutrinos in Dark Matter Detectors
![Page 3: Non-Standard Interaction of Solar Neutrinos in Dark Matter ... · Dark Matter Detectors Shu Liao Texas A&M University Collaboration with: J. Dent, B. Dutta, J. Newstead, L. Strigari](https://reader036.vdocuments.us/reader036/viewer/2022081613/5fba264de573210e290351f0/html5/thumbnails/3.jpg)
MotivationCombination of oscillation and CEnNS
Future work and conclusion
Non-standard interactions of neutrinoTransition probability of solar neutrinoCurrent constrains
Non-standard interactions of neutrinos
General four fermion interaction:
Lint = 2p2GF ⌫↵L�
µ⌫�L
⇣✏fL↵� fL�µfL + ✏fR↵� fR�µfR
⌘
⌫�
⌫↵
f
f
= SM +BSM
Shu Liao Non-Standard Interaction of Solar Neutrinos in Dark Matter Detectors
![Page 4: Non-Standard Interaction of Solar Neutrinos in Dark Matter ... · Dark Matter Detectors Shu Liao Texas A&M University Collaboration with: J. Dent, B. Dutta, J. Newstead, L. Strigari](https://reader036.vdocuments.us/reader036/viewer/2022081613/5fba264de573210e290351f0/html5/thumbnails/4.jpg)
MotivationCombination of oscillation and CEnNS
Future work and conclusion
Non-standard interactions of neutrinoTransition probability of solar neutrinoCurrent constrains
Differential cross section
Differential cross section of ⌫� + f ! ⌫↵ + f as a function of recoilenergy Er:
d�
dEr=
2
⇡G2
Fmf⇥"���✏fL↵�
���2+���✏fR↵�
���2✓1� Er
E⌫
◆2
� 1
2
⇣✏fL⇤↵� ✏fR↵� + ✏fL↵�✏
fR⇤↵�
⌘ mfEr
E2⌫
#
Shu Liao Non-Standard Interaction of Solar Neutrinos in Dark Matter Detectors
![Page 5: Non-Standard Interaction of Solar Neutrinos in Dark Matter ... · Dark Matter Detectors Shu Liao Texas A&M University Collaboration with: J. Dent, B. Dutta, J. Newstead, L. Strigari](https://reader036.vdocuments.us/reader036/viewer/2022081613/5fba264de573210e290351f0/html5/thumbnails/5.jpg)
MotivationCombination of oscillation and CEnNS
Future work and conclusion
Non-standard interactions of neutrinoTransition probability of solar neutrinoCurrent constrains
Cross section on nucleus
✏L↵↵ ! 1
2Z✏pV↵↵ +
1
2(Z+ � Z�) ✏
pA↵↵ +
1
2N✏nV↵↵ +
1
2(N+ �N�) ✏
nA↵↵
✏R↵↵ ! 1
2Z✏pV↵↵ � 1
2(Z+ � Z�) ✏
pA↵↵ +
1
2N✏nV↵↵ � 1
2(N+ �N�) ✏
nA↵↵
d�
dEr! d�
dEr⇥ F 2
�Q2
�
✏pV↵↵ =1
2� 2 sin2 ✓w + 2✏uV↵↵ + ✏dV↵↵
✏pA↵↵ =1
2+ 2✏uA↵↵ + ✏dA↵↵
✏nV↵↵ = �1
2+ ✏uV↵↵ + 2✏dV↵↵
✏pA↵↵ = �1
2+ ✏uA↵↵ + 2✏dA↵↵
Shu Liao Non-Standard Interaction of Solar Neutrinos in Dark Matter Detectors
![Page 6: Non-Standard Interaction of Solar Neutrinos in Dark Matter ... · Dark Matter Detectors Shu Liao Texas A&M University Collaboration with: J. Dent, B. Dutta, J. Newstead, L. Strigari](https://reader036.vdocuments.us/reader036/viewer/2022081613/5fba264de573210e290351f0/html5/thumbnails/6.jpg)
MotivationCombination of oscillation and CEnNS
Future work and conclusion
Non-standard interactions of neutrinoTransition probability of solar neutrinoCurrent constrains
Transition probability of solar neutrino
The propagation of neutrino is described by:
H�↵ =
Udiag
✓0,
�m221
2E,�m2
31
2E
◆U †
�
�↵
+p2GF
X
f
nf
⇣�ef�e↵ + ✏f�↵
⌘
U : mixing matrix, �m2ij = m2
i �m2j , nf : number density of
fermion f .Neutrino propagates through the sun adiabatically (diagonalize Hinto UdiagU †):
P�!↵ =���U (t)↵k
���2��A1
jk
��2��A2ij
��2���U (0)�i
���2
A: transition probability between mass eigenstate when resonancehappens.
Shu Liao Non-Standard Interaction of Solar Neutrinos in Dark Matter Detectors
![Page 7: Non-Standard Interaction of Solar Neutrinos in Dark Matter ... · Dark Matter Detectors Shu Liao Texas A&M University Collaboration with: J. Dent, B. Dutta, J. Newstead, L. Strigari](https://reader036.vdocuments.us/reader036/viewer/2022081613/5fba264de573210e290351f0/html5/thumbnails/7.jpg)
MotivationCombination of oscillation and CEnNS
Future work and conclusion
Non-standard interactions of neutrinoTransition probability of solar neutrinoCurrent constrains
Current constraints
(a) Gonzalez-Garcia et al,
arXiv:1307.3092
(b) Coloma et al, arXiv:1701.04828
Figure: Current constraints
Shu Liao Non-Standard Interaction of Solar Neutrinos in Dark Matter Detectors
![Page 8: Non-Standard Interaction of Solar Neutrinos in Dark Matter ... · Dark Matter Detectors Shu Liao Texas A&M University Collaboration with: J. Dent, B. Dutta, J. Newstead, L. Strigari](https://reader036.vdocuments.us/reader036/viewer/2022081613/5fba264de573210e290351f0/html5/thumbnails/8.jpg)
MotivationCombination of oscillation and CEnNS
Future work and conclusion
Expected number of events under NSIOscillation effects
Electron scattering ⌫� + e ! ⌫↵ + e
Figure: Number of events above an equivalent electron recoil energythreshold of 1 keV as each ✏ varies over its allowable range (blue curves).Orange curve: SM contribution.
Shu Liao Non-Standard Interaction of Solar Neutrinos in Dark Matter Detectors
![Page 9: Non-Standard Interaction of Solar Neutrinos in Dark Matter ... · Dark Matter Detectors Shu Liao Texas A&M University Collaboration with: J. Dent, B. Dutta, J. Newstead, L. Strigari](https://reader036.vdocuments.us/reader036/viewer/2022081613/5fba264de573210e290351f0/html5/thumbnails/9.jpg)
MotivationCombination of oscillation and CEnNS
Future work and conclusion
Expected number of events under NSIOscillation effects
Nucleus scattering ⌫� +N ! ⌫↵ +N
Figure: Number of events above an equivalent nucleus recoil energythreshold of 1 keV as each e varies over its allowable range (blue curves).Orange curve: SM contribution.
Shu Liao Non-Standard Interaction of Solar Neutrinos in Dark Matter Detectors
![Page 10: Non-Standard Interaction of Solar Neutrinos in Dark Matter ... · Dark Matter Detectors Shu Liao Texas A&M University Collaboration with: J. Dent, B. Dutta, J. Newstead, L. Strigari](https://reader036.vdocuments.us/reader036/viewer/2022081613/5fba264de573210e290351f0/html5/thumbnails/10.jpg)
MotivationCombination of oscillation and CEnNS
Future work and conclusion
Expected number of events under NSIOscillation effects
LMA-Dark solution
✓12 ! ⇡
2� ✓12
✓13 ! ⇡ � ✓13
� ! ⇡ � �
�m231 ! ��m2
32
✏ ! �✏⇤
H ! �H⇤
Figure: Number of events for LMA-d solution withdifferent threshold energies.
Shu Liao Non-Standard Interaction of Solar Neutrinos in Dark Matter Detectors
![Page 11: Non-Standard Interaction of Solar Neutrinos in Dark Matter ... · Dark Matter Detectors Shu Liao Texas A&M University Collaboration with: J. Dent, B. Dutta, J. Newstead, L. Strigari](https://reader036.vdocuments.us/reader036/viewer/2022081613/5fba264de573210e290351f0/html5/thumbnails/11.jpg)
MotivationCombination of oscillation and CEnNS
Future work and conclusion
Expected number of events under NSIOscillation effects
Threshold
Figure: Number of events with different threshold energies.
Shu Liao Non-Standard Interaction of Solar Neutrinos in Dark Matter Detectors
![Page 12: Non-Standard Interaction of Solar Neutrinos in Dark Matter ... · Dark Matter Detectors Shu Liao Texas A&M University Collaboration with: J. Dent, B. Dutta, J. Newstead, L. Strigari](https://reader036.vdocuments.us/reader036/viewer/2022081613/5fba264de573210e290351f0/html5/thumbnails/12.jpg)
MotivationCombination of oscillation and CEnNS
Future work and conclusion
Expected number of events under NSIOscillation effects
Oscillation vs. no oscillation
✏eLee = 0.052 ✏uee = 0.2 ✏dee = 0.17U�mU † +
p2Gfdiag (1, 0, 0) +
p2Gf ✏ 1.10 0.69 0.69
U�mU † +p2Gfdiag (1, 0, 0) +
p2Gf ✏ 1.12 0.67 0.67
U�mU † +p2Gfdiag (1, 0, 0) +
p2Gf ✏ 1.13 0.44 0.44
U�mU † +p2Gfdiag (1, 0, 0) +
p2Gf ✏ 1.72 3.88⇥ 10�5 1.18⇥ 10�3
Table: Ratio to only SM prediction N/NSM
Shu Liao Non-Standard Interaction of Solar Neutrinos in Dark Matter Detectors
![Page 13: Non-Standard Interaction of Solar Neutrinos in Dark Matter ... · Dark Matter Detectors Shu Liao Texas A&M University Collaboration with: J. Dent, B. Dutta, J. Newstead, L. Strigari](https://reader036.vdocuments.us/reader036/viewer/2022081613/5fba264de573210e290351f0/html5/thumbnails/13.jpg)
MotivationCombination of oscillation and CEnNS
Future work and conclusion
Expected number of events under NSIOscillation effects
Survival probability due to NSI
Figure: Electron neutrino survival probability for the SM (blue) comparedto cases in of NSI.
Shu Liao Non-Standard Interaction of Solar Neutrinos in Dark Matter Detectors
![Page 14: Non-Standard Interaction of Solar Neutrinos in Dark Matter ... · Dark Matter Detectors Shu Liao Texas A&M University Collaboration with: J. Dent, B. Dutta, J. Newstead, L. Strigari](https://reader036.vdocuments.us/reader036/viewer/2022081613/5fba264de573210e290351f0/html5/thumbnails/14.jpg)
MotivationCombination of oscillation and CEnNS
Future work and conclusion
Resolving degeneraciesConclusion
Oscillations
Figure: Oscillation experiment can only detect ✏ee � ✏µµ, Coloma et al.2017
Shu Liao Non-Standard Interaction of Solar Neutrinos in Dark Matter Detectors
![Page 15: Non-Standard Interaction of Solar Neutrinos in Dark Matter ... · Dark Matter Detectors Shu Liao Texas A&M University Collaboration with: J. Dent, B. Dutta, J. Newstead, L. Strigari](https://reader036.vdocuments.us/reader036/viewer/2022081613/5fba264de573210e290351f0/html5/thumbnails/15.jpg)
MotivationCombination of oscillation and CEnNS
Future work and conclusion
Resolving degeneraciesConclusion
Complementarity of various experiments
Reactor + SNS + Solar-DM = constraints on ✏ee � ✏µµ? u and ddegeneracy?
Figure: Combining different result togetherShu Liao Non-Standard Interaction of Solar Neutrinos in Dark Matter Detectors
![Page 16: Non-Standard Interaction of Solar Neutrinos in Dark Matter ... · Dark Matter Detectors Shu Liao Texas A&M University Collaboration with: J. Dent, B. Dutta, J. Newstead, L. Strigari](https://reader036.vdocuments.us/reader036/viewer/2022081613/5fba264de573210e290351f0/html5/thumbnails/16.jpg)
MotivationCombination of oscillation and CEnNS
Future work and conclusion
Resolving degeneraciesConclusion
Conclusion
1 Direct dark matter searches are able to probe NSI parameterspace that cannot be probed by current neutrino experiments.
1 A low threshold detector is more likely to be able to observesignificant number of events
2 Due to interference between SM and BSM, number ofobserved events can be lower than SM expectations.
2 Uncertainties of additional NSI parameters will not only affectthe detection side, but also affect the solar neutrino flux.
Shu Liao Non-Standard Interaction of Solar Neutrinos in Dark Matter Detectors