Search for exotic interactions of solar neutrinos in the CDEX-10 experiment X. P. Geng1L. T. Yang1Q. Yue1K. J. Kang1Y. J. Li1H. P. An1 2Greeshma C.3J. P. Chang4 Y. H. Chen5J. P. Cheng1 6W. H. Dai1Z. Deng1C. H. Fang7H. Gong1Q. J. Guo8X. Y. Guo5

2025-05-03 0 0 869.19KB 6 页 10玖币

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Search for exotic interactions of solar neutrinos in the CDEX-10 experiment

X. P. Geng,1L. T. Yang,1, ∗Q. Yue,1, †K. J. Kang,1Y. J. Li,1H. P. An,1, 2 Greeshma C.,3, ‡J. P. Chang,4

Y. H. Chen,5J. P. Cheng,1, 6 W. H. Dai,1Z. Deng,1C. H. Fang,7H. Gong,1Q. J. Guo,8X. Y. Guo,5

L. He,4S. M. He,5J. W. Hu,1H. X. Huang,9T. C. Huang,10 H. T. Jia,7X. Jiang,7S. Karmakar,3, ‡

H. B. Li,3, ‡J. M. Li,1J. Li,1Q. Y. Li,7R. M. J. Li,7X. Q. Li,11 Y. L. Li,1Y. F. Liang,1B. Liao,6

F. K. Lin,3, ‡S. T. Lin,7J. X. Liu,1S. K. Liu,7Y. D. Liu,6Y. Liu,7Y. Y. Liu,6Z. Z. Liu,1H. Ma,1

Y. C. Mao,8Q. Y. Nie,1J. H. Ning,5H. Pan,4N. C. Qi,5J. Ren,9X. C. Ruan,9Z. She,1M. K. Singh,3, 12, ‡

T. X. Sun,6C. J. Tang,7W. Y. Tang,1Y. Tian,1G. F. Wang,6L. Wang,13 Q. Wang,1, 2 Y. F. Wang,1

Y. X. Wang,8H. T. Wong,3, ‡S. Y. Wu,5Y. C. Wu,1H. Y. Xing,7R. Xu,1Y. Xu,11 T. Xue,1Y. L. Yan,7

N. Yi,1C. X. Yu,11 H. J. Yu,4J. F. Yue,5M. Zeng,1Z. Zeng,1B. T. Zhang,1F. S. Zhang,6L. Zhang,7

Z. H. Zhang,1Z. Y. Zhang,1K. K. Zhao,7M. G. Zhao,11 J. F. Zhou,5Z. Y. Zhou,9and J. J. Zhu7

(CDEX Collaboration)

Y. C. Wu14

1Key Laboratory of Particle and Radiation Imaging (Ministry of Education)

and Department of Engineering Physics, Tsinghua University, Beijing 100084

2Department of Physics, Tsinghua University, Beijing 100084

3Institute of Physics, Academia Sinica, Taipei 11529

4NUCTECH Company, Beijing 100084

5YaLong River Hydropower Development Company, Chengdu 610051

6College of Nuclear Science and Technology, Beijing Normal University, Beijing 100875

7College of Physics, Sichuan University, Chengdu 610065

8School of Physics, Peking University, Beijing 100871

9Department of Nuclear Physics, China Institute of Atomic Energy, Beijing 102413

10Sino-French Institute of Nuclear and Technology, Sun Yat-sen University, Zhuhai 519082

11School of Physics, Nankai University, Tianjin 300071

12Department of Physics, Banaras Hindu University, Varanasi 221005

13Department of Physics, Beijing Normal University, Beijing 100875

14Department of Physics and Institute of Theoretical Physics, Nanjing Normal University, Nanjing, 210023

(Dated: June 5, 2023)

We investigate exotic neutrino interactions using the 205.4 kg·day dataset from the CDEX-10

experiment at the China Jinping Underground Laboratory. New constraints on the mass and cou-

plings of new gauge bosons are presented. Two nonstandard neutrino interactions are considered: a

U(1)B−Lgauge-boson-induced interaction between an active neutrino and electron/nucleus, and a

dark-photon-induced interaction between a sterile neutrino and electron/nucleus via kinetic mixing

with a photon. This work probes an unexplored parameter space involving sterile neutrino coupling

with a dark photon. New laboratory limits are derived on dark photon masses below 1 eV/c2at

some benchmark values of ∆m2

41 and g′2sin22θ14.

I. INTRODUCTION

Various cosmological and astrophysical observations at

diﬀerent scales reveal phenomena beyond the Standard

Model (SM) [1]. The measurement of nonstandard inter-

action (NSI) in the neutrino sector is an attractive ap-

proach to probe beyond-SM physics [2, 3]. Current exper-

imental eﬀorts on neutrino NSI are conducted with diﬀer-

ent neutrino sources, such as reactor neutrinos [4–12], ac-

celerator neutrinos [13–16], and radioactive sources [17–

21]. In addition to these terrestrial sources, NSI can

also be probed with neutrinos from astrophysical sources,

∗Corresponding author: yanglt@mail.tsinghua.edu.cn

†Corresponding author: yueq@mail.tsinghua.edu.cn

‡Participating as a member of TEXONO Collaboration

such as stars [22], supernovae [23, 24], terrestrial atmo-

sphere [25], and others [26]. In this paper, we inves-

tigate two attractive exotic neutrino NSIs, where new

gauge boson mediators (generically denoted as A′) from

the hidden sector couple active or sterile neutrinos with

SM particles. Constraints are placed with data from the

CDEX-10 experiment [27–32] using solar neutrino (ν⊙)

as the source.

The ﬁrst NSI model is based on a gauged U(1)B−L

symmetry [33, 34] with the corresponding A′interacting

with SM particles with a nonzero B−L number (baryon

number minus lepton number) at tree level. This global

U(1) symmetry appears in grand uniﬁed theory and will

not be violated by chiral and gravitational anomalies.

The symmetry can give rise to neutrino mass when spon-

taneously broken, and the corresponding A′is a dark

matter (DM) candidate. The free parameters are the

new gauge coupling constant (gB−L) and the gauge boson

arXiv:2210.01604v2 [hep-ex] 2 Jun 2023

mass (MA′). This additional U(1)B−Lmediator would

lead to a new interaction between the neutrino and the

SM particles which is measurable by enhanced event

rates. The second NSI model considers the existence of

a sterile neutrino (νs) which couples with A′, called a

dark photon, under a new gauged symmetry U(1)′[33].

The dark photon is a popular DM candidate and can

be a portal between the SM and the dark sector. Ob-

servable interactions between νsand SM matter are in-

duced by A′. The coupling strength between A′and νs

is parametrized by g′, while that with SM particles with

charge Qis via its kinetic mixing (ε) with the SM pho-

tons. Other interesting NSI models with an extra U(1)

gauge boson [35, 36] are beyond the scope of this work.

The p-type point contact germanium (PPCGe) semi-

conductor in ionization mode is ideal for the studies of

exotic processes due to its ultralow energy threshold of

O(100 eVee) (“eVee” represents the electron equivalent

energy derived from energy calibration) and low back-

ground level of O(1 count kg−1keVee−1day−1) [37, 38].

It has been adopted by the CDEX experiment [27–32, 39–

44] for searches of DM and beyond-SM NSI at the China

Jinping Underground Laboratory (CJPL) where the rock

overburden is about 2400 m [45]. The second phase of the

CDEX experiment, CDEX-10, takes data with a 10-kg

PPCGe detector array, consisting of three triple-element

PPCGe detector strings encapsulated in copper vacuum

tubes and immersed in liquid nitrogen which serves both

for cooling and shielding. The CDEX-10 experimental

conﬁguration was described in Refs. [27, 32]. Data tak-

ing started in February 2017, and the physics analysis

threshold is 160 eVee [27]. Previous scientiﬁc results were

published in Refs. [27–31].

II. DATA ANALYSIS

The data analysis of this work is based on a 205.4

kg·day dataset from CDEX-10 [28–31] and follows the es-

tablished procedures of previous works [27, 28, 32, 42, 43].

The energy calibration was performed with zero energy

(deﬁned by random trigger events) and the internal cos-

mogenic K-shell x-ray peaks: 8.98 keVee of 65Zn and

10.37 keVee of 68,71Ge. The signal events are identiﬁed

after pedestal noise cut, physics events selection, and

bulk/surface events discrimination [46, 47]. The mea-

sured energy spectrum in the detector (Edet) in keVee

units after physics event selections and eﬃciency correc-

tions is shown in Fig. 1. The physics analysis threshold is

set to be 160 eVee at which the combined signal eﬃciency

(including the trigger eﬃciency and the eﬃciency for the

pulse shape discrimination) is 4.5% [32]. The characteris-

tic K-shell x-ray peaks from internal cosmogenic radionu-

clides like 68Ge, 68Ga, 65Zn, 55Fe, 54Mn, and 49V can be

identiﬁed. Their intensities are derived from the best

ﬁt of the spectrum [27]. At the sub-keVee energy range

relevant to this analysis, background events are domi-

nated by Compton scattering of high-energy gamma rays

FIG. 1. The measured energy spectrum with error bars in-

cluding both the statistical and systematical uncertainties

based on the 205.4 kg·day dataset of the CDEX-10 exper-

iment [28–31]. The bin width is 100 eVee and the energy

range is 0.16–11.76 keVee. The characteristic K-shell x-ray

peaks from internal cosmogenic radionuclides are marked by

the isotope symbols in color. Both the best ﬁt curve of the

measured energy spectrum in 4–11.8 keV, which is the red

line, and the contributions of these radionuclides derived by

the best ﬁt are superimposed. Displayed in the inset are the

contributions of L- and M-shell x-ray peaks derived from the

corresponding K-shell line intensities [48]. The L-shell x-ray

peaks are shown in solid lines. The dashed line represents the

M-shell x-ray peak of 68Ge.

and internal radioactivity from long-lived cosmogenic iso-

topes. Figure 2 shows the residual spectrum in the re-

gion of 0.16–2.16 keVee after subtracting the contribu-

tions from L- and M-shell x-ray peaks which are derived

from the corresponding K-shell line intensities [27–31].

This is illustrated in the inset of Fig. 1. The count rate

is several orders of magnitude larger than the predictions

of SM ν⊙interaction.

A minimum-χ2analysis [27, 28, 31, 41] is applied to

the residual spectrum in the range 0.16–2.16 keVee, in

which χ2is deﬁned as

χ2=X

[ni−Si−B]2

∆2

,(1)

where niis the measured count at the ith energy bin,

and Siis the expected event rate due to the neutrino

NSI model being probed. ∆iis the combination of the

statistical and systematic uncertainties [27], and Bis the

ﬂat background contribution from the Compton scatter-

ing of high-energy gamma rays. The best estimator of

the couplings (see discussion below) at certain mediator

mass MA′is evaluated by minimizing the χ2values. Up-

per limits at 90% conﬁdence level (CL) are derived by

the uniﬁed approach [50].

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SearchforexoticinteractionsofsolarneutrinosintheCDEX-10experimentX.P.Geng,1L.T.Yang,1,∗Q.Yue,1,†K.J.Kang,1Y.J.Li,1H.P.An,1,2GreeshmaC.,3,‡J.P.Chang,4Y.H.Chen,5J.P.Cheng,1,6W.H.Dai,1Z.Deng,1C.H.Fang,7H.Gong,1Q.J.Guo,8X.Y.Guo,5L.He,4S.M.He,5J.W.Hu,1H.X.Huang,9T.C.Huang,10H.T.Jia,7X.Jiang,7S.Karmakar,3...

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Search for exotic interactions of solar neutrinos in the CDEX-10 experiment X. P. Geng1L. T. Yang1Q. Yue1K. J. Kang1Y. J. Li1H. P. An1 2Greeshma C.3J. P. Chang4 Y. H. Chen5J. P. Cheng1 6W. H. Dai1Z. Deng1C. H. Fang7H. Gong1Q. J. Guo8X. Y. Guo5.pdf

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Search for exotic interactions of solar neutrinos in the CDEX-10 experiment X. P. Geng1L. T. Yang1Q. Yue1K. J. Kang1Y. J. Li1H. P. An1 2Greeshma C.3J. P. Chang4 Y. H. Chen5J. P. Cheng1 6W. H. Dai1Z. Deng1C. H. Fang7H. Gong1Q. J. Guo8X. Y. Guo5

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