Constraining new physics with Borexino Phase-II spectral data

Coloma, Pilar; Gonzalez-Garcia, M. C.; Maltoni, Michele; Pinheiro, João Paulo; Urrea, Salvador

doi:10.1007/jhep07(2022)138

Cited by 17 publications

(12 citation statements)

References 54 publications

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“…In recent years, neutrino experiments [12][13][14][15][16][17][18][19][20][21][22][23] and dark-matter direct detection experiments [24][25][26][27][28] have become increasingly important tools for studying the physics beyond the Standard Model [29][30][31][32][33][34][35][36][37][38][39][40][41][42][43]. Among these experiments, XENONnT [27] and Borexino [15][16][17] are particularly noteworthy for their sensitivity to relatively low-energy new physics.…”

Section: Introductionmentioning

confidence: 99%

Probing non-standard neutrino interactions with interference: insights from dark matter and neutrino experiments

Park

Tomar

2023

J. Cosmol. Astropart. Phys.

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Neutrino-electron scattering experiments play a crucial role in investigating the non-standard interactions of neutrinos. In certain models, these interactions can include interference terms that may affect measurements. Next-generation direct detection experiments, designed primarily for dark-matter searches, are also getting sensitive to probe the neutrino properties. We utilise the data from XENONnT, a direct detection experiment, and Borexino, a low-energy solar neutrino experiment, to investigate the impact of interference on non-standard interactions. Our study considers models with an additional U(1) B-L , including U(1), U(1) L e - L µ , and U(1) L e - L τ , to investigate the impact of interference on non-standard neutrino interactions. We demonstrate that this interference can lead to a transition between the considered non-standard interaction models in the energy range relevant to both the XENONnT and Borexino experiments. This transition can be used to distinguish among the considered models if any signals are observed at direct detection or neutrino experiments. Our findings underscore the importance of accounting for the interference and incorporating both direct detection and solar neutrino experiments to gain a better understanding of neutrino interactions and properties.

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Section: Introductionmentioning

confidence: 99%

Probing non-standard neutrino interactions with interference: insights from dark matter and neutrino experiments

Park

Tomar

2023

J. Cosmol. Astropart. Phys.

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“…Neutrino experiments that probe electron-neutrino or coherent elastic neutrino-nucleus scattering (CEνNS) are sensitive to the contribution of X to their amplitudes [100][101][102][103][104][105][106][107]. Experiments searching decays into invisible final states can also be used to set constraints with the assumption that invisible states can be treated as decays to neutrino final states [108][109][110][111][112].…”

Section: Other Constraintsmentioning

confidence: 99%

Cosmological implications of gauged U(1)_B-L on ΔN _eff in the CMB and BBN

Esseili,

Kribs

2024

J. Cosmol. Astropart. Phys.

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We calculate the effects of a light, very weakly-coupled boson X arising from a spontaneously broken U(1) B-L symmetry on ΔN eff as measured by the CMB and Yp from BBN. Our focus is the mass range 1 eV ≲ mX ≲ 100 MeV; masses lighter than about an eV have strong constraints from fifth-force law constraints, while masses heavier than about 100 MeV are constrained by other probes, including terrestrial experiments. We do not assume N eff began in thermal equilibrium with the SM; instead, we allow N eff to freeze-in from its very weak interactions with the SM. We find U(1) B-L is more strongly constrained by ΔN eff than previously considered. The bounds arise from the energy density in electrons and neutrinos slowly siphoned off into N eff bosons, which become nonrelativistic, redshift as matter, and then decay, dumping their slightly larger energy density back into the SM bath causing ΔN eff > 0. While some of the parameter space has complementary constraints from stellar cooling, supernova emission, and terrestrial experiments, we find future CMB observatories including Simons Observatory and CMB-S4 can access regions of mass and coupling space not probed by any other method. In gauging U(1) B-L , we assume the [U(1) B-L ]3 anomaly is canceled by right-handed neutrinos, and so our ΔN eff calculations have been carried out in two scenarios: neutrinos have Dirac masses, or, right-handed neutrinos acquire Majorana masses. In the latter scenario, we comment on the additional implications of thermalized right-handed neutrinos decaying during BBN. We also briefly consider the possibility that X decays into dark sector states. If these states behave as radiation, we find weaker constraints, whereas if they are massive, there are stronger constraints, though now from ΔN eff < 0.

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“…We compare our results with the existing limits from other CEνNS experiments, in particular CONNIE [110], CONUS [12] and Dresden-II [26], from the analysis given in ref. [88] of two multi-ton DM experiments (namely XENONnT [111] and LZ [112]), from the analysis of solar neutrino data collected by Borexino [113], from collider experiments [43], including BaBar [114] and LHCb [115], and from rare meson decays at NA48 [116]. In the ∼ 1 GeV mass region, we also show bounds from beam-dump experiments [41,117], including E141 [118,119], E137 [120], E774 [121], KEK [122], Orsay [123], U70/ν-CAL I [124,125], CHARM [126,127], NO-MAD [128], NA64 [129,130] and the fixed target experiments A1 [131] and APEX [132].…”

Section: Light Mediatorsmentioning

confidence: 99%

Physics implications of a combined analysis of COHERENT CsI and LAr data

Romeri

Miranda

Papoulias

et al. 2023

J. High Energ. Phys.

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The observation of coherent elastic neutrino nucleus scattering has opened the window to many physics opportunities. This process has been measured by the COHERENT Collaboration using two different targets, first CsI and then argon. Recently, the COHERENT Collaboration has updated the CsI data analysis with a higher statistics and an improved understanding of systematics. Here we perform a detailed statistical analysis of the full CsI data and combine it with the previous argon result. We discuss a vast array of implications, from tests of the Standard Model to new physics probes. In our analyses we take into account experimental uncertainties associated to the efficiency as well as the timing distribution of neutrino fluxes, making our results rather robust. In particular, we update previous measurements of the weak mixing angle and the neutron root mean square charge radius for CsI and argon. We also update the constraints on new physics scenarios including neutrino nonstandard interactions and the most general case of neutrino generalized interactions, as well as the possibility of light mediators. Finally, constraints on neutrino electromagnetic properties are also examined, including the conversion to sterile neutrino states. In many cases, the inclusion of the recent CsI data leads to a dramatic improvement of bounds.

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Constraining new physics with Borexino Phase-II spectral data

Cited by 17 publications

References 54 publications

Probing non-standard neutrino interactions with interference: insights from dark matter and neutrino experiments

Probing non-standard neutrino interactions with interference: insights from dark matter and neutrino experiments

Cosmological implications of gauged U(1)_B-L on ΔN _eff in the CMB and BBN

Physics implications of a combined analysis of COHERENT CsI and LAr data

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Constraining new physics with Borexino Phase-II spectral data

Cited by 17 publications

References 54 publications

Probing non-standard neutrino interactions with interference: insights from dark matter and neutrino experiments

Probing non-standard neutrino interactions with interference: insights from dark matter and neutrino experiments

Cosmological implications of gauged U(1) B-L on ΔN eff in the CMB and BBN

Physics implications of a combined analysis of COHERENT CsI and LAr data

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Product

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Cosmological implications of gauged U(1)_B-L on ΔN _eff in the CMB and BBN