Solar and supernova neutrinos in DUNE

Solar and supernova neutrinos in DUNE XXI International Workshop on Neutrino Telescopes – October 2, 2025 Daniele Guffanti on behalf of the DUNE Collaboration University & INFN Milano-Bicocca The Deep Underground Neutrino Experiment (DUNE) Open questions in neutrino physics (oscillations): Mass ordering CP violation Octant of θ23 Test the 3-flavor paradigm with unprecedented precision in a single experiment Plenary talk by D. Rivera today at 15:00 The huge DUNE Far Detector complex, 1.5 km underground at the Sanford Underground Research Facility (SURF), offers unique opportunities for non-beam neutrino physics BSM physics Atmospheric neutrinos supernova neutrinos solar neutrinos 2/ 14 D. Guffanti (University & INFN MiB) Solar and supernova neutrinos in DUNE NuTel25, 02.10.2025 Liquid Argon Time Projection Chambers Strong electric field (∼500 V/cm) →ionization electrons collected on readout planes Long absorption length for LAr VUV scintillation light →self-triggering capability DUNE Coll, Phys. Rev. D 107 (2023) 3D tracking with mm-scale resolution Excellent calorimetric performance Topological reconstruction 3/ 14 D. Guffanti (University & INFN MiB) Solar and supernova neutrinos in DUNE NuTel25, 02.10.2025 The DUNE Far Detector Complex Horizontal Drift (HD) module: JINST 15 (2020) 08, T08010 17.5 kt LAr 4 drift volumes, 3.6 m drift Wire charge readout (APA) X-ARAPUCA light detectors integrated in APA Vertical Drift (VD) module: JINST 19 (2024) 08, T08004 17.5 kt LAr 2 drift volumes, 6 m drift Strip charge readout (CRP) LAr + Xe doping for enhanced light yield X-ARAPUCA light detectors on the cathode plane + cryostat membrane 4/ 14 D. Guffanti (University & INFN MiB) Solar and supernova neutrinos in DUNE NuTel25, 02.10.2025 DUNE as a neutrino telescope The significant overburden (4300 m.w.e.), good energy resolution, and huge target mass make an ideal candidate for observation of low-energy neutrinos from astrophysical sources Image credits: Symmetry Magazine 5/ 14 D. Guffanti (University & INFN MiB) Solar and supernova neutrinos in DUNE NuTel25, 02.10.2025 Low-energy neutrino interactions in DUNE 0 20 40 10−1 100 101 102 103 Neutrino energy Eν[MeV] σ(Eν)/atom [10−42 cm2] νeCC ¯νeCC νxNC ¯νxNC νeES ¯νeES νµ,τES ¯νµ,τES νeCC interaction on 40Ar νe+40Ar →e−+40K∗→e−+40K+Nγ νx-e−elastic scattering (ES) νx+e−→νx+e− νxNC interactions on 40Ar DUNE Coll, Eur.Phys.J.C 81 (2021) 5, 423 Ee=10.25 MeV Eν=20.25 MeV 6/ 14 D. Guffanti (University & INFN MiB) Solar and supernova neutrinos in DUNE NuTel25, 02.10.2025 Supernova neutrinos ergs/s) 52 L (10 e ν e ν x ν Infall Neutronization Accretion Cooling 0.1 1 10 <E> (MeV) 6 8 10 12 14 Time (seconds) 2− 10 1− 10 1 Alpha 2.5 3 3.5 4 4.5 DUNE Coll, Eur.Phys.J.C 81 (2021) 5, 423 Core-collapse supernovae (CCSNe): ∼99%of the gravitational energy released in neutrinos Neutrino emission lasts for ∼10 s Neutrino energies in the 1–30 MeV range Only one SN neutrino signal observed: SN1987A in the Large Magellanic Cloud What can we learn from the next Galactic SN? Probe the core-collapse mechanism Neutronization burst, effects of shock waves and turbulence, BH formation... Neutrino properties ∠Study of ν-νinteractions and collective oscillations ∠Possible constraints on neutrino absolute mass ∠Hint of neutrino mass ordering from the neutronization burst 7/ 14 D. Guffanti (University & INFN MiB) Solar and supernova neutrinos in DUNE NuTel25, 02.10.2025 Supernova neutrinos in DUNE primarily sensitive to the νecomponent of the SNB Complementary to other experiments (mainly sensitive to ¯νe) Exp. νe¯νeνx DUNE 89% 4% 7% SK110% 87% 3% JUNO21% 72% 27% Channel Events/40 kton @ 10 kpc Livermore GKVM Garching νeCC 2648 3295 882 ¯νeCC 224 155 23 νxES 341 206 142 Trigger system: Trigger can use both TPC and PDS information, exploiting signal coincidences over the SNB timescale Aims at 95% efficiency @ 20 kpc 1/month false trigger rate Preliminary results for PDS-only trigger: Trigger primitives made of PDS hits + clusters based on space-time information >90% efficiency on a SNB at ≲20 kpc (Milky Way edge) Preliminary 1SK Coll Astropart.Phys. 81 (2016) 2Lu, Li & Zhou Phys.Rev.D 94 (2016) DUNE Coll, Eur.Phys.J.C 81 (2021) 5, 423 8/ 14 D. Guffanti (University & INFN MiB) Solar and supernova neutrinos in DUNE NuTel25, 02.10.2025 Supernova neutrinos in DUNE primarily sensitive to the νecomponent of the SNB Complementary to other experiments (mainly sensitive to ¯νe) Exp. νe¯νeνx DUNE 89% 4% 7% SK110% 87% 3% JUNO21% 72% 27% Channel Events/40 kton @ 10 kpc Livermore GKVM Garching νeCC 2648 3295 882 ¯νeCC 224 155 23 νxES 341 206 142 Trigger system: Trigger can use both TPC and PDS information, exploiting signal coincidences over the SNB timescale Aims at 95% efficiency @ 20 kpc 1/month false trigger rate Preliminary results for PDS-only trigger: Trigger primitives made of PDS hits + clusters based on space-time information >90% efficiency on a SNB at ≲20 kpc (Milky Way edge) Preliminary 1SK Coll Astropart.Phys. 81 (2016) 2Lu, Li & Zhou Phys.Rev.D 94 (2016) DUNE Coll, Eur.Phys.J.C 81 (2021) 5, 423 8/ 14 D. Guffanti (University & INFN MiB) Solar and supernova neutrinos in DUNE NuTel25, 02.10.2025 Solar neutrinos in DUNE Studies based on the FD-HD design Full background model + simulation and reconstruction chain Aggressive fiducialization (only central drift volumes) 100 kton-year - FD-HD - CC only Solar oscillation’s parameters sensitivity with 8B: CC channel only 4% prior on Φ(8B)(imitating ES constraints) θ13 prior from reactor experiments Even the aggressive fiducialization, the high background level limits the sensitivity to oscillation parameters Passive shielding under consideration for the FD-VD module ,→significant impact on the sensitivity! 13 / 14 D. Guffanti (University & INFN MiB) Solar and supernova neutrinos in DUNE NuTel25, 02.10.2025 Solar neutrinos in DUNE Studies based on the FD-HD design Full background model + simulation and reconstruction chain Aggressive fiducialization (only central drift volumes) 100 kton-year - FD-HD - CC only + shielding (projection) Solar oscillation’s parameters sensitivity with 8B: CC channel only 4% prior on Φ(8B)(imitating ES constraints) θ13 prior from reactor experiments Even the aggressive fiducialization, the high background level limits the sensitivity to oscillation parameters Passive shielding under consideration for the FD-VD module ,→significant impact on the sensitivity! 13 / 14 D. Guffanti (University & INFN MiB) Solar and supernova neutrinos in DUNE NuTel25, 02.10.2025 Conclusions and outlooks has a unique potential as a neutrino telescope for low-energy (electron) neutrinos Supernova neutrinos ∠Detector subsystems (TPC, PDS) provide efficient and reliable trigger for SNB in the galaxy ∠The good energy resolution and large target mass will make it possible to collect a high-statistics sample of νeCC events, an invaluable source of information in the core-collapse dynamics and neutrino properties ∠The ES channel can be used to point back to the SN direction with a few-degree resolution Solar neutrinos ∠Preliminary studies based on FDHD design show excellent prospects for hep neutrino discovery ∠The sensitivity to solar oscillation parameters is limited by the high radiological background level ∠Passive shielding under consideration Low-energy program is one of the key drivers of innovations proposed for the DUNE Phase II, which foresees the construction of 2 additional modules (FD3, FD4) DUNE Coll, JINST 19 (2024) 12, P12005 14 / 14 D. Guffanti (University & INFN MiB) Solar and supernova neutrinos in DUNE NuTel25, 02.10.2025