SUPRISE 2025: Supernova Probes of Invisible Sectors

11 Mar 2025, 09:00 → 14 Mar 2025, 19:00 Europe/Madrid

IFT UAM/CSIC

David Cerdeño , Marina Cermeño Gavilán (IFT UAM-CSIC) , SUPRISE25

Description

The high temperatures and densities reached in supernova cores constitute an ideal environment to produce and test exotic particles such as axions, axion-like particles, heavy neutral leptons, dark photons, gauge bosons, Majorons, sterile neutrinos and other light dark matter candidates. Besides, these objects are also crucial to test neutrino self-interactions, which cannot be probed otherwise in terrestrial experiments.

The potential signatures from this invisible sectors include an increase in the photon or neutrino flux; effects on the cosmic ray spectrum; the shortening of the neutrino burst duration due to an excessive cooling; the enhancement of the explosion energy released by Type II supernovae; modifications of the neutrino flavour composition; and changes in the standard explosion mechanism which must be carefully explored in self-consistent simulations.

This workshop, which will be held at the Institute of Theoretical Physics (IFT UAM/CSIC) in Madrid from the 11th to the 14th of March 2025, will explore this window to new physics from a wide perspective.

Conference poster

Tuesday, 11 March
- 14:15 → 14:40
  
  Registration
- 14:40 → 15:00
  
  Welcome
  
  Welcome_SUPRISE2025.pdf
- 15:00 → 16:10
  Supernova Physics (I)
  - 15:00
    
    A brief overview on Supernova equation of state and beyond 45m
    
    In this talk, I will provide a brief overview of the key aspects of supernova matter during the final stages of stellar evolution, when the collapsing stellar core undergoes gravitational collapse and triggers a subsequent explosion. I will discuss the current knowledge on composition, relevant thermodynamic properties, and the emission of multimessengers. Additionally, I will highlight open questions that remain unresolved, yet are crucial for achieving a comprehensive understanding of these astrophysical events. Finally I will discuss on exploring new avenues involving invisible sectors.
    
    Speaker: M. Ángeles Pérez-García (USAL)
    
    SUPRISE_m.angelesperezUSAL.pdf
  - 15:45
    
    On the time structure of electronic antineutrino emission from SN1987A 25m
    
    The neutrinos from the core collapse SN1987A are the first extrasolar neutrinos to be ever detected and have been widely studied to infer the thermodynamical and temporal features of a supernova; however their interpretation in terms of the astrophysical properties of the explosion has been giving rise to heated debates since ever. At date, models are still under construction and simulations do not always depict same things, thus the significance of the data at our disposal must be assessed as accurately as possible.
    By adopting a state-of-the-art parameterized model of electron antineutrino emission, we have made some steps forward in the analysis of the available data from core collapse SN1987A taking into account the times, energies and angles of arrival of all detected events in a reliable framework which includes a finite ramp in the initial stage of the neutrino emission.
    We determine the parameters of the accretion and cooling emissions and discuss their durations. The results compare well with theoretical expectations and overcome some tensions found in previous similar analyses. We estimate the delay times between the first antineutrino and the first event in the detectors. We test the agreement of the best-fit flux with the empirical temporal, energy and angular distributions, eventually finding a good compatibility with the observed data.
    
    Speaker: Vigilante di Risi (University of Naples Federico II)
    
    Presentation Vigilante.pdf
- 16:10 → 16:40
  
  COFFEE
- 16:40 → 17:30
  Supernova Physics (II)
  - 16:40
    
    Gravitational Waves from core-collapse Supernovae 25m
    
    The theory of core-collapse Supernovae (SNe) has been developed during the past five decades, and nowadays can be considered a field mature enough to be studied at the interface of gravitational, particle, nuclear and numerical physics. Recent realistic 3D SN simulations have revealed that successful explosions can be self-triggered only by accounting for the heating by neutrinos anisotropically emitted from the protoneutron star (PNS) and large neutrino-driven convective instabilities. Nevertheless, both of these phenomena are characterized by a non-vanishing quadrupole momentum, which could generate a large emission of gravitational waves (GW) in the range of frequencies $1-10^3$ Hz. In this talk, I will discuss the main features of the expected GW signal from both anisotropic neutrino emission and matter motions, showing that it might be in the reach of current and future GW detectors for a future Galactic SN event. In particular, I will argue that, in case of a direct detection, the GW signal could provide a lot of information regarding the different phase of the explosion, neutrino emission and PNS oscillation modes. In many cases, this analysis results to be complementary to what we can learn from a direct detection of the SN neutrino burst.
    
    Speaker: Alessandro Lella (University of Bari, INFN Bari)
    
    2025_SUPRISE2025_Madrid.pdf
  - 17:05
    
    Dark Photons can Prevent Core Collapse Supernova Explosions 25m
    
    During the accretion phase of a core-collapse supernova, dark-photon cooling can be largest in the gain layer below the stalled shock wave, in this way counter-act the usual shock rejuvenation by neutrino energy deposition, and thus prevent the explosion. The peculiar energy-loss profile derives from the resonant nature of dark-photon production. The largest effect obtains for the mass range 0.1–0.5 MeV, corresponding to the photon plasma mass in the gain region. For a coupling strength so small as to avoid this effect, the cooling of the core is too small to affect the neutrino signal.
    
    Speaker: Dr. Seokhoon Yun (IBS-CTPU)
    
    SUPRISE2025_S.Yun_11.03.25.pdf
- 18:00 → 20:00
  
  Reception
Wednesday, 12 March
- 10:00 → 11:10
  Supernova Neutrinos (I)
  - 10:00
    
    Neutrinos from dense environments and how they keep surprising us 45m
    
    Speaker: M. Cristina Volpe (APC Paris)
    
    SUPRISE-MCVOLPE-vf.pdf
  - 10:45
    
    Supernova neutrinos and Earth matter effects 25m
    
    In this talk, I will explore how the oscillation pattern of neutrinos emitted from a Supernova can be influenced by Earth matter effects and how these modifications can provide valuable insights into two significant areas of study. First, I will discuss how these effects could be used to probe the internal structure of the Earth, offering a unique approach to understanding its composition and properties. Second, I will explain how such observations could contribute to refining our knowledge of the solar neutrino mixing parameters, which are fundamental to our understanding of neutrino oscillations and their role in particle physics.
    
    Speaker: Rasmi Hajjar (IFIC (CSIC-UV))
    
    RHajjar_SN_SUPRISE.pdf
- 11:10 → 11:40
  
  COFFEE
- 11:40 → 12:30
  Supernova Neutrinos (II)
  
  Supernova Neutrinos
  - 11:40
    
    The RES-NOVA neutrino observatory 25m
    
    Recent development in the cryogenic detector’s technique opened the possibility to detect neutrinos via Coherent Elastic Neutrino-Nucleus Scattering (CEvNS) with cm3-scale detectors. RES-NOVA will leverage the high cross-section and low-radioactivity of Pb of archaeological origin to investigate the neutrino signal from the next galactic Supernova. Its unique features will allow for the first time the real-time, all-neutrino-flavor observation of this dramatic phenomenon with only a thousandth of the mass of conventional kton water-cherenkov detectors. In this contribution the key aspects of RES-NOVA that can investigate the invisible sector will be presented together with the novelties of this technology.
    
    Speaker: Nahuel Ferreiro Iachellini (University of Milano-Bicocca)
    
    SUP2025.pdf
  - 12:05
    
    Unveiling the DSNB via high energy neutrino fluxes 25m
    
    DSNB is a Standard Model prediction which should be soon confirmed. We will use data from high-energy neutrino fluxes to better asses the foregrounds affecting DSNB detection.
    
    Speaker: Pablo Blanco (IFT UAM/CSIC)
    
    SURPRISE2025-5-PBM.pdf
- 12:30 → 14:30
  
  LUNCH
- 14:30 → 15:40
  Supernova Neutrinos (III)
  - 14:30
    
    Supernova neutrinos as a laboratory for new particle physics 45m
    
    Speaker: Damiano Fiorillo (DESY Zeuthen)
    
    SlidesSUPRISE.pdf
  - 15:15
    
    The Diffuse Supernova Neutrino Background: Looking into the Neutrino Past 25m
    
    Neutrinos have been continuously emitted since the first supernova explosions, forming a persistent background known as the Diffuse Supernova Neutrino Background (DSNB), which is actively being searched for in various experiments. Notably, these neutrinos are the oldest within experimental reach, raising the question of what new physics, whether effects that influenced neutrinos in the early Universe or slow-evolving properties that manifest over time, could be probed following the detection of the DSNB. In this context, in this talk we explore two generic scenarios: neutrinos with masses that vary in the early Universe and the possibility that neutrinos exhibit a pseudo-Dirac nature.
    
    Speaker: Yuber F Perez-Gonzalez
- 15:40 → 16:10
  
  COFFEE
- 16:10 → 17:00
  Supernova Neutrinos (IV)
  - 16:10
    
    Probing neutrino non-radiative decay with supernova neutrinos 25m
    
    Neutrinos are produced in large quantities in core-collapse supernovae. However, to this date, the observation of supernovae through neutrino detection has been limited to a single event, SN1987A. Another possibility for studying supernova neutrinos is through the detection of the Diffuse Supernova Neutrino Background (DSNB), which represents the collective flux of neutrinos emitted by all past supernovae in the universe.
    Supernova neutrinos can be used to explore new physics. In particular, one can investigate the effect of neutrino decay, both in vacuum and in matter, through the detection of these neutrinos. In my talk, I will present bounds extracted from SN1987A data on the lifetime-to-mass ratio of neutrinos when considering neutrino decay in vacuum [1]. Furthermore, new limits using SN1987A data on the couplings of neutrinos with Majorons will be shown [2]. These interactions are responsible for neutrino decay inside the supernova. Finally, I will present the potential to extract information on the neutrino lifetime from future observations of the DSNB flux detection at the running Super-Kamiokande + Gd and the upcoming Hyper-Kamiokande, JUNO, and DUNE experiments [3]. Indeed, the DSNB flux has a unique sensitivity to neutrino non-radiative decay in vacuum for $\tau/m \in [10^9, 10^{11}]$ eV/s.
    
    [1] P. Iváñez-Ballesteros and M. C. Volpe, Phys. Lett. B, 847 (2023) 138252, arXiv:2307.03549
    [2] P. Iváñez-Ballesteros and M. C. Volpe, arXiv:2410.11517
    [3] P. Iváñez-Ballesteros and M. C. Volpe, Phys. Rev. D, 107 023017, arXiv:2209.12465
    
    Speaker: Pilar Iváñez Ballesteros (APC - Université Paris Cité)
    
    supernova_neutrinos_and_decay.pdf supernova_neutrinos_and_decay.ppsx
  - 16:35
    
    Probing Neutrino Decays in Core-Collapse Supernovae: Implications for Mass Ordering and Lifetime Constraints 25m
    
    The discovery of nonzero neutrino masses naturally leads to the consideration of heavier neutrinos decaying into lighter ones. We explore the impact of two-body neutrino decays on the neutronization burst of a core-collapse supernova—the intense burst of electron neutrino emission occurring within the first 25 ms after the core bounce. In the scenario considered, the electron neutrinos are primarily produced in the more massive state and they can decay into the lightest one or their antiparticles, along with an almost massless scalar. These decays can result in the emergence of a neutronization peak in the normal ordering or the suppression of the same peak in the inverted ordering, effectively allowing one mass ordering to mimic the other. By simulating supernova-neutrino signals at the Deep Underground Neutrino Experiment (DUNE) and the Hyper-Kamiokande (HK) experiment, we evaluate their sensitivity to the neutrino lifetime. Assuming the mass ordering is known, and depending on the underlying physics driving neutrino decay, we find that DUNE can probe lifetimes of τ/m≲10^{6} s/eV for a galactic supernova within approximately 10 kpc, while HK is sensitive to lifetimes one order of magnitude larger. These constraints significantly surpass existing limits from solar-system-bound oscillation experiments. Finally, we demonstrate that by combining data from DUNE and HK, it is generally possible to distinguish between decaying Dirac and decaying Majorana neutrinos.
    
    Speaker: Ivan Martinez Soler
    
    Talk_IMS.pdf
Thursday, 13 March
- 10:00 → 11:10
  Axions and ALPs in Supernovae (I)
  - 10:00
    
    Supernova Probes of Axions and Axion-Like Particles 45m
    
    Speaker: Maurizio Giannotti (Universidad de Zaragoza)
    
    MG_SURPRISE_EuCAPT-2025-updated.pdf
  - 10:45
    
    Axion emission from strange matter in core-collapse SNe 25m
    
    The duration of the neutrino burst from the supernova event SN 1987A is known to be sensitive to exotic sources of cooling, such as axions radiated from the dense and hot hadronic matter thought to constitute the inner core of the supernova. We perform the first quantitative study of the role of hadronic matter beyond the first generation—in particular strange matter. We do so by consistently including the full baryon and meson octets, and computing axion emissivity induced from baryon-meson to baryon-axion scatterings as well as from baryon decays. We consider a range of supernova thermodynamic conditions, as well as equation-of-state models with different strangeness content. We obtain the first bound on the axial axion-strange-strange coupling, as well as the strongest existing bound on the axion-down-strange counterpart. Our bound on the latter coupling can be as small as $O(10^{-2})$ for $f_a = 10^9$ GeV.
    
    Speaker: Mael Cavan (Lapth (Annecy - France))
    
    Cavan_03_13_SURPRISE25.pdf
- 11:10 → 11:40
  
  COFFEE
- 11:40 → 12:30
  Axions and ALPs in Supernovae (II)
  - 11:40
    
    Probing a diffuse flux of axion-like particles from galactic supernovae with neutrino water Cherenkov detectors 25m
    
    Axion-like particles (ALPs) with MeV masses can be produced with semi-relativistic velocities in core-collapse supernovae (SNe). In this talk, I will demonstrate that a diffuse galactic flux of ALPs arises from the accumulated fluxes of past SNe and that these ALPs can be detected in neutrino water Cherenkov detectors via $a$ $p$ $\rightarrow$ $p$ $\gamma$ interactions. Using Super-Kamiokande data, I will present new constraints on the ALP parameter space, excluding a region above cooling bounds for ALP masses in the range of 1−80 MeV and ALP-proton couplings between $8 \times 10^{−6}$ and $2 \times 10^{−4}$. Furthermore, I will show that the future Hyper-Kamiokande will be able to probe couplings as small as $2.5 \times 10^{−6}$, fully closing the allowed region between current Super-Kamiokande diffuse ALP flux limits and the SN 1987A cooling bounds.
    
    Speaker: Dr. Andres D. Perez (IFT-UAM/CSIC)
    
    AndresDanielPerezSuprise2025.pdf
  - 12:05
    
    Disentangling axion-like particle couplings to nucleons via a delayed signal in Super-Kamiokande from a future supernova 25m
    
    In this talk we show that, if axion-like particles (ALPs) from core-collapse supernovae (SNe) couple to protons, they would produce very characteristic signatures in neutrino water Cherenkov detectors through their scattering off free protons via $a \, p \rightarrow p \, \gamma$ interactions. Specifically, sub-MeV ALPs would generate photons with energies $\sim 30$ MeV, which could be observed by Super-Kamiokande and Hyper-Kamiokande as a delayed signal after a future detection of SN neutrinos. We apply this to a hypothetical neighbouring SN (at a maximum distance of 100~kpc) and demonstrate that the region in the parameter space with ALP masses between $10^{-4}$~MeV and $1$~MeV and ALP-proton couplings in the range $3 \times 10^{-6}-4 \times 10^{-5}$ could be probed. We argue that this new signature, combined with the one expected at $\sim 7$~MeV from oxygen de-excitation, would allow us to disentangle ALP-neutron and ALP-proton couplings.
    
    Speaker: David Alonso-González (IFT (UAM-CSIC))
    
    AlonsoGonzalez_SUPRISE2025.pdf
- 12:30 → 14:30
  
  LUNCH 2h
- 14:30 → 15:40
  Axions and ALPs in Supernovae (III)
  - 14:30
    
    High-energy astrophysics as a probe of SN ALPs 45m
    
    Speaker: Francesca Calore (LAPTH)
    
    SURPRISE_Madrid_FCalore.pdf
  - 15:15
    
    Direct searches for axions from supernovae in gamma-ray and neutrino detectors 25m
    
    Supernova explosions would emit large numbers of axions (and axionlike particles) if these hypothetical particles have masses of at most a few hundred MeV and couplings to nucleons, pions, electrons, muons, or photons. The emitted relativistic axions can lead to directly observable signals through decays or conversions to photons, which would also efficiently happen at the one-loop level. Thus, the potential photon signal does not require tree-level photon couplings. We show how the resulting gamma rays can be observed with gamma-ray detectors such as the Fermi-LAT even for extragalactic supernovae, e.g., the relatively recent SN 2023ixf. We discuss the possibility to infer detailed axion properties in case of a detection. Furthermore, the relativistic axions can be observed directly through rare scattering events in neutrino detectors such as Super-K, Hyper-K, or JUNO. We discuss predictions for event rates and which axion masses and couplings are potentially observable in those detectors.
    
    Speaker: Eike Ravensburg (SDU Odense)
    
    2503_SupriseConferenceMadrid_Ravensburg.pdf
- 15:40 → 16:10
  
  COFFEE
- 16:10 → 17:00
  Axions and ALPs in Supernovae (IV)
  - 16:10
    
    Constraining Light QCD Axions with Isolated Neutron Star Cooling 25m
    
    The existence of light QCD axions, whose mass depends on an additional free parameter, can lead to a new ground state of matter, where the sourced axion field reduces the nucleon effective mass. The presence of the axion field has structural consequences, in particular, it results in a thinner (or even prevents its existence) heat-blanketing envelope, significantly altering the cooling patterns of neutron stars. We exploit the anomalous cooling behavior to constrain previously uncharted regions of the axion parameter space by comparing model predictions with existing data from isolated neutron stars. Notably, this analysis does not require the light QCD axion to be the dark matter candidate.
    
    Speaker: Antonio Gómez Bañón (Universidad de Alicante)
    
    main.pdf
  - 16:35
    
    Constraining axion-like particles coupled to electrons with gamma rays from recent supernova events 25m
    
    Axion-like particles (ALPs) can be produced in core-collapse supernovae (SNe) through various mechanisms, such as photon coalescence, Primakoff, electron-positron fusion and electron-Bremsstrahlung, due to their potential coupling to electrons. In this talk, I will explore ALP production for masses between 10 keV and 100 MeV, which are expected to decay producing gamma-ray signals that could be detected at Earth. Constraints on ALP-electron couplings have been derived from the non-detection of gamma rays from SN 1987A. I will extend these analyses to modern observations, such as SN 2023ixf, to establish updated bounds on ALP-electron couplings.
    
    Speaker: Jorge García García (Universidad de Granada, Instituto de Astrofísica de Andalucía)
    
    SUPRISE_Madrid_JorgeGarcia.pdf
- 20:00 → 22:00
  
  Conference dinner
Friday, 14 March
- 10:00 → 11:10
  Other exotics in Supernovae (I)
  - 10:00
    
    DSNB-boosted dark matter 45m
    
    Speaker: Valentina de Romeri (IFIC)
    
    De_Romeri_SURPRISE.pdf
  - 10:45
    
    Analyzing Fermionic Dark Matter scenarios with the HESS J1731-347 Compact Object 25m
    
    In this presentation I will show how we can constrain Dark Matter (DM) scenarios with the supernova remnant HESS J1731-347. We assume the compact object to be an admixture of DM and Neutron Star, and presume the former to behave as a free Fermi gas. For the Neutron Star we use recently calculated regulator-independent equations of state for neutron stars obtained from first principles. Using the two-fluid formalism we analyze the impact of the DM contribution to the mass and radius of the compact object in terms of the DM particle mass and the DM fraction. This allows us to constrain different scenarios for fermonic DM behaving as a free Fermi gas.
    
    Speaker: Yaiza Cano Ruiperez (Universidad de Alcalá de Henares)
    
    Analyzing Fermionic Dark Matter scenarios with the HESS.pdf
- 11:10 → 11:40
  
  COFFEE 30m
- 11:40 → 12:30
  Other exotics in Supernovae (II)
  - 11:40
    
    Testing g-2 with neutrino cooling in White Dwarfs 25m
    
    In this talk, I will present the first $ab\ initio$ computation of the neutrino emissivities of White Dwarf stars due to plasmon decay in a model of gauged $U(1)_{L_\mu-L_\tau}$. I will present the relevant White Dwarf luminosities over the entire mass range of the new leptophilic gauge boson $A'$. In particular, taking into account the resonance effects, where the $A'$ mass is comparable to the White Dwarf plasma frequencies. I will demonstrate how current observations of the early-stage White Dwarf neutrino luminosity at the 30% accuracy level can test the allowed parameter space for explaining the $(g-2)_\mu$ anomaly in this model.
    
    Speaker: Patrick Foldenauer (IFT UAM-CSIC)
    
    foldenauer_suprise.pdf
  - 12:05
    
    Heating the dark matter halo with dark radiation from supernovae 25m
    
    Supernova explosions are extreme cosmic events that may impact not only ordinary matter but also dark matter (DM) halos. In this talk, I explore the possibility that a fraction of supernova energy is released as dark radiation, which could transform a cuspy DM halo into a cored one, potentially explaining observed cores in some dwarf galaxies. Alternatively, limits on DM core sizes provide constraints on the energy channeled into light particles beyond the Standard Model (SM). Based on evaluation of energetics, one finds that even a small fraction of the total SN energy is sufficient to change the overall shape of the DM halo and transform a cuspy halo into a cored one. We evaluate some well motivated benchmark models, e.g. the dark photon and dark Higgs, to demonstrate that significant supernova emissivity of dark radiation and large DM halo opacity are achievable in realistic particle physics model. Interestingly, couplings consistent with SN1987A observations can still have a measurable impact on dwarf galaxy halos.
    
    Speaker: Stefan Vogl (University of Freiburg)
    
    Vogl_SN_heating_2025.pdf
- 12:30 → 12:45
  
  Closing
  
  SUPRISE 2025 outro.pdf
- 12:45 → 14:30
  
  LUNCH 1h 45m

SUPRISE 2025: Supernova Probes of Invisible Sectors

IFT UAM/CSIC

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