Workshop on core-collapse supernova neutrino detection

Salle du Conseil (Institut de Physique Nucléaire d'Orsay)

Salle du Conseil

Institut de Physique Nucléaire d'Orsay

The location of the conference venue is indicated on the maps below.
  • Wednesday, July 4
    • 9:30 AM 10:00 AM
      Welcome coffee 30m
    • 10:00 AM 10:20 AM
      Introduction 20m
      Speaker: Alexis Coleiro (APC / Université Paris Diderot)
    • 10:20 AM 11:00 AM
      SuperNova Early Warning System (SNEWS) 40m

      The Supernova Early Warning System (SNEWS) is a cooperative effort between the world's neutrino detection experiments to spread the news that a star in our galaxy has just experienced a core-collapse event and is about to become a Type II Supernova. This project exploits the ~hours time difference between neutrinos promptly escaping the nascent supernova and photons which originate when the shock wave breaks through the stellar photosphere, to give the world a chance to get ready to observe such an exciting event at the earliest possible time. A coincidence trigger between experiments is used to eliminate potential local false alarms, allowing a rapid, automated alert.

      Speaker: Alec Habig (University of Minnesota Duluth)
    • 11:00 AM 11:40 AM
      CCSN neutrino detection with Super-Kamiokande and Hyper-Kamiokande 40m
      Speaker: Yusuke Koshio
    • 11:40 AM 12:20 PM
      CCSN neutrino detection with IceCube 40m
      Speaker: Segev BenZvi
    • 2:00 PM 2:40 PM
      CCSN neutrino detection with Borexino 40m
      Speaker: Zara Bagdasarian
    • 2:40 PM 3:20 PM
      Towards detecting extra-galactic supernovae in the antarctic ice 40m

      While the detection of a neutrino burst from a galactic supernova would provide a plethora of information on the stellar collapse as well as the neutrino properties, the low rate of 1-2 CCSNe per century make this a tedious endeavor. Instead, a detector with an effective mass of 10 Mton at 10MeV would detect extra-galactic supernovae at a rate of 1-2 per year - albeit with a much lower number of neutrino interactions per burst. I will present a conceptual design for the Megaton Ice Cherenkov Array (MICA) — a dedicated setup in the antarctic to ice optimized to detect extra-galactic neutrino bursts. Alongside with first results highlighting the physics potential I will show first steps towards realization of the required sensor technology.

      Speaker: Sebastian Böser (Universität Bonn)
    • 3:20 PM 4:00 PM
      CCSN neutrino detection with DUNE 40m

      The Deep Underground Neutrino Experiment (DUNE), a 40-kt liquid argon time projection chamber detector located deep underground at the 4850L of the Sanford Underground Research Facility (SURF) in South Dakota, will record the burst of neutrinos from the core collapse of a massive star in the Milky Way neighborhood.DUNE's liquid argon has unique sensitivity to the electron neutrino component of the burst. This talk will present the expected capabilities of DUNE for measurements of neutrinos in the few-tens-of-MeV range relevant for supernova detection, and the corresponding sensitivities to neutrino physics and supernova astrophysics. Recent progress and some outstanding issues will be highlighted.

      Speaker: Inés Gil-Botella
    • 4:00 PM 4:30 PM
      Coffee break 30m
    • 4:30 PM 5:00 PM
      Prospects for CCSN neutrino detection with KM3NeT 30m
      Speaker: Marta Colomer-Molla
  • Thursday, July 5
    • 9:30 AM 10:00 AM
      Welcome coffee 30m
    • 10:00 AM 10:30 AM
      Prospects for CCSN alert triggering with KM3NeT 30m
      Speaker: Massimiliano Lincetto (Aix Marseille Univ, CNRS/IN2P3, CPPM, Marseille, France)
    • 10:30 AM 11:10 AM
      Triangulation method for locating a core-collapse supernova 40m

      Modern neutrino facilities will be able to detect a large number of neutrinos from the next Galactic supernova.
      In this talk we will present the update of the triangulation method for locating a core-collapse supernova by employing the neutrino arrival time differences at various detectors. We will discuss detailed numerical fits which are necessary in order to determine the uncertainties of these time differences for the cases when the core collapses into a neutron star or a black hole. A global picture with the inclusion of all relevant present and near future neutrino detectors is presented.

      Speaker: Vedran Brdar
    • 11:10 AM 11:50 AM
      Neutrinos from supernovae and in binary neutron star mergers 40m

      We discuss the recent progress in our understanding of flavor evolution in dense astrophysical environments, in particular core-collapse supernovae and binary neutron star mergers. We highlight what we might learn from a galactic supernova, the connection to r-process nucleosynthesis and to the recent kilonova observation.

      Speaker: Cristina VOLPE (APC)
    • 2:00 PM 2:40 PM
      Physics of supernova neutrino oscillations 40m

      In this talk the status of both known and unknown neutrino oscillation parameters will be reviewed, with particular focus on the mass ordering and the its discrimination with present experiments and future projects. In this context our current understanding of supernova neutrino flavor conversions is discussed, from ordinary flavor oscillations during the shock-wave propagation to collective flavor transitions induced by self-interactions.

      Speaker: Antonio Marrone (Dipartimento di Fisica, Univ. di Bari & INFN Bari)
    • 2:40 PM 3:20 PM
      Collective Neutrino Oscillations in Dense Neutrino Media 40m

      Neutrino evolution in dense neutrino media is a very nonlinear and rich phenomenon. Such a dense neutrino medium could be found in very extreme astrophysical sites such as core collapse supernovae and neutron star mergers. Studying collective neutrino oscillations in the aforementioned settings is very important since neutrinos could play a key role in their dynamics and nucleosynthesis. In this talk, I will discuss our current understanding of this topic which has tremendously changed in the past few years.

      Speaker: Sajad Abbar
    • 3:20 PM 4:00 PM
      Discussions 40m
    • 4:00 PM 4:30 PM
      Coffee break 30m
    • 4:30 PM 5:30 PM
      Discussions 1h