BEGIN:VCALENDAR
VERSION:2.0
PRODID:-//CERN//INDICO//EN
BEGIN:VEVENT
SUMMARY:Constraining axion-like particles coupled to electrons with gamma 
 rays from recent supernova events
DTSTART;VALUE=DATE-TIME:20250313T153500Z
DTEND;VALUE=DATE-TIME:20250313T160000Z
DTSTAMP;VALUE=DATE-TIME:20260720T133928Z
UID:indico-contribution-26-309@indico.ift.uam-csic.es
DESCRIPTION:Speakers: Jorge García García (Universidad de Granada\, Inst
 ituto de Astrofísica de Andalucía)\nAxion-like particles (ALPs) can be p
 roduced in core-collapse supernovae (SNe) through various mechanisms\, suc
 h as photon coalescence\, Primakoff\, electron-positron fusion and electro
 n-Bremsstrahlung\, due to their potential coupling to electrons. In this t
 alk\, 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 de
 tected at Earth. Constraints on ALP-electron couplings have been derived f
 rom the non-detection of gamma rays from SN 1987A. I will extend these ana
 lyses to modern observations\, such as SN 2023ixf\, to establish updated b
 ounds on ALP-electron couplings.\n\nhttps://indico.ift.uam-csic.es/event/2
 6/contributions/309/
LOCATION:IFT UAM/CSIC
URL:https://indico.ift.uam-csic.es/event/26/contributions/309/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Direct searches for axions from supernovae in gamma-ray and neutri
 no detectors
DTSTART;VALUE=DATE-TIME:20250313T141500Z
DTEND;VALUE=DATE-TIME:20250313T144000Z
DTSTAMP;VALUE=DATE-TIME:20260720T133928Z
UID:indico-contribution-26-311@indico.ift.uam-csic.es
DESCRIPTION:Speakers: Eike Ravensburg (SDU Odense)\nSupernova explosions w
 ould emit large numbers of axions (and axionlike particles) if these hypot
 hetical particles have masses of at most a few hundred MeV and couplings t
 o nucleons\, pions\, electrons\, muons\, or photons. The emitted relativis
 tic axions can lead to directly observable signals through decays or conve
 rsions to photons\, which would also efficiently happen at the one-loop le
 vel. Thus\, the potential photon signal does not require tree-level photon
  couplings. We show how the resulting gamma rays can be observed with gamm
 a-ray detectors such as the Fermi-LAT even for extragalactic supernovae\, 
 e.g.\, the relatively recent SN 2023ixf. We discuss the possibility to inf
 er detailed axion properties in case of a detection. Furthermore\, the rel
 ativistic axions can be observed directly through rare scattering events i
 n neutrino detectors such as Super-K\, Hyper-K\, or JUNO. We discuss predi
 ctions for event rates and which axion masses and couplings are potentiall
 y observable in those detectors.\n\nhttps://indico.ift.uam-csic.es/event/2
 6/contributions/311/
LOCATION:IFT UAM/CSIC
URL:https://indico.ift.uam-csic.es/event/26/contributions/311/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Constraining Light QCD Axions with Isolated Neutron Star Cooling
DTSTART;VALUE=DATE-TIME:20250313T151000Z
DTEND;VALUE=DATE-TIME:20250313T153500Z
DTSTAMP;VALUE=DATE-TIME:20260720T133928Z
UID:indico-contribution-26-326@indico.ift.uam-csic.es
DESCRIPTION:Speakers: Antonio Gómez Bañón (Universidad de Alicante)\nTh
 e 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 thinne
 r (or even prevents its existence) heat-blanketing envelope\, significantl
 y altering the cooling patterns of neutron stars. We exploit the anomalous
  cooling behavior to constrain previously uncharted regions of the axion p
 arameter space by comparing model predictions with existing data from isol
 ated neutron stars. Notably\, this analysis does not require the light QCD
  axion to be the dark matter candidate.\n\nhttps://indico.ift.uam-csic.es/
 event/26/contributions/326/
LOCATION:IFT UAM/CSIC
URL:https://indico.ift.uam-csic.es/event/26/contributions/326/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Dark Photons can Prevent Core Collapse Supernova Explosions
DTSTART;VALUE=DATE-TIME:20250311T160500Z
DTEND;VALUE=DATE-TIME:20250311T163000Z
DTSTAMP;VALUE=DATE-TIME:20260720T133928Z
UID:indico-contribution-26-303@indico.ift.uam-csic.es
DESCRIPTION:Speakers: Seokhoon Yun (IBS-CTPU)\nDuring the accretion phase 
 of a core-collapse supernova\, dark-photon cooling can be largest in the g
 ain layer below the stalled shock wave\, in this way counter-act the usual
  shock rejuvenation by neutrino energy deposition\, and thus prevent the e
 xplosion. The peculiar energy-loss profile derives from the resonant natur
 e 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 regio
 n. For a coupling strength so small as to avoid this effect\, the cooling 
 of the core is too small to affect the neutrino signal.\n\nhttps://indico.
 ift.uam-csic.es/event/26/contributions/303/
LOCATION:IFT UAM/CSIC
URL:https://indico.ift.uam-csic.es/event/26/contributions/303/
END:VEVENT
BEGIN:VEVENT
SUMMARY:A brief overview on Supernova equation of state and beyond
DTSTART;VALUE=DATE-TIME:20250311T140000Z
DTEND;VALUE=DATE-TIME:20250311T144500Z
DTSTAMP;VALUE=DATE-TIME:20260720T133928Z
UID:indico-contribution-26-314@indico.ift.uam-csic.es
DESCRIPTION:Speakers: M. Ángeles Pérez-García (USAL)\nIn this talk\, I 
 will provide a brief overview of the key aspects of supernova matter durin
 g the final stages of stellar evolution\, when the collapsing stellar core
  undergoes gravitational collapse and triggers a subsequent explosion. I w
 ill discuss the current knowledge on composition\, relevant thermodynamic 
 properties\, and the emission of multimessengers. Additionally\, I will hi
 ghlight open questions that remain unresolved\, yet are crucial for achiev
 ing a comprehensive understanding of these astrophysical events. Finally I
  will discuss on exploring new avenues involving invisible sectors.\n\nhtt
 ps://indico.ift.uam-csic.es/event/26/contributions/314/
LOCATION:IFT UAM/CSIC
URL:https://indico.ift.uam-csic.es/event/26/contributions/314/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Heating the dark matter halo with dark radiation from supernovae
DTSTART;VALUE=DATE-TIME:20250314T110500Z
DTEND;VALUE=DATE-TIME:20250314T113000Z
DTSTAMP;VALUE=DATE-TIME:20260720T133928Z
UID:indico-contribution-26-305@indico.ift.uam-csic.es
DESCRIPTION:Speakers: Stefan Vogl (University of Freiburg)\nSupernova expl
 osions 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 s
 izes provide constraints on the energy channeled into light particles beyo
 nd 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 o
 ne. We evaluate some well motivated benchmark models\, e.g. the dark photo
 n and dark Higgs\, to demonstrate that significant supernova emissivity of
  dark radiation and large DM halo opacity are achievable in realistic part
 icle physics model. Interestingly\, couplings consistent with SN1987A obse
 rvations can still have a measurable impact on dwarf galaxy halos.\n\nhttp
 s://indico.ift.uam-csic.es/event/26/contributions/305/
LOCATION:IFT UAM/CSIC
URL:https://indico.ift.uam-csic.es/event/26/contributions/305/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Testing g-2 with neutrino cooling in White Dwarfs
DTSTART;VALUE=DATE-TIME:20250314T104000Z
DTEND;VALUE=DATE-TIME:20250314T110500Z
DTSTAMP;VALUE=DATE-TIME:20260720T133928Z
UID:indico-contribution-26-327@indico.ift.uam-csic.es
DESCRIPTION:Speakers: Patrick Foldenauer (IFT UAM-CSIC)\nIn this talk\, I 
 will present the first $ab\\ initio$ computation of the neutrino emissivit
 ies 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 ove
 r the entire mass range of the new leptophilic gauge boson  $A'$. In parti
 cular\, 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 explainin
 g the $(g-2)_\\mu$ anomaly in this model.\n\nhttps://indico.ift.uam-csic.e
 s/event/26/contributions/327/
LOCATION:IFT UAM/CSIC
URL:https://indico.ift.uam-csic.es/event/26/contributions/327/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Analyzing Fermionic Dark Matter scenarios with the HESS J1731-347 
 Compact Object
DTSTART;VALUE=DATE-TIME:20250314T094500Z
DTEND;VALUE=DATE-TIME:20250314T101000Z
DTSTAMP;VALUE=DATE-TIME:20260720T133928Z
UID:indico-contribution-26-313@indico.ift.uam-csic.es
DESCRIPTION:Speakers: Yaiza Cano Ruiperez  (Universidad de Alcalá de Hena
 res)\nIn this presentation I will show how we can constrain Dark Matter (D
 M) scenarios with the supernova remnant HESS J1731-347. We assume the comp
 act object to be an admixture of DM and Neutron Star\, and presume the for
 mer to behave as a free Fermi gas. For the Neutron Star we use recently ca
 lculated regulator-independent equations of state for neutron stars obtain
 ed from first principles. Using the two-fluid formalism we analyze the imp
 act 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 cons
 train different scenarios for fermonic DM behaving as a free Fermi gas.\n\
 nhttps://indico.ift.uam-csic.es/event/26/contributions/313/
LOCATION:IFT UAM/CSIC
URL:https://indico.ift.uam-csic.es/event/26/contributions/313/
END:VEVENT
BEGIN:VEVENT
SUMMARY:DSNB-boosted dark matter
DTSTART;VALUE=DATE-TIME:20250314T090000Z
DTEND;VALUE=DATE-TIME:20250314T094500Z
DTSTAMP;VALUE=DATE-TIME:20260720T133928Z
UID:indico-contribution-26-319@indico.ift.uam-csic.es
DESCRIPTION:Speakers: Valentina de Romeri (IFIC)\nhttps://indico.ift.uam-c
 sic.es/event/26/contributions/319/
LOCATION:IFT UAM/CSIC
URL:https://indico.ift.uam-csic.es/event/26/contributions/319/
END:VEVENT
BEGIN:VEVENT
SUMMARY:High-energy astrophysics as a probe of SN ALPs
DTSTART;VALUE=DATE-TIME:20250313T133000Z
DTEND;VALUE=DATE-TIME:20250313T141500Z
DTSTAMP;VALUE=DATE-TIME:20260720T133928Z
UID:indico-contribution-26-318@indico.ift.uam-csic.es
DESCRIPTION:Speakers: Francesca Calore (LAPTH)\nhttps://indico.ift.uam-csi
 c.es/event/26/contributions/318/
LOCATION:IFT UAM/CSIC
URL:https://indico.ift.uam-csic.es/event/26/contributions/318/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Disentangling axion-like particle couplings to nucleons via a dela
 yed signal in Super-Kamiokande from a future supernova
DTSTART;VALUE=DATE-TIME:20250313T110500Z
DTEND;VALUE=DATE-TIME:20250313T113000Z
DTSTAMP;VALUE=DATE-TIME:20260720T133928Z
UID:indico-contribution-26-299@indico.ift.uam-csic.es
DESCRIPTION:Speakers: David Alonso-González (IFT (UAM-CSIC))\nIn this tal
 k we show that\, if axion-like particles (ALPs) from core-collapse superno
 vae (SNe) couple to protons\, they would produce very characteristic signa
 tures in neutrino water Cherenkov detectors through their scattering off f
 ree protons via $a \\\, p \\rightarrow p \\\, \\gamma$ interactions. Speci
 fically\, sub-MeV ALPs would generate photons with energies $\\sim 30$ MeV
 \, which could be observed by Super-Kamiokande and Hyper-Kamiokande as a d
 elayed signal after a future detection of SN neutrinos. We apply this to a
  hypothetical neighbouring SN (at a maximum distance of 100~kpc) and demon
 strate 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-excitatio
 n\, would allow us to disentangle ALP-neutron and ALP-proton couplings.\n\
 nhttps://indico.ift.uam-csic.es/event/26/contributions/299/
LOCATION:IFT UAM/CSIC
URL:https://indico.ift.uam-csic.es/event/26/contributions/299/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Probing a diffuse flux of axion-like particles from galactic super
 novae with neutrino water Cherenkov detectors
DTSTART;VALUE=DATE-TIME:20250313T104000Z
DTEND;VALUE=DATE-TIME:20250313T110500Z
DTSTAMP;VALUE=DATE-TIME:20260720T133928Z
UID:indico-contribution-26-329@indico.ift.uam-csic.es
DESCRIPTION:Speakers: Andres D. Perez (IFT-UAM/CSIC)\nAxion-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 detec
 tors via $a$ $p$ $\\rightarrow$ $p$ $\\gamma$ interactions. Using Super-Ka
 miokande 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-Kamiokan
 de will be able to probe couplings as small as $2.5 \\times 10^{−6}$\, f
 ully closing the allowed region between current Super-Kamiokande diffuse A
 LP flux limits and the SN 1987A cooling bounds.\n\nhttps://indico.ift.uam-
 csic.es/event/26/contributions/329/
LOCATION:IFT UAM/CSIC
URL:https://indico.ift.uam-csic.es/event/26/contributions/329/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Axion emission from strange matter in core-collapse SNe
DTSTART;VALUE=DATE-TIME:20250313T094500Z
DTEND;VALUE=DATE-TIME:20250313T101000Z
DTSTAMP;VALUE=DATE-TIME:20260720T133928Z
UID:indico-contribution-26-301@indico.ift.uam-csic.es
DESCRIPTION:Speakers: Mael Cavan (Lapth (Annecy - France))\nThe duration o
 f the neutrino burst from the supernova event SN 1987A is known to be sens
 itive to exotic sources of cooling\, such as axions radiated from the dens
 e and hot hadronic matter thought to constitute the inner core of the supe
 rnova. We perform the first quantitative study of the role of hadronic mat
 ter beyond the first generation—in particular strange matter. We do so b
 y 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 strangene
 ss content. We obtain the first bound on the axial axion-strange-strange c
 oupling\, as well as the strongest existing bound on the axion-down-strang
 e counterpart. Our bound on the latter coupling can be as small as $O(10^{
 -2})$ for $f_a = 10^9$ GeV.\n\nhttps://indico.ift.uam-csic.es/event/26/con
 tributions/301/
LOCATION:IFT UAM/CSIC
URL:https://indico.ift.uam-csic.es/event/26/contributions/301/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Supernova Probes of Axions and Axion-Like Particles
DTSTART;VALUE=DATE-TIME:20250313T090000Z
DTEND;VALUE=DATE-TIME:20250313T094500Z
DTSTAMP;VALUE=DATE-TIME:20260720T133928Z
UID:indico-contribution-26-317@indico.ift.uam-csic.es
DESCRIPTION:Speakers: Maurizio Giannotti (Universidad de Zaragoza)\nhttps:
 //indico.ift.uam-csic.es/event/26/contributions/317/
LOCATION:IFT UAM/CSIC
URL:https://indico.ift.uam-csic.es/event/26/contributions/317/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Probing Neutrino Decays in Core-Collapse Supernovae: Implications 
 for Mass Ordering and Lifetime Constraints
DTSTART;VALUE=DATE-TIME:20250312T153500Z
DTEND;VALUE=DATE-TIME:20250312T160000Z
DTSTAMP;VALUE=DATE-TIME:20260720T133928Z
UID:indico-contribution-26-310@indico.ift.uam-csic.es
DESCRIPTION:Speakers: Ivan Martinez Soler ()\nThe discovery of nonzero neu
 trino masses naturally leads to the consideration of heavier neutrinos dec
 aying into lighter ones. We explore the impact of two-body neutrino decays
  on the neutronization burst of a core-collapse supernova—the intense bu
 rst of electron neutrino emission occurring within the first 25 ms after t
 he core bounce. In the scenario considered\, the electron neutrinos are pr
 imarily produced in the more massive state and they can decay into the lig
 htest one or their antiparticles\, along with an almost massless scalar. T
 hese decays can result in the emergence of a neutronization peak in the no
 rmal ordering or the suppression of the same peak in the inverted ordering
 \, effectively allowing one mass ordering to mimic the other. By simulatin
 g supernova-neutrino signals at the Deep Underground Neutrino Experiment (
 DUNE) and the Hyper-Kamiokande (HK) experiment\, we evaluate their sensiti
 vity to the neutrino lifetime. Assuming the mass ordering is known\, and d
 epending on the underlying physics driving neutrino decay\, we find that D
 UNE can probe lifetimes of τ/m≲10^{6} s/eV for a galactic supernova wit
 hin 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 dis
 tinguish between decaying Dirac and decaying Majorana neutrinos.\n\nhttps:
 //indico.ift.uam-csic.es/event/26/contributions/310/
LOCATION:IFT UAM/CSIC
URL:https://indico.ift.uam-csic.es/event/26/contributions/310/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Probing neutrino non-radiative decay with supernova neutrinos
DTSTART;VALUE=DATE-TIME:20250312T151000Z
DTEND;VALUE=DATE-TIME:20250312T153500Z
DTSTAMP;VALUE=DATE-TIME:20260720T133928Z
UID:indico-contribution-26-308@indico.ift.uam-csic.es
DESCRIPTION:Speakers: Pilar Iváñez Ballesteros (APC - Université Paris 
 Cité)\nNeutrinos are produced in large quantities in core-collapse supern
 ovae. However\, to this date\, the observation of supernovae through neutr
 ino detection has been limited to a single event\, SN1987A. Another possib
 ility for studying supernova neutrinos is through the detection of the Dif
 fuse Supernova Neutrino Background (DSNB)\, which represents the collectiv
 e flux of neutrinos emitted by all past supernovae in the universe.\nSuper
 nova 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 bou
 nds extracted from SN1987A data on the lifetime-to-mass ratio of neutrinos
  when considering neutrino decay in vacuum [1]. Furthermore\, new limits u
 sing SN1987A data on the couplings of neutrinos with Majorons will be show
 n [2]. These interactions are responsible for neutrino decay inside the su
 pernova. 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\, J
 UNO\, and DUNE experiments [3]. Indeed\, the DSNB flux has a unique sensit
 ivity to neutrino non-radiative decay in vacuum for $\\tau/m \\in [10^9\, 
 10^{11}]$ eV/s.\n\n[1] P. Iváñez-Ballesteros and M. C. Volpe\, Phys. Let
 t. B\, 847 (2023) 138252\, arXiv:2307.03549\n[2] P. Iváñez-Ballesteros a
 nd M. C. Volpe\, arXiv:2410.11517 \n[3] P. Iváñez-Ballesteros and M. C. 
 Volpe\, Phys. Rev. D\, 107 023017\, arXiv:2209.12465\n\nhttps://indico.ift
 .uam-csic.es/event/26/contributions/308/
LOCATION:IFT UAM/CSIC
URL:https://indico.ift.uam-csic.es/event/26/contributions/308/
END:VEVENT
BEGIN:VEVENT
SUMMARY:The Diffuse Supernova Neutrino Background: Looking into the Neutri
 no Past
DTSTART;VALUE=DATE-TIME:20250312T141500Z
DTEND;VALUE=DATE-TIME:20250312T144000Z
DTSTAMP;VALUE=DATE-TIME:20260720T133928Z
UID:indico-contribution-26-306@indico.ift.uam-csic.es
DESCRIPTION:Speakers: Yuber F Perez-Gonzalez ()\nNeutrinos have been conti
 nuously emitted since the first supernova explosions\, forming a persisten
 t background known as the Diffuse Supernova Neutrino Background (DSNB)\, w
 hich is actively being searched for in various experiments. Notably\, thes
 e neutrinos are the oldest within experimental reach\, raising the questio
 n of what new physics\, whether effects that influenced neutrinos in the e
 arly Universe or slow-evolving properties that manifest over time\, could 
 be probed following the detection of the DSNB. In this context\, in this t
 alk we explore two generic scenarios: neutrinos with masses that vary in t
 he early Universe and the possibility that neutrinos exhibit a pseudo-Dira
 c nature.\n\nhttps://indico.ift.uam-csic.es/event/26/contributions/306/
LOCATION:IFT UAM/CSIC
URL:https://indico.ift.uam-csic.es/event/26/contributions/306/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Supernova neutrinos as a laboratory for new particle physics
DTSTART;VALUE=DATE-TIME:20250312T133000Z
DTEND;VALUE=DATE-TIME:20250312T141500Z
DTSTAMP;VALUE=DATE-TIME:20260720T133928Z
UID:indico-contribution-26-316@indico.ift.uam-csic.es
DESCRIPTION:Speakers: Damiano Fiorillo (DESY Zeuthen)\nhttps://indico.ift.
 uam-csic.es/event/26/contributions/316/
LOCATION:IFT UAM/CSIC
URL:https://indico.ift.uam-csic.es/event/26/contributions/316/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Unveiling the DSNB via high energy neutrino fluxes
DTSTART;VALUE=DATE-TIME:20250312T110500Z
DTEND;VALUE=DATE-TIME:20250312T113000Z
DTSTAMP;VALUE=DATE-TIME:20260720T133928Z
UID:indico-contribution-26-312@indico.ift.uam-csic.es
DESCRIPTION:Speakers: Pablo Blanco (IFT UAM/CSIC)\nDSNB is a Standard Mode
 l prediction which  should be soon confirmed. We will use data from high-e
 nergy neutrino fluxes to better asses the foregrounds affecting DSNB detec
 tion.\n\nhttps://indico.ift.uam-csic.es/event/26/contributions/312/
LOCATION:IFT UAM/CSIC
URL:https://indico.ift.uam-csic.es/event/26/contributions/312/
END:VEVENT
BEGIN:VEVENT
SUMMARY:The RES-NOVA neutrino observatory
DTSTART;VALUE=DATE-TIME:20250312T104000Z
DTEND;VALUE=DATE-TIME:20250312T110500Z
DTSTAMP;VALUE=DATE-TIME:20260720T133928Z
UID:indico-contribution-26-307@indico.ift.uam-csic.es
DESCRIPTION:Speakers: Nahuel Ferreiro Iachellini (University of Milano-Bic
 occa)\nRecent development in the cryogenic detector’s technique opened t
 he possibility to detect neutrinos via Coherent Elastic Neutrino-Nucleus S
 cattering (CEvNS) with cm3-scale detectors. RES-NOVA will leverage the hig
 h cross-section and low-radioactivity of Pb of archaeological origin to in
 vestigate the neutrino signal from the next galactic Supernova. Its unique
  features will allow for the first time the real-time\, all-neutrino-flavo
 r observation of this dramatic phenomenon with only a thousandth of the ma
 ss of conventional kton water-cherenkov detectors. In this contribution th
 e key aspects of RES-NOVA that can investigate the invisible sector will b
 e presented together with the novelties of this technology.\n\nhttps://ind
 ico.ift.uam-csic.es/event/26/contributions/307/
LOCATION:IFT UAM/CSIC
URL:https://indico.ift.uam-csic.es/event/26/contributions/307/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Neutrinos from dense environments and how they keep surprising us
DTSTART;VALUE=DATE-TIME:20250312T090000Z
DTEND;VALUE=DATE-TIME:20250312T094500Z
DTSTAMP;VALUE=DATE-TIME:20260720T133928Z
UID:indico-contribution-26-315@indico.ift.uam-csic.es
DESCRIPTION:Speakers: M. Cristina Volpe (APC Paris)\nhttps://indico.ift.ua
 m-csic.es/event/26/contributions/315/
LOCATION:IFT UAM/CSIC
URL:https://indico.ift.uam-csic.es/event/26/contributions/315/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Supernova neutrinos and Earth matter effects
DTSTART;VALUE=DATE-TIME:20250312T094500Z
DTEND;VALUE=DATE-TIME:20250312T101000Z
DTSTAMP;VALUE=DATE-TIME:20260720T133928Z
UID:indico-contribution-26-300@indico.ift.uam-csic.es
DESCRIPTION:Speakers: Rasmi Hajjar (IFIC (CSIC-UV))\nIn 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 structu
 re of the Earth\, offering a unique approach to understanding its composit
 ion and properties. Second\, I will explain how such observations could co
 ntribute 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.\n\nhttps://indico.ift.uam-csic.es/event/2
 6/contributions/300/
LOCATION:IFT UAM/CSIC
URL:https://indico.ift.uam-csic.es/event/26/contributions/300/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Gravitational Waves from core-collapse Supernovae
DTSTART;VALUE=DATE-TIME:20250311T154000Z
DTEND;VALUE=DATE-TIME:20250311T160500Z
DTSTAMP;VALUE=DATE-TIME:20260720T133928Z
UID:indico-contribution-26-302@indico.ift.uam-csic.es
DESCRIPTION:Speakers: Alessandro Lella (University of Bari\, INFN Bari)\nT
 he theory of core-collapse Supernovae (SNe) has been developed during the 
 past five decades\, and nowadays can be considered a field mature enough t
 o be studied at the interface of gravitational\, particle\, nuclear and nu
 merical physics. Recent realistic 3D SN simulations have revealed that suc
 cessful explosions can be self-triggered only by accounting for the heatin
 g by neutrinos anisotropically emitted from the protoneutron star (PNS) an
 d large neutrino-driven convective instabilities. Nevertheless\, both of t
 hese phenomena are characterized by a non-vanishing quadrupole momentum\, 
 which could generate a large emission of gravitational waves (GW) in the r
 ange of frequencies $1-10^3$ Hz. In this talk\, I will discuss the main fe
 atures of the expected GW signal from both anisotropic neutrino emission a
 nd matter motions\, showing that it might be in the reach of current and f
 uture 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\, neutr
 ino emission and PNS oscillation modes. In many cases\, this analysis resu
 lts to be complementary to what we can learn from a direct detection of th
 e SN neutrino burst.\n\nhttps://indico.ift.uam-csic.es/event/26/contributi
 ons/302/
LOCATION:IFT UAM/CSIC
URL:https://indico.ift.uam-csic.es/event/26/contributions/302/
END:VEVENT
BEGIN:VEVENT
SUMMARY:On the time structure of electronic antineutrino emission from SN1
 987A
DTSTART;VALUE=DATE-TIME:20250311T144500Z
DTEND;VALUE=DATE-TIME:20250311T151000Z
DTSTAMP;VALUE=DATE-TIME:20260720T133928Z
UID:indico-contribution-26-328@indico.ift.uam-csic.es
DESCRIPTION:Speakers: Vigilante di Risi (University of Naples Federico II)
 \nThe neutrinos from the core collapse SN1987A are the first extrasolar ne
 utrinos to be ever detected and have been widely studied to infer the ther
 modynamical and temporal features of a supernova\; however their interpret
 ation in terms of the astrophysical properties of the explosion has been g
 iving rise to heated debates since ever.  At date\,  models are still unde
 r construction and simulations do not always depict same things\, thus the
  significance of the data at our disposal must be assessed as accurately a
 s possible.\nBy adopting a state-of-the-art parameterized model of electro
 n 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 reliabl
 e framework which includes a finite ramp in the initial stage of the neutr
 ino emission.\n We determine the parameters of the accretion and cooling e
 missions and discuss their durations. The results compare well with theore
 tical expectations and overcome some tensions found in previous similar an
 alyses. 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\, eventuall
 y finding a good compatibility with the observed data.\n\nhttps://indico.i
 ft.uam-csic.es/event/26/contributions/328/
LOCATION:IFT UAM/CSIC
URL:https://indico.ift.uam-csic.es/event/26/contributions/328/
END:VEVENT
END:VCALENDAR