2010/06/30 by Tina Lund, Andreas Marek, Cecilia Lunardini +4
Physics and Astronomy · #Accretion (finance) #Amplitude #Astronomy #Astrophysics #Astrophysics and Cosmic Phenomena #Gamma-ray bursts and supernovae #Instability #Neutrino #Neutrino Physics Research #Nuclear physics #Optics #Physics #Supernova #astro-ph.HE #hep-ex
paper · pdf · doi:10.1103/physrevd.82.063007
published as Phys.Rev.D82:063007,2010 · 14 pages, 11 figures. Final version accepted in PRD. Section on astrophysical relevance and several references added
arxiv created 2010/08/23 · openalex publication_date 2010/09/21 · arxiv updated 2014/11/21 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
In the delayed explosion scenario of core-collapse supernovae, the accretion phase shows pronounced convective overturns and a low-multipole hydrodynamic instability, the standing accretion shock instability. These effects imprint detectable fast time variations on the emerging neutrino flux. Among existing detectors, IceCube is best suited to this task, providing an event rate of \ensuremath∼1000 ms^\ensuremath-1 during the accretion phase for a fiducial SN distance of 10 kpc, comparable to what could be achieved with a megaton water Cherenkov detector. If the standing accretion shock instability activity lasts for several hundred ms, a Fourier component with an amplitude of 1% of the average signal clearly sticks out from the shot noise. We analyze in detail the output of axially symmetric hydrodynamical simulations that predict much larger amplitudes up to frequencies of a few hundred Hz. If these models are roughly representative for realistic SNe, fast time variations of the neutrino signal are easily detectable in IceCube or future megaton-class instruments. We also discuss the information that could be deduced from such a measurement about the physics in the SN core and the explosion mechanism of the SN.