The neutrino signal from protoneutron star accretion and black hole formation

By Tobias Fischer, S. Whitehouse, A. Mezzacappa, Friedrich-Karl Thielemann, M. Liebendorfer. 2008

135 citations recorded by the source corpus.

We discuss the formation of stellar mass black holes via protoneutron star (PNS) collapse. In the absence of an earlier explosion, the PNS collapses to a black hole due to the continued mass accretion onto the PNS. We present an analysis of the emitted neutrino spectra of all three flavors during the PNS contraction. Special attention is given to the physical conditions which depend on the input physics, e.g. the equation of state (EoS) and the progenitor model. The PNSs are modeled as the central object in core collapse simulations using general relativistic three-flavor Boltzmann neutrino transport in spherical symmetry. The simulations are launched from several massive progenitors of 40 M{omicron} and 50 M{omicron}. We analyze the electron-neutrino luminosity dependencies and construct a simple approximation for the electron-neutrino luminosity, which depends only on the physical conditions at the electron-neutrinosphere. In addition, we analyze different ({mu}, {tau})-neutrino pair-reactions separately and compare the differences during the post-bounce phases of failed core collapse supernova explosions of massive progenitors. We also investigate the connection between the increasing {mu},{tau}-neutrino luminosity and the PNS contraction during the accretion phase before black hole formation. Comparing the different post bounce phases of the progenitor models under investigation, wemore » find large differences in the emitted neutrino spectra. These differences and the analysis of the electron-neutrino luminosity indicate a strong progenitor model dependency of the emitted neutrino signal.« less

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/22cde83c0acbefcd469c1ba5309bbb342e18db02

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Citations in the corpus

CORE-COLLAPSE SUPERNOVA EQUATIONS OF STATE BASED ON NEUTRON STAR OBSERVATIONS (2012, background): “This progenitor has been discussed before within the scenario of black-hole formation, also explored for the LS and STOS supernova EOSs (see, e.g., Sumiyoshi et al. 2006, 2007; Nakazato et al. 2008; Fischer et al. 2009; O’Connor & Ott 2011; Hempel et al. 2012).”
NEW EQUATIONS OF STATE IN SIMULATIONS OF CORE-COLLAPSE SUPERNOVAE (2011, methodology): “Here, one could expect that the maximum mass of a cold neutron star is correlated with the time until black hole formation and the corresponding neutrino signal, as was also found in previous studies of Sumiyoshi et al. (2007), Fischer et al. (2009), and O’Connor & Ott (2011).”
What can be learned from a future supernova neutrino detection (2017, methodology): “[197] and Sumiyoshi, Yamada and Suzuki [196] found a strong dependence of the neutrino spectra upon the progenitor, and several studies [199, 42, 200] observed a strong dependence of the number of detected neutrino events upon the EOS they used in the computations.”
A NEW MULTI-DIMENSIONAL GENERAL RELATIVISTIC NEUTRINO HYDRODYNAMIC CODE FOR CORE-COLLAPSE SUPERNOVAE. I. METHOD AND CODE TESTS IN SPHERICAL SYMMETRY (2010, methodology): “Different from the G15 run and from published long-time simulations of the same progenitor model (Fischer et al. 2009; Hüdepohl et al. 2010), we now use a new nuclear EOS kindly provided by J. Lattimer (2007, private communication) in the high-density regime; a more extensive discussion of this…”
CORE-COLLAPSE SUPERNOVA EXPLOSIONS TRIGGERED BY A QUARK–HADRON PHASE TRANSITION DURING THE EARLY POST-BOUNCE PHASE (2010, background): “General relativistic effects have been investigated with respect to the PNS collapse and black hole formation for several massive progenitor stars of 40 and 50 M⊙ in Fischer et al. (2009).”
Protoneutron star evolution and the neutrino-driven wind in general relativistic neutrino radiation hydrodynamics simulations (2009, background): “…via the annihilation of trapped electron-neutrino pairs, νe + ν̄e νµ/τ + ν̄ν/τ, as well as contributions from nucleon-recoil and weak magnetism as studied in Horowitz (2002) are investigated in Fischer et al. (2009) and are not taken into account in the present study of the neutrino driven wind.”
Symmetry energy impact in simulations of core-collapse supernovae (2013, background): “etric SN code AGILE-Boltztran and enhance the neutrino heating/cooling rates in order to trigger the explosion. Once the shock has been revived, we switch back to the standard rates (for details, see [73]). The mass fractions of free nucleons, alpha particles, and other light clusters are shown in t”
A simple approach to the supernova progenitor–explosion connection (2016, background): “The neutrino luminosity L ν (of electron neutrinos and anti-neutrinos) is modelled as consisting of an accretion component L acc , ζ , and a diffusive component L diff originating from deeper layers of the proto-neutron star (compare Fischer et al. 2009 ; M¨uller & Janka 2014).”
AN OPEN-SOURCE NEUTRINO RADIATION HYDRODYNAMICS CODE FOR CORE-COLLAPSE SUPERNOVAE (2014, methodology): “The same heavy-lepton neutrino luminosity structure is seen in Fischer et al. (2009).”
BLACK HOLE FORMATION IN FAILING CORE-COLLAPSE SUPERNOVAE (2010, methodology): “They are the largest forνx and the lowest forνe and increase with decreasing neutrinosphere radii (e.g., Thompson et al. 2003; Sumiyoshi et al. 2007; Ott et al. 2008; Fischer et al. 2009).”