Exploiting the neutronization burst of a galactic supernova

Kachelrieß, M.; Tomàs, R.; Buras, R.; Janka, Hans-Thomas; Marek, Andreas; Rampp, Markus

doi:10.1103/physrevd.71.063003

Cited by 147 publications

(213 citation statements)

References 56 publications

(62 reference statements)

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“…The ν e rate from the neutronization burst is largely independent of the progenitor mass; the corresponding uncertainties are estimated to be around 10%; uncertainties arising from neutrino oscillations are estimated to be below 5% for a normal hierarchy (Kachelriess et al 2005).…”

Section: External Sources Of Systematicsmentioning

confidence: 97%

“…The shock stalls but is presumably soon revived by interactions of the large flux of neutrinos generated in the proto-neutron star. The models describing the prompt neutronization burst appear to be robust and consistent (Kachelriess et al 2005). The proto-neutron star subsequently cools over ∼20 s. The neutrino flux decreases until neutrinos are no longer produced in the cooled down protoneutron star (see e.g.…”

Section: Supernovae and Neutrinosmentioning

confidence: 99%

“…While differences in the onset of the neutrino emission between various models are small (Kachelriess et al 2005), the models have yet to overcome problems with the supernova explosion mechanisms. The theoretical knowledge about the neutrino emission at times longer than several 100 μs after the deleptonization (Buras et al 2003;Kitaura et al 2006) is limited.…”

Section: Introductionmentioning

confidence: 99%

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IceCube sensitivity for low-energy neutrinos from nearby supernovae

Abbasi¹,

Abdou²,

Abu‐Zayyad³

et al. 2011

A&A

138

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This paper describes the response of the IceCube neutrino telescope located at the geographic south pole to outbursts of MeV neutrinos from the core collapse of nearby massive stars. IceCube was completed in December 2010 forming a lattice of 5160 photomultiplier tubes that monitor a volume of ∼1 km 3 in the deep Antarctic ice for particle induced photons. The telescope was designed to detect neutrinos with energies greater than 100 GeV. Owing to subfreezing ice temperatures, the photomultiplier dark noise rates are particularly low. Hence IceCube can also detect large numbers of MeV neutrinos by observing a collective rise in all photomultiplier rates on top of the dark noise. With 2 ms timing resolution, IceCube can detect subtle features in the temporal development of the supernova neutrino burst. For a supernova at the galactic center, its sensitivity matches that of a background-free megaton-scale supernova search experiment. The sensitivity decreases to 20 standard deviations at the galactic edge (30 kpc) and 6 standard deviations at the Large Magellanic Cloud (50 kpc). IceCube is sending triggers from potential supernovae to the Supernova Early Warning System. The sensitivity to neutrino properties such as the neutrino hierarchy is discussed, as well as the possibility to A109, page 1 of 18 detect the neutronization burst, a short outbreak of ν e 's released by electron capture on protons soon after collapse. Tantalizing signatures, such as the formation of a quark star or a black hole as well as the characteristics of shock waves, are investigated to illustrate IceCube's capability for supernova detection.

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Section: External Sources Of Systematicsmentioning

confidence: 97%

Section: Supernovae and Neutrinosmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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IceCube sensitivity for low-energy neutrinos from nearby supernovae

Abbasi¹,

Abdou²,

Abu‐Zayyad³

et al. 2011

A&A

138

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“…Depending upon mixing angles and matter densities achieved during the collapse, neutrinos in supernovae may also experience matter-enhanced MikheyevSmirnov-Wolfenstein (MSW) resonances [26]. It has also been predicted [27,28] that the mass hierarchy, whether "normal" (m 1 < m 2 < m 3 ) or "inverted" (m 3 < m 1 < m 2 ), will alter the emergent neutrino spectra if there is mixing and may even be detectable by the associated ν-process nucleosynthesis in the C/He shell [29,30]. In addition, neutrino self-interactions [31] may be important but are not as well understood due to their nonlinear nature.…”

Section: Introductionmentioning

confidence: 99%

Sterile neutrino oscillations in core-collapse supernovae

et al. 2014

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We have made core-collapse supernova simulations that allow oscillations between electron neutrinos (or their antiparticles) with right-handed sterile neutrinos. We have considered a range of mixing angles and sterile neutrino masses including those consistent with sterile neutrinos as a dark matter candidate. We examine whether such oscillations can impact the core bounce and shock reheating in supernovae. We identify the optimum ranges of mixing angles and masses that can dramatically enhance the supernova explosion by efficiently transporting electron antineutrinos from the core to behind the shock, where they provide additional heating leading to much larger explosion kinetic energies. We show that this effect can cause stars to explode that otherwise would have collapsed. We find that an interesting periodicity in the neutrino luminosity develops due to a cycle of depletion of the neutrino density by conversion to sterile neutrinos that shuts off the conversion, followed by a replenished neutrino density as neutrinos transport through the core.

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“…The burst peak shown in Figure 2 is fairly independent of the details of the SN models such as electron capture rates, nuclear equation of state and the progenitor mass. In fact, the neutronization burst phase is considered as the "standard neutrino candle" for the core-collapse supernovae scenario, and thus serves as one of the most sensitive probes of the physics of neutrino oscillation [25] and nonstandard physics [26].…”

Section: Supernova Neutrinos and Their Detection In Dark Matter mentioning

confidence: 99%

Observing supernova neutrino light curve in future dark matter detectors

2014

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The possibility of observing supernova (SN) neutrinos through the process of coherent elastic neutrino-nucleus scattering (CENNS) in future ton scale detectors designed primarily for direct detection of dark matter is investigated. In particular, we focus on the possibility of distinguishing the various phases of the SN neutrino emission. The neutrino emission rates from the recent long term Basel/Darmstadt simulations are used to calculate the expected event rates. The recent stateof-the-art SN simulations predict closer fluxes among different neutrino flavors and lower average energies compared to the earlier simulation models. We find that our estimated total event rates are typically a factor of two lower than those predicted using older simulation models. We further find that, with optimistic assumptions on the detector's time resolution (∼ 10 ms) and energy threshold (∼ 0.1 keV), the neutrinos associated with the accretion phase of the SN can in principle be demarcated out with, for example, a 10-ton Xe detector, although distinguishing the neutrinos associated with the neutronization burst phase of the explosion would typically require several tens of ton detectors. We also comment on the possibility of studying the properties of non-electron flavor neutrinos from the CENNS of SN neutrinos.

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Exploiting the neutronization burst of a galactic supernova

Cited by 147 publications

References 56 publications

IceCube sensitivity for low-energy neutrinos from nearby supernovae

IceCube sensitivity for low-energy neutrinos from nearby supernovae

Sterile neutrino oscillations in core-collapse supernovae

Observing supernova neutrino light curve in future dark matter detectors

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