Detecting the QCD phase transition in the next Galactic supernova neutrino burst

Dasgupta, Basudeb; Fischer, Tobias; Horiuchi, Shunsaku; Liebendörfer, M.; Mirizzi, Alessandro; Sagert, Irina; Schaffner-Bielich, J.

doi:10.1103/physrevd.81.103005

Cited by 48 publications

(59 citation statements)

References 40 publications

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“…At these densities, hyperons, kaons, and quarks, if they appear at all, should not play a dominant role [46]. However, their possible appearance in a first order phase transition could be probed in the neutrino signal of a galactic supernova explosion [47,48]. In Fig.…”

Section: Implications Of the Nuclear Symmetry Energy On Radii Anmentioning

confidence: 99%

Soft nuclear equation-of-state from heavy-ion data and implications for compact stars

Sagert

Tolós

Chatterjee³

et al. 2012

Phys. Rev. C

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Measurements of kaon production at subthreshold energies in heavy-ion collisions point to a soft nuclear equation-of-state for densities up to 2-3 times nuclear matter saturation density. We apply these results to study the implications on compact star properties, especially in the context of the recent measurement of the two solar mass pulsar PSR J1614-2230. The implications are twofold: Firstly, the heavy-ion results constrain nuclear matter at densities relevant to light neutron stars. Hence, a radius measurement could provide information about the density dependence of the symmetry energy which is a crucial quantity in nuclear physics. Secondly, the information on the nucleon potential obtained from the analysis of the heavy-ion data can be combined with restrictions from causality on the nuclear equation-of-state. From this we can derive a limit for the highest allowed compact star mass of three solar masses.

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Section: Implications Of the Nuclear Symmetry Energy On Radii Anmentioning

confidence: 99%

Soft nuclear equation-of-state from heavy-ion data and implications for compact stars

Sagert

Tolós

Chatterjee³

et al. 2012

Phys. Rev. C

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“…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. Fischer et al 2010 and references therein).…”

Section: Supernovae and Neutrinosmentioning

confidence: 99%

“…Following original work by Takahara & Sato (1988), recent simulations (Dasgupta et al 2010) of certain stellar corecollapse supernovae predict a sharp burst ofν e several hundred milliseconds after the prompt ν e neutronization burst associated with a quark-hadron phase transition at high baryon densities. A detection of this prominent feature would constitute direct evidence of quark matter.…”

Section: Supernovae and Neutrinosmentioning

confidence: 99%

“…In addition, we introduce specific models by Dasgupta et al (2010) and Sumiyoshi et al (2007) that were selected to demonstrate IceCube's physics performance in Sect. 6.…”

Section: Supernovae and Neutrinosmentioning

confidence: 99%

“…This class of stars may represent up to 30% of all core collapse supernovae. Recent simulations by Fischer et al (2010) and Hüdepohl et al (2010) extend over 22 s from the collapse of a 8.8 M progenitor to the completed formation of the deleptonized neutron star. They are the only examples so far where one-dimensional simulations obtain neutrino-powered supernova explosions and two-dimensional simulations yield only minor dynamical and energetic modifcations.…”

Section: Supernovae and Neutrinosmentioning

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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Detecting extra-galactic supernova neutrinos in the Antarctic ice

Böser

Kowalski

Schulte

et al. 2015

Astroparticle Physics

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Building on the technological success of the IceCube neutrino telescope, we outline a prospective low-energy extension that utilizes the clear ice of the South Pole. Aiming at a 10 Mton effective volume and a 10 MeV threshold, the detector would provide sufficient sensitivity to detect neutrino bursts from core-collapse supernovae (SNe) in nearby galaxies. The detector geometry and required density of instrumentation are discussed along with the requirements to control the various sources of background, such as solar neutrinos. In particular, the suppression of spallation events induced by atmospheric muons poses a challenge that will need to be addressed. Assuming this background can be controlled, we find that the resulting detector will be able to detect SNe from beyond 10 Mpc, delivering between 10 and 41 regular core-collapse SN detections per decade. It would further allow to study more speculative phenomena, such as optically dark (failed) SNe, where the collapse proceeds directly to a black hole, at a detection rate similar to that of regular SNe. We find that the biggest technological challenge lies in the required number of large area photo-sensors, with simultaneous strict limits on the allowed noise rates. If both can be realized, the detector concept we present will reach the required sensitivity with a comparatively small construction effort and hence offers a route to future routine observations of SNe with neutrinos.Comment: revised to include full treatment of diffusive ice, conclusion unchange

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Detecting the QCD phase transition in the next Galactic supernova neutrino burst

Cited by 48 publications

References 40 publications

Soft nuclear equation-of-state from heavy-ion data and implications for compact stars

Soft nuclear equation-of-state from heavy-ion data and implications for compact stars

IceCube sensitivity for low-energy neutrinos from nearby supernovae

Detecting extra-galactic supernova neutrinos in the Antarctic ice

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