Phase Transition of Hot Neutron Matter to π<sup>0</sup>-Condensed State

Takahara, Mariko; Takatsuka, Tatsuyuki; Sato, Katsuhiko

doi:10.1143/ptp.86.57

Cited by 17 publications

(20 citation statements)

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“…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: 91%

IceCube sensitivity for low-energy neutrinos from nearby supernovae

Abbasi¹,

Abdou²,

Abu‐Zayyad³

et al. 2011

A&A

133

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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: Supernovae and Neutrinosmentioning

confidence: 91%

IceCube sensitivity for low-energy neutrinos from nearby supernovae

Abbasi¹,

Abdou²,

Abu‐Zayyad³

et al. 2011

A&A

133

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“…Recently, the possible appearance of quark matter in the supernova core received increasing attention (see, e.g., [5,43,44,49]). Therefore, we also show results obtained for simulations which include the QB EOS.…”

Section: Simulations In Spherical Symmetrymentioning

confidence: 99%

“…Depending on the model, they can be both consistent with nuclear physics and give large neutron star masses. Moreover, the large uncertainty in the properties of high-density nuclear matter results in a relatively large freedom in the exploration of the quark or hyperon impact in core-collapse supernova studies [5,[43][44][45][46][47][48][49][50]. With that, we construct a quark-hadron hybrid EOS (hereafter QB), that allows for large hybrid star maximum masses of 2.01 M .…”

Section: Introductionmentioning

confidence: 99%

Symmetry energy impact in simulations of core-collapse supernovae

et al. 2014

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Abstract. We present a review of a broad selection of nuclear matter equations of state (EOSs) applicable in core-collapse supernova studies. The large variety of nuclear matter properties, such as the symmetry energy, which are covered by these EOSs leads to distinct outcomes in supernova simulations. Many of the currently used EOS models can be ruled out by nuclear experiments, nuclear many-body calculations, and observations of neutron stars. In particular the two classical supernova EOS describe neutron matter poorly. Nevertheless, we explore their impact in supernova simulations since they are commonly used in astrophysics. They serve as extremely soft and stiff representative nuclear models. The corresponding supernova simulations represent two extreme cases, e.g., with respect to the protoneutron star (PNS) compactness and shock evolution. Moreover, in multi-dimensional supernova simulations EOS differences have a strong effect on the explosion dynamics. Because of the extreme behaviors of the classical supernova EOSs we also include DD2, a relativistic mean field EOS with density-dependent couplings, which is in satisfactory agreement with many current nuclear and observational constraints. This is the first time that DD2 is applied to supernova simulations and compared with the classical supernova EOS. We find that the overall behaviour of the latter EOS in supernova simulations lies in between the two extreme classical EOSs. As pointed out in previous studies, we confirm the impact of the symmetry energy on the electron fraction. Furthermore, we find that the symmetry energy becomes less important during the post-bounce evolution, where conversely the symmetric part of the EOS becomes increasingly dominating, which is related to the high temperatures obtained. Moreover, we study the possible impact of quark matter at high densities and light nuclear clusters at low and intermediate densities.

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“…Phase transitions have long been investigated in the context of SNe [9] and neutron stars [10]. By including prescriptions of additional matter in the equation of state (EoS), many simulations predict the appearance of strange matter in the form of hyperons, a kaon condensate, or quark matter at supernuclear densities [10][11][12].…”

Section: Introductionmentioning

confidence: 99%

“…In this paper we concentrate on recent developments in quarkhadron phase transitions. Initial attempts were based on general relativistic hydrodynamics using a parametrized equation of state [9], discussing possible relations to the neutrino spectrum of SN1987A [13]. Applying a more sophisticated equation of state, the formation of a strong second shock wave was found as a direct consequence of the phase transition [14].…”

Section: Introductionmentioning

confidence: 99%

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

et al. 2010

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Predictions of the thermodynamic conditions for phase transitions at high baryon densities and large chemical potentials are currently uncertain and largely phenomenological. Neutrino observations of core-collapse supernovae can be used to constrain the situation. Recent simulations of stellar core-collapse that include a description of quark matter, predict a sharp burst ofνe several hundred milliseconds after the prompt νe neutronization burst. We study the observational signatures of thatνe burst at current neutrino detectors -IceCube and Super-Kamiokande. For a Galactic corecollapse supernova, we find that signatures of the QCD phase transition can be detected, regardless of the neutrino oscillation scenario. The detection would constitute strong evidence of a phase transition in the stellar core, with implications for the equation of state at high matter density and the supernova explosion mechanism.

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Phase Transition of Hot Neutron Matter to π⁰-Condensed State

Cited by 17 publications

References 0 publications

IceCube sensitivity for low-energy neutrinos from nearby supernovae

IceCube sensitivity for low-energy neutrinos from nearby supernovae

Symmetry energy impact in simulations of core-collapse supernovae

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

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Phase Transition of Hot Neutron Matter to π0-Condensed State

Cited by 17 publications

References 0 publications

IceCube sensitivity for low-energy neutrinos from nearby supernovae

IceCube sensitivity for low-energy neutrinos from nearby supernovae

Symmetry energy impact in simulations of core-collapse supernovae

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

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Phase Transition of Hot Neutron Matter to π⁰-Condensed State