Supernova Neutrino Light Curves and Spectra for Various Progenitor Stars: From Core Collapse to Proto-Neutron Star Cooling

Nakazato, Ken’ichiro; Sumiyoshi, Kohsuke; Suzuki, Hideyuki; Totani, Tomonori; Umeda, Hideyuki; Yamada, Shoichi

doi:10.1088/0067-0049/205/1/2

Cited by 160 publications

(207 citation statements)

References 63 publications

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“…In Fig.1, the progenitor mass is 13, 15 and 27 M ⊙ from top to bottom. The time evolution of the average energy and the luminosity is quantitatively different in each models, however these qualitative behaviours are rather similar to previous studies (e.g., [19]). For each of the models, we calculate the neutrino spectra at the neutrino sphere (PNS) using these average energies and luminosities (e.g., [14,15]).…”

Section: Supernova Model and Numerical Methodssupporting

confidence: 88%

Effects of Collective Oscillation and MSW Matter Effect on 3d Hydrodynamics Core-Collapse Supernova Models

Kawagoe¹

2015

Proceedings of XIII Nuclei in the Cosmos — PoS(NIC XIII)

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We investigate possible impacts of collective oscillations and MSW matter effects on neutrino signals from core-collapse supernovae (CCSNe). Using results of spherically-symmetric and three-dimensional radiation-hydrodynamics CCSN simulations for multiple progenitors (11.2, 13, 15, 27 and 40 M ⊙ ), we estimate the neutrino signals, in which both of the collective oscillations and the MSW effects are taken into account. As previously identified, the collective oscillations are unlikely to impact the revival of a stalled supernova shock for most of the progenitors, while we find that they could potentially affect the subsequent evolution of the revived shock in a lighter progenitor model (11.3M ⊙ ). Neutrinos emitted from a nascent proto-neutron star (PNS) change its flavor typically twice in propagating out to the stellar mantle due to the collective oscillations and the MSW effects. As a result, the spectrum of anti-electron type neutrinos (ν e ) becomes relatively close to those emitted from the PNS. For a variety of the progenitor models, we estimate the event numbers in Super-Kamiokande and discuss how the behaviors of the signals are sensitive to the employed progenitors.

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Section: Supernova Model and Numerical Methodssupporting

confidence: 88%

Effects of Collective Oscillation and MSW Matter Effect on 3d Hydrodynamics Core-Collapse Supernova Models

Kawagoe¹

2015

Proceedings of XIII Nuclei in the Cosmos — PoS(NIC XIII)

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“…Smaller energy differences are found in recent long term simulations, e.g. Hüdepohl et al [14] and Nakazato et al [13], where energies are on the order of E νe = 9 − 10.1 MeV, Eν e = 11.5 − 12.9 MeV and E νx ∼ 13 MeV. Among others, Roberts et al [51] and Horowitz et al [52] have pointed out that the neutrino opacities and interaction cross sections used by the modeling community are not as correct as they could be.…”

Section: Introductionmentioning

confidence: 69%

Combining collective, MSW, and turbulence effects in supernova neutrino flavor evolution

Lund¹,

Kneller²

2013

Phys. Rev. D

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In order to decode the neutrino burst signal from a Galactic core-collapse supernova (ccSN) and reveal the complicated inner workings of the explosion we need a thorough understanding of the neutrino flavor evolution from the proto-neutron star outwards. The flavor content of the signal evolves due to both neutrino collective effects and matter effects which can lead to a highly interesting interplay and distinctive spectral features. In this paper we investigate the supernova neutrino flavor evolution in three different progenitors and include collective flavor effects, the evolution of the Mikheyev, Smirnov & Wolfenstein (MSW) conversion due to the shock wave passage through the star, and the impact of turbulence. We consider both normal and inverted neutrino mass hierarchies and a value of θ13 close to the current experimental measurements. In the Oxygen-Neon-Magnesium (ONeMg) supernova we find that the impact of turbulence is both brief and slight during a window of 1-2 seconds post bounce. This is because the shock races through the star extremely quickly and the turbulence amplitude is expected to be small, less than 10%, since these stars do not require multi-dimensional physics to explode. Thus the spectral features of collective and shock effects in the neutrino signals from Oxygen-Neon-Magnesium supernovae may be almost turbulence free making them the easiest to interpret. For the more massive progenitors we again find that small amplitude turbulence, up to 10%, leads to a minimal modification of the signal, and the emerging neutrino spectra retain both collective and MSW features. However, when larger amounts of turbulence is added, 30% and 50%, which is justified by the requirement of multi-dimensional physics in order to make these stars explode, the features of collective and shock wave effects in the high (H) density resonance channel are almost completely obscured at late times. Yet at the same time we find the other mixing channels -the low (L) density resonance channel and the non-resonant channels -begin to develop turbulence signatures. Large amplitude turbulent motions in the outer layers of more massive, iron core-collapse supernovae may obscure the most obvious fingerprints of collective and shock wave effects in the neutrino signal but cannot remove them completely, and additionally bring about new features in the signal.

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“…Here, to study the validity of this approximation, we utilize the spectrum of binary BH merger proposed by Ajith et al (2011) for comparison. For illustration, we adopt the critical metallicity Z crit = Z ⊙ / √ 5 from the heavy-BH formation model in Nakazato et al (2013Nakazato et al ( , 2015, while the choice of Z crit does not affect the result for the GW spectrum. Furthermore, we assume the distribution of binary chirp mass based on the results of the first observational run of the Advanced LIGO detectors (Abbott et al 2016f).…”

Section: Discussionmentioning

confidence: 99%

“…The upper and lower ones are for the cases with (R BH m (0), t min ) = (240 Gpc −3 yr −1 , 50 Myr) and (R BH m (0), t min ) = (9 Gpc −3 yr −1 , 5 Gyr), respectively. The sensitivity curves correspond, from top to bottom, to observation runs O1, O2 and O5 from Abbott et al (2016c). 2004; Nakazato et al 2013). Therefore, the BH binaries found as GW150914 are expected to have been formed in a low-metallicity environment (Belczynski et al 2010a,b;Spera et al 2015;Abbott et al 2016b).…”

Section: +4mentioning

confidence: 99%

Gravitational Wave Background From Binary Mergers and Metallicity Evolution of Galaxies

Nakazato

Niino

Sago

2016

ApJ

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The cosmological evolution of the binary black hole (BH) merger rate and the energy density of the gravitational-wave (GW) background are investigated. To evaluate the redshift dependence of the BH formation rate, BHs are assumed to originate from low-metallicity stars, and the relations between the star formation rate, metallicity and stellar mass of galaxies are combined with the stellar mass function at each redshift. As a result, it is found that when the energy density of the GW background is scaled with the merger rate at the local Universe, the scaling factor does not depend on the critical metallicity for the formation of BHs. Also taking into account the merger of binary neutron stars, a simple formula to express the energy spectrum of the GW background is constructed for the inspiral phase. The relation between the local merger rate and the energy density of the GW background will be examined by future GW observations.

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Supernova Neutrino Light Curves and Spectra for Various Progenitor Stars: From Core Collapse to Proto-Neutron Star Cooling

Cited by 160 publications

References 63 publications

Effects of Collective Oscillation and MSW Matter Effect on 3d Hydrodynamics Core-Collapse Supernova Models

Effects of Collective Oscillation and MSW Matter Effect on 3d Hydrodynamics Core-Collapse Supernova Models

Combining collective, MSW, and turbulence effects in supernova neutrino flavor evolution

Gravitational Wave Background From Binary Mergers and Metallicity Evolution of Galaxies

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