Three-dimensional Boltzmann-Hydro Code for Core-collapse in Massive Stars. II. The Implementation of Moving-mesh for Neutron Star Kicks

Nagakura, Hiroki; Iwakami, Wakana; Furusawa, Shun; Sumiyoshi, K.; Yamada, Shoichi; Matsufuru, Hideo; Imakura, Akira

doi:10.3847/1538-4365/aa69ea

Cited by 67 publications

(85 citation statements)

References 59 publications

(92 reference statements)

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“…The details of the code development of our Boltzmann solver are described in a series of papers Nagakura et al 2014Nagakura et al , 2017Nagakura et al , 2019d and its reliability has been well established by a detailed comparison to another Monte-Carlo neutrino transport code (Richers et al 2017). Some results of axisymmetric CCSN simulations by using our code can be seen in Nagakura et al (2018); Harada et al (2019); Nagakura et al (2019c).…”

Section: Ccsn Modelmentioning

confidence: 96%

Fast-pairwise Collective Neutrino Oscillations Associated with Asymmetric Neutrino Emissions in Core-collapse Supernovae

Nagakura

Morinaga

Kato

et al. 2019

ApJ

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107

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We present a linear stability analysis of the fast-pairwise neutrino flavor conversion based on a result of our latest axisymmetric core-collapse supernova (CCSN) simulation with full Boltzmann neutrino transport. In the CCSN simulation, coherent asymmetric neutrino emissions of electron-type neutrinos (ν e ) and their anti-particles (ν e ), in which the asymmetry of ν e andν e is anti-correlated with each other, occur at almost the same time as the onset of aspherical shock expansion. We find that the asymmetric neutrino emissions play a crucial role on occurrences of fast flavor conversions. The linear analysis shows that unstable modes appear in both pre-and post-shock flows; for the latter they appear only in the hemisphere of higherν e emissions (the same hemisphere with stronger shock expansion). We analyze in depth the characteristics of electron-lepton-number (ELN) crossing by closely inspecting the angular distributions of neutrinos in momentum space. The ELN crossing happens in various ways, and the property depends on the radius: in the vicinity of neutron star,ν e (ν e ) dominates over ν e (ν e ) in the forward (backward) direction: at the larger radius the ELN crossing occurs in the opposite way. We also find that the non-radial ELN crossing occurs at the boundary between no ELN crossing and the radial one, which is an effect of genuine multi-D transport. Our findings indicate that the collective neutrino oscillation may occur more commonly in CCSNe and suggest that the CCSN community needs to accommodate these oscillations self-consistently in the modelling of CCSNe.

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Section: Ccsn Modelmentioning

confidence: 96%

Fast-pairwise Collective Neutrino Oscillations Associated with Asymmetric Neutrino Emissions in Core-collapse Supernovae

Nagakura

Morinaga

Kato

et al. 2019

ApJ

Self Cite

107

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“…Theoretically, it has been considered that a canonical core-collapse supernova could be triggered by the delayed neutrino heating aided by convection (Herant et al 1994) and/or standing accretion shock instability (SASI) (Blondin et al 2003), where multi-dimensional effects are essential (for a review of the mechanism of core-collapse supernovae, see Kotake et al 2012a,b;Janka 2012;Janka et al 2012;Burrows 2013;Müller 2016). Hitherto, based on the delayed neutrino heating mechanism many twodimensional (2D) and 3D hydrodynamical simulations with an approximate neutrino transport have been performed for a few decades (Burrows et al 1995a;Kifonidis et al 2003;Scheck et al 2006;Kifonidis et al 2006;Scheck et al 2008;Marek & Janka 2009;Suwa et al 2010;Nordhaus et al 2010b;Müller et al 2012b,a;Takiwaki et al 2012;Kuroda et al 2012;Müller et al 2012c;Bruenn et al 2013;Wongwathanarat et al 2013;Couch & Ott 2013;Hanke et al 2013;Dolence et al 2013;Ott et al 2013;Nakamura et al 2014;Takiwaki et al 2014;Couch & O'Connor 2014;Couch & Ott 2015;Bruenn et al 2016;Pan et al 2016;Radice et al 2016;Nagakura et al 2017;Radice et al 2017;Müller et al 2017;Vartanyan et al 2019;Burrows et al 2019). Since the involved physical effects, e.g., neutrino transport, general relativity, and n...…”

Section: Introductionmentioning

confidence: 99%

Matter Mixing in Aspherical Core-collapse Supernovae: Three-dimensional Simulations with Single-star and Binary Merger Progenitor Models for SN 1987A

Ono

Nagataki

Ferrand

et al. 2020

ApJ

104

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We perform three-dimensional hydrodynamic simulations of aspherical core-collapse supernovae focusing on the matter mixing in SN 1987A. The impacts of four progenitor (pre-supernova) models and parameterized aspherical explosions are investigated. The four pre-supernova models include a blue supergiant (BSG) model based on a slow merger scenario developed recently for the progenitor of SN 1987A (Urushibata et al. 2018. The others are a BSG model based on a single star evolution and two red supergiant (RSG) models. Among the investigated explosion (simulation) models, a model with the binary merger progenitor model and with an asymmetric bipolar-like explosion, which invokes a jetlike explosion, best reproduces constraints on the mass of high velocity 56 Ni, as inferred from the observed [Fe II] line profiles. The advantage of the binary merger progenitor model for the matter mixing is the flat and less extended ρ r 3 profile of the C+O core and the helium layer, which may be characterized by the small helium core mass. From the best explosion model, the direction of the bipolar explosion axis (the strongest explosion direction), the neutron star (NS) kick velocity, and its direction are predicted. Other related implications and future prospects are also given.

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“…The velocity actually corresponds to the shift vector, which is chosen to track approximately the motion of PNS (seeNagakura et al (2017)). …”

mentioning

confidence: 99%

Possible Early Linear Acceleration of Proto-neutron Stars via Asymmetric Neutrino Emission in Core-collapse Supernovae

Nagakura

Sumiyoshi

Yamada

2019

ApJL

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In this Letter, we present the result of an axisymmetric CCSN simulation conducted with appropriate treatments of neutrino transport and proper motions of proto-neutron star (PNS), in which a remarkable PNS acceleration is observed in association with asymmetric neutrino emissions by the time of 300ms after bounce. We find that these asymmetric neutrino emissions play important roles in the acceleration of PNS in this phase. The correlation between the PNS proper motion and the asymmetric ejecta is similar to that in the neutron star (NS) kick of hydrodynamic origin. Both electron-type neutrinos (ν e ) and their anti-particles (ν e ) have ∼ 10% level of asymmetry between the northern and southern hemispheres, while other heavy-leptonic neutrinos (ν x ) have much smaller asymmetry of ∼ 1%. The emissions ofν e and ν x are higher in the hemisphere of stronger shock expansion whereas the ν e emission is enhanced in the opposite hemisphere: in total the neutrinos carry some linear momentum to the hemisphere of the stronger shock expansion. The asymmetry is attributed to the non-spherical distribution of electron-fraction (Y e ) in the envelope of PNS. Although it is similar to LESA (lepton-emission self-sustained asymmetry), the Y e asymmetry seems to be associated with the PNS motion: the latter triggers lateral circular motions in the envelope of PNS by breaking symmetry of the matter distribution there, which are then sustained by a combination of convection, lateral neutrino diffusion and matter-pressure gradient. Our findings may have an influence on the current theories on the NS kick mechanism although long-term simulations are required to assess their impact on the later evolution.

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Three-dimensional Boltzmann-Hydro Code for Core-collapse in Massive Stars. II. The Implementation of Moving-mesh for Neutron Star Kicks

Cited by 67 publications

References 59 publications

Fast-pairwise Collective Neutrino Oscillations Associated with Asymmetric Neutrino Emissions in Core-collapse Supernovae

Fast-pairwise Collective Neutrino Oscillations Associated with Asymmetric Neutrino Emissions in Core-collapse Supernovae

Matter Mixing in Aspherical Core-collapse Supernovae: Three-dimensional Simulations with Single-star and Binary Merger Progenitor Models for SN 1987A

Possible Early Linear Acceleration of Proto-neutron Stars via Asymmetric Neutrino Emission in Core-collapse Supernovae

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