Neutrino emission characteristics and detection opportunities based on three-dimensional supernova simulations

被引：117

作者：

Tamborra, Irene ^{[1
]}

Raffelt, Georg ^{[2
]}

Hanke, Florian ^{[3
,4
]}

Janka, Hans-Thomas ^{[3
]}

Mueller, Bernhard ^{[5
]}

机构：

[1] Univ Amsterdam, GRAPPA Inst, NL-1098 XH Amsterdam, Netherlands

[2] Werner Heisenberg Inst, Max Planck Inst Phys, D-80805 Munich, Germany

[3] Max Planck Inst Astrophys, D-85748 Garching, Germany

[4] Tech Univ Munich, Dept Phys, D-85748 Garching, Germany

[5] Monash Univ, Sch Math Sci, Monash Ctr Astrophys, Clayton, Vic 3800, Australia

来源：

PHYSICAL REVIEW D | 2014年 / 90卷 / 04期

关键词：

CORE-COLLAPSE SUPERNOVAE; EQUATION-OF-STATE; MASSIVE STARS; HYDRODYNAMICS CODE; DRIVEN EXPLOSIONS; SASI ACTIVITY; SHOCK; CONVECTION; MECHANISM; EVOLUTION;

D O I：

10.1103/PhysRevD.90.045032

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The neutrino emission characteristics of the first full-scale three-dimensional supernova simulations with sophisticated three-flavor neutrino transport for three models with masses 11.2, 20, and 27M(circle dot) are evaluated in detail. All the studied progenitors show the expected hydrodynamical instabilities in the form of large-scale convective overturn. In addition, the recently identified lepton-number emission self-sustained asymmetry (LESA) phenomenon is generic for all our cases. Standing accretion-shock instability (SASI) activity appears in the 20 and 27M(circle dot) cases, partly in the form of a spiral mode, inducing large but direction-and flavor-dependent modulations of neutrino emission. These modulations can be clearly identified in the existing IceCube and future Hyper-Kamiokande detectors, depending on the distance and detector location relative to the main standing accretion-shock instability sloshing direction.

引用

页数：18

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