Self-induced flavor conversion of supernova neutrinos on small scales

被引：54

作者：

Chakraborty, S. ^{[1
]}

Hansen, R. S. ^{[2
]}

Izaguirre, I. ^{[1
]}

Ragffelt, G. G. ^{[1
]}

机构：

[1] Max Planck Inst Phys & Astrophys, Werner Heisenberg Inst, Fohringer Ring 6, D-80805 Munich, Germany

[2] Univ Aarhus, Dept Phys & Astron, DK-8000 Aarhus C, Denmark

来源：

JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS | 2016年 / 01期

关键词：

core-collapse supernovas; supernova neutrinos; CORE-COLLAPSE SUPERNOVAE; DRIVEN SUPERNOVA; 3; DIMENSIONS; OSCILLATIONS; EXPLOSIONS; PROGENITOR; MATTER; HYDRODYNAMICS; SIMULATIONS; CONVECTION;

D O I：

10.1088/1475-7516/2016/01/028

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Self-induced flavor conversion of supernova (SN) neutrinos is a generic feature of neutrino-neutrino dispersion. The corresponding run-away modes in flavor space can spontaneously break the original symmetries of the neutrino flux and in particular can spontaneously produce small-scale features as shown in recent schematic studies. However, the unavoidable "multi-angle matter effect" shifts these small-scale instabilities into regions of matter and neutrino density which are not encountered on the way out from a SN. The traditional modes which are uniform on the largest scales are most prone for instabilities and thus provide the most sensitive test for the appearance of self-induced flavor conversion. As a by-product we clarify the relation between the time evolution of an expanding neutrino gas and the radial evolution of a stationary SN neutrino flux. Our results depend on several simplifying assumptions, notably stationarity of the solution, the absence of a "backward" neutrino flux caused by residual scattering, and global spherical symmetry of emission.

引用

页数：50

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