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: Neutrino quantum states and spin light in matter
.

.. .. ..

- 2 2010


A. Grigoriev, A. Lokhov, A. Studenikin, A. Ternov

"Spin light in neutrino transition between different mass states in matter"
arXiv:1003.0630 [hep-ph]


New mechanism of electromagnetic radiation by neutrino in matter

Recent review of neutrino electromagnetic properties see:
C. Giunti, A. Studenikin, Phys.Atom.Nucl. 72, 2151 (2009)

Spin Light of Neutrino in matter (gamma-rays for relativistic neutrinos

~ 1/3 E )

A.Lobanov, A.Studenikin, Phys.Lett.B; 564 (2003) 27; 601 (2004) 171 A.Studenikin, A.Ternov, Phys.Lett.B 608 (2005) 107 A.Grigoriev, A.Studenikin, A.Ternov, Phys.Lett.B 622 (2005) 199


Neutrino radiative decay in vacuum

was also considered before:
S. G. A. P. C. Petcov, Nucl. Phys. 25 (1977) 641 Zatsepin, A. Smirnov, Nucl. Phys. 28 (1978) 6 De Rujula and S. L. Glashow, Phys. Rev. Lett. 45 (1980) 942 Pal, L. Wolfenstein, Phys.Rev.D 25 (1982) 766 Giunti, C.W. Kim, W.P. Lam, Phys.Rev.D 43 (1991) 164


Neutrinos weak interaction with matter is taking into account: we use exact wave functions for the initial and final neutrinos in presence of matter
is coupled to

neutrinos by transition magnetic moment

high density of matter

(neutron stars)
relativistic neutrinos


Modified Dirac Equation

for unpolarized and matter at rest

neutrino energy spectrum
matter density parameter

neutrino momentum
S is neutrino helicity

= ±1

defines positive and negative energy solutions

nn

is neutron number density

A. Studenikin, A. Ternov Phys.Lett. B 60 (2005) 107 A. Studenikin, J.Phys. A:Math.Theor. 41 (2008) 16402


Total rate
Parameters:

Ultrahigh density

matter density parameter

for

High density

Low density

Heavy neutrino


Conclusions
The theory of spin light of neutrino in matter is now generalized for the case of neutrino transition between two different mass states (originally SLv was considered for the case of equal masses of neutrino in initial and final states) The rate of the process provided by the transition magnetic moment is of the same order as provided by the diagonal one The energy spectrum of SLv for the case of relativistic neutrino moving in dense matter span up to the range peculiar for gamma-rays In the case of ultra-relativistic neutrino energies and high densities of matter (astrophysical applications) the neutrino mass difference gives subdominant effect In the case of low neutrino energies and low densities of matter in the leading order our result is in agreement with
A. De Rujula and S. L. Glashow; G. Zatsepin, A.Smirnov; S. Petcov; P. Pal, L. Wolfenstein

The rate of SLv is determined by the value of neutrino effective magnetic (transition) moment



Neutrino magnetic moment
Recent review of neutrino electromagnetic properties see:
C. Giunti, A. Studenikin, Phys.Atom.Nucl. 72, 2151 (2009)

Theory SM with massive neutrino

- mixing matrix

K. Fujikawa and R. E. Shrock, Phys. Rev. Lett. 45, 963 (1980)

Experiment

GEMMA collaboration

A.G. Beda et al., in Particle Physics on the Eve of LHC, Ed. by A. Studenikin (World Sci., Singapore, 2009), p. 112, arXiv:0906.1926


It is possible to have For ultra-relativistic with momentum and magnetic moment in very dense matter from
A.Lobanov, A.Studenikin, PLB 2003; PLB 2004 A.Grigoriev, A.Studenikin, PLB 2005 A.Grigoriev, A.Studenikin, A.Ternov, PLB 2005

<< age of the Universe ?

recently also discussed by A.Kuznetsov, N.Mikheev, 2006

it follows that