Reexamining nonstandard interaction effects on supernova neutrino flavor oscillations

Details Reexamining nonstandard interaction effects on supernova neutrino flavor oscillations Reexamining nonstandard interaction effects on supernova neutrino flavor oscillations

2002-02-27

arxiv.org/abs/hep-ph/0202269v3

Phys.Rev.D66:013009,2002

Physics

High Energy Physics

High Energy Physics - Phenomenology

Text clarified, one figure added. To appear in PRD

Scientific paper

10.1103/PhysRevD.66.013009

Several extensions of the standard electroweak model allow new four-fermion interactions (nu_a nu_b * ff) with strength eps_ab*G_F, where (a,b) are flavor indices. We revisit their effects on flavor oscillations of massive (anti)neutrinos in supernovae, in order to achieve, in the region above the protoneutron star, an analytical treatment valid for generic values of the neutrino mixing angles (omega,phi,psi)=(theta_12,theta_13,theta_23). Assuming that eps_ab<<1, we find that the leading effects on the flavor transitions occurring at high (H) and low (L) density along the supernova matter profile can be simply embedded through the replacements phi-->phi+eps_H and omega-->omega+eps_L, respectively, where eps_H and eps_L are specific linear combinations of the eps_ab's. Similar replacements hold for eventual oscillations in the Earth matter. From a phenomenological point of view, the most relevant consequence is a possible uncontrolled bias (phi-->phi+eps_H) in the value of the mixing angle phi inferred by inversion of supernova neutrino data. Such a drawback, however, does not preclude the discrimination of the neutrino mass spectrum hierarchy (direct or inverse) through supernova neutrino oscillations.

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