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Stars as Laboratories for Fundamental Physics - MPP Theory Group

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Miscellaneous Exotica 555<br />

A violation of the equivalence principle could also manifest itself by<br />

a relative shift of the energies of different neutrino flavors in a gravitational<br />

field. For a given momentum p the matrix of energies in flavor<br />

space (relativistic limit) is E = p + M 2 /2p + 2pϕ(r)(1 + F ) where M 2<br />

is the squared matrix of neutrino m<strong>as</strong>ses, ϕ(r) is the Newtonian gravitational<br />

potential, and F is a matrix of dimensionless constants which<br />

parametrize the violation of the equivalence principle; in general relativity<br />

F = 0. A nontrivial matrix F can lead to neutrino oscillations in<br />

analogy to the standard vacuum oscillations which are caused by the<br />

matrix M 2 (G<strong>as</strong>perini 1988, 1989; Halprin and Leung 1991; Pantaleone,<br />

Halprin, and Leung 1993; Iida, Minakata, and Y<strong>as</strong>uda 1993; Minakata<br />

and Nunokawa 1995; Bahcall, Kr<strong>as</strong>tev, and Leung 1995). Values <strong>for</strong><br />

F ij in the general 10 −14 −10 −17 range could account <strong>for</strong> the solar neutrino<br />

problem and perhaps could be probed with future long-b<strong>as</strong>eline<br />

oscillation experiments.<br />

15.4 Photon M<strong>as</strong>s and Charge<br />

Even though in cl<strong>as</strong>sical electrodynamics gauge invariance implies that<br />

photons must be m<strong>as</strong>sless, quantum electrodynamics (QED) can be<br />

<strong>for</strong>mulated consistently with the inclusion of a photon m<strong>as</strong>s, and the<br />

limit m γ → 0 takes the modified theory smoothly over to m<strong>as</strong>sless QED<br />

(Stückelberg 1941). There<strong>for</strong>e, the possibility of a small photon m<strong>as</strong>s<br />

cannot be excluded theoretically; limits must be set by laboratory and<br />

<strong>as</strong>trophysical methods. A still up-to-date review of the laboratory limits<br />

w<strong>as</strong> given by Goldhaber and Nieto (1971); the best is m γ ∼ < 10 −14 eV<br />

from a test of Coulomb’s law (a photon m<strong>as</strong>s would modify the inversesquare<br />

behavior). More recent experiments worked at low temperature<br />

(Ryan, Accetta, and Austin 1985; Chernikov et al. 1992); the resulting<br />

limits on m γ are relatively weak, however.<br />

An <strong>as</strong>trophysical limit may be set by the absence of an anomalous<br />

dispersion of photon signals from distant sources, notably the pulsed<br />

signal from radiopulsars. This method is limited by the presence of the<br />

ionized interstellar medium. It causes a dispersion relation <strong>for</strong> photons<br />

which mimics the effect of a photon m<strong>as</strong>s m γ = ω P where the pl<strong>as</strong>ma<br />

frequency is given by ω 2 P = 4παn e /m e . With a typical electron density<br />

n e of order 0.1 cm −3 the photon pl<strong>as</strong>ma m<strong>as</strong>s is of order 10 −11 eV so<br />

that a vacuum m<strong>as</strong>s much smaller than this value cannot be probed.<br />

In Sect. 13.3.3 a limit on a hypothetical ν e charge w<strong>as</strong> derived from<br />

the absence of a dispersion of the SN 1987A neutrino pulse. The path of

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