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Stars as Laboratories for Fundamental Physics - MPP Theory Group

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Neutrino Oscillations 301<br />

8.3.5 The Triangle and the Bathtub<br />

The most important application of resonant neutrino oscillations is the<br />

possible reduction of the solar ν e flux, an issue to be discussed more<br />

fully in Chapter 10. Here, I will use the above simple analytic results to<br />

discuss schematically the survival probability prob(ν e →ν e ) of neutrinos<br />

produced in the Sun.<br />

To this end I use an exponential profile <strong>for</strong> the electron density,<br />

n e = n c e −r/R 0<br />

, which is a re<strong>as</strong>onable first approximation with R 0 =<br />

R ⊙ /10.54 (Bahcall 1989). Then |∇ ln n e | = R0 −1 is a quantity independent<br />

of location so that there is no need to evaluate it specifically on<br />

resonance. Thus |∇ ln n e | res = 3×10 −15 eV is independent of neutrino<br />

parameters. There<strong>for</strong>e, the adiabaticity parameter is<br />

γ = 1 6 × 103 sin 2θ 0 tan 2θ 0<br />

∆m 2<br />

meV 2 MeV<br />

E ν<br />

. (8.45)<br />

An electron density at the center of n c = 1.6×10 26 cm −3 yields<br />

ξ c = 40 meV2<br />

∆m 2<br />

E ν<br />

MeV . (8.46)<br />

The quantity ξ w<strong>as</strong> defined in Eq. (8.31).<br />

It is further <strong>as</strong>sumed that all neutrinos are produced with a fixed<br />

energy by a point-like source at the solar center. They will encounter<br />

a resonance on their way out if ξ c > cos 2θ 0 . In this c<strong>as</strong>e one may<br />

calculate the “jump probability” p according to Eq. (8.42) with F from<br />

Eq. (8.43) <strong>for</strong> the exponential profile. The survival probability is then<br />

given by Eq. (8.40) with the mixing angle at the solar center<br />

cos 2θ =<br />

cos 2θ 0 − ξ c<br />

[(cos 2θ 0 − ξ c ) 2 + sin 2 . (8.47)<br />

2θ 0 ]<br />

1/2<br />

If ξ c < cos 2θ 0 no resonance is encountered; the vacuum parameters<br />

dominate throughout the Sun. In this c<strong>as</strong>e one may use p = 0.<br />

In the framework of these approximations it is straight<strong>for</strong>ward to<br />

evaluate prob(ν e →ν e ) <strong>as</strong> a function of ∆m 2 and sin 2 2θ 0 . In Fig. 8.9<br />

contours <strong>for</strong> the survival probability are shown <strong>for</strong> E ν = 1 MeV. Because<br />

the energy always appears in the combination ∆m 2 /2E ν one may<br />

obtain an analogous plot <strong>for</strong> other energies by an appropriate vertical<br />

shift. This kind of plot represents the well-known MSW triangle. The<br />

d<strong>as</strong>hed line marks the condition γ = 1 and thus divides the parameter<br />

plane into a region where the oscillations are adiabatic and one

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