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Stars as Laboratories for Fundamental Physics - MPP Theory Group

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440 Chapter 11<br />

b) Impact of Neutrino-Neutrino Interactions<br />

The discussion so far h<strong>as</strong> been relatively simplistic because the role of<br />

neutrino-neutrino interactions h<strong>as</strong> been ignored. During the hot-bubble<br />

ph<strong>as</strong>e the neutrino refractive index caused by other neutrinos is not necessarily<br />

negligible (Pantaleone 1995; Qian and Fuller 1995). In terms of<br />

the neutrino luminosity the number flux and thus the density of neutrinos<br />

of a given species at a radius r is given by n ν = L ν ⟨E ν ⟩ −1 (4πr 2 ) −1 .<br />

Moreover, <strong>as</strong> in the discussion in Sect. 11.4.2 one must include an average<br />

of the factor (1 − cos Θ) to account <strong>for</strong> the anisotropy of the neutrino<br />

ph<strong>as</strong>e space distribution (angle Θ between test and background<br />

neutrino). At a given distance r the neutron star (neutrino sphere<br />

radius R) subtends an angle given by sin Θ R = R/r. For a radially<br />

moving test neutrino one finds (<strong>for</strong> a more rigorous treatment see e.g.<br />

Qian and Fuller 1995)<br />

∫ 1<br />

/ ∫ 1<br />

⟨1 − cos Θ⟩ = (1 − cos Θ) d cos Θ d cos Θ<br />

cos Θ R cos Θ R<br />

[<br />

]<br />

1 −<br />

√1 − (R/r) 2 , (11.15)<br />

= 1 2<br />

which <strong>for</strong> large r approaches 1 4 (R/r)2 . There<strong>for</strong>e, the effective neutrino<br />

density n ν ⟨1 − cos Θ⟩ varies <strong>as</strong> r −4 at large distances.<br />

The electrons and positrons cause a refractive energy shift between<br />

ν e and, say, ν µ of ∆V = √ 2G F (n e − − n e +) while the effect of the<br />

neutrinos is<br />

∆V ≈ √ 2G F (n νe − n νe − n νµ + n νµ )⟨1 − cos Θ⟩<br />

√ ( 2GF ⟨1 − cos Θ⟩ Lνe<br />

≈<br />

4πr 2 ⟨E νe ⟩ − L ν e<br />

⟨E νe ⟩ − L ν µ<br />

⟨E νµ ⟩ + L )<br />

ν µ<br />

.<br />

⟨E νµ ⟩<br />

(11.16)<br />

The tau-flavored neutrino contribution h<strong>as</strong> not been included because<br />

it cancels exactly between ν τ and ν τ . The same is true <strong>for</strong> the muflavored<br />

terms be<strong>for</strong>e oscillations have taken place. For a test-neutrino<br />

of momentum p ν one finds numerically<br />

2p ν ∆V ≈ 420 eV 2 (10 km/r) 2 ⟨1 − cos Θ⟩ ×<br />

(<br />

p ν Lνe<br />

×<br />

10 51 erg s −1 ⟨E νe ⟩ − L ν e<br />

⟨E νe ⟩ − L ν µ<br />

⟨E νµ ⟩ + L )<br />

ν µ<br />

.<br />

⟨E νµ ⟩<br />

(11.17)<br />

A few seconds after bounce typical values might be ⟨E νe ⟩ = 11 MeV,<br />

⟨E νe ⟩ = 16 MeV, and ⟨E νµ ⟩ = ⟨E νµ ⟩ = 25 MeV, the luminosities can

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