Physics – High Energy Physics – High Energy Physics - Phenomenology
Scientific paper
2003-09-08
Phys.Atom.Nucl. 67 (2004) 1151; Yad.Fiz. 67 (2004) 1176-1178
Physics
High Energy Physics
High Energy Physics - Phenomenology
Based on talk given at NANP'03, JINR Dubna, Russia, June 2003. To be published in "Physics of Atomic Nuclie"
Scientific paper
10.1134/1.1772451
We use the recent KamLAND observations to predict the solar antineutrino spectrum at some confidence limits. We find that a scaling of the antineutrino probability with respect to the magnetic field profile --in the sense that the same probability function can be reproduced by any profile with a suitable peak field value-- can be utilised to obtain a general shape of the solar antineutrino spectrum. This scaling and the upper bound on the solar antineutrino event rate, that can be derived from the data, lead to: 1) an upper bound on the solar antineutrino flux, 2) the prediction of their energy spectrum, as the normalisation of the spectrum can be obtained from the total number of antineutrino events recorded in the experiment. We get $\phi_{\bar\nu}<3.8\times 10^{-3}\phi(^8B)$ or $\phi_{\bar\nu} <5.5\times 10^{-3}\phi(^8B)$ at 95% CL, assuming Gaussian or Poissonian statistics, respectively. And for 90% CL these become $\phi_{\bar\nu}<3.4 \times 10^{-3}\phi(^8B)$ and $\phi_{\bar\nu}<4.9\times 10^{-3}\phi(^8B)$. It shows an improvement by a factor of 3-5 with respect to existing bounds. These limits are quite general and independent of the detailed structure of the magnetic field in the solar interior.
Chauhan Bhag C.
Pulido Joao
Torrente-Lujan Emilio
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