Appendices A and B are only available in electronic form at http://www.edpsciences.org

.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.

Istituto di Fisica dello Spazio Interplanetario, corso Fiume 4, 10133 Torino, Italy.

.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.

... $\delta t = 20~$ s

Using the values: $f_{\nu_{\rm e}} = 1/5$ and $T_{\nu_x}=1.3 T_{\bar \nu_{\rm e}}$ , the limits weakens of a factor <2.

.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.

... scenarios

NC data are not affected by oscillations. However, the limits from IBD data stay almost the same even assuming that MSW oscillations are completely absent. In fact, on accounting for vacuum oscillations we get $P_{\rm\bar{e}\bar{e}}=1-\sin^2 2\theta_{12}/2 \sim 0.6$ in all scenarios; this is practically the same value implied by MSW oscillations in the scenarios NH and $\rm IH_{\rm non\ ad.}$ , $P_{\rm\bar{e}\bar{e}}=\cos^2\theta_{12}\sim 0.7$ .

.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.