Solar neutrino problem accounting for self-consistent magnetohydrodynamics solution for solar magnetic fields

The analysis of the resonant spin-�avour (RSF) solutions to the solar neutrino problem in the frame- work of simplest analytic solutions to the solar magnetohydrodynamics (MHD) equations is presented. We performed the globalt of the recent solar neutrino data, including event rates as well as zenith an- gle distributions and recoil electron spectra induced by solar neutrino interactions in Superkamiokande. We compare quantitatively our simplest MHD-RSFt with vacuum oscillation (VAC) and MSW-type (SMA, LMA and LOW) solutions to the solar neutrino problem using a common well-calibrated theo- retical calculation andt procedure andnd MHD-RSFt to be somewhat better than those obtained for the favored neutrino oscillation solutions. We made the predictions for future experiments (e.g., SNO) to disentangle the MHD-RSF scenario from other scenarios. Œ¥I ´¨§³ ·¥§µ´ ´¸´µ° ¸¶¨´- ·µ³ E´µ° ±µ´¢¥·¸¨¨ ´¥°E·¨´µ ¤²O ·¥I¥´¨O ¶·µi²¥³O ¸µ²´¥I- ´OI ´¥°E·¨´µ ¶¥·¥¸³µE·¥´ ¢ · ³± I ´ ²¨E¨I¥¸±µ£µ ·¥I¥´¨O E· ¢´¥´¨° ¸µ²´¥I´µ° ³ £´¨E´µ° £¨¤·µ¤¨´ ³¨±¨ (Œƒ"). "I¨EO¢ O ³ E¥³ E¨I¥¸±EO ¸ ³µ¸µ£² ¸µ¢ ´´µ¸EO E· ¢´¥´¨° ¨ ¸EÐ¥¸E¢EO- Ш¥ E¨§¨I¥¸±¨¥ µ£· ´¨I¥´¨O, ³O ¶·¥¤² £ ¥³ ¶·µ¸E¥°IEO ¸I¥³E ±µ´¢¥·¸¨¨ ´¥°E·¨´µ ¢ · ³± I ·¥ ²¨¸E¨I´OI ¸E E¨I¥¸±¨I ·¥I¥´¨° Œƒ"-E· ¢´¥´¨°. ŒO ¶·µ¢¥²¨ ±µ²¨I¥¸E¢¥´´µ¥ ¸· ¢´¥´¨¥ ¶µ- ²EI¥´´OI ·¥§E²OE Eµ¢ ¸ ¤·E£¨³¨ ³¥I ´¨§³ ³¨, E ±¨³¨ ± ± ¢ ±EE³´O¥ µ¸I¨²²OI¨¨ ¨ Œ'‚-OEE¥±E, ¨¸¶µ²O§EO ¥¤¨´EO ¸I¥³E ¢OI¨¸²¥´¨°, ¨ ¶µ± § ²¨, IEµ ´ I ¸I¥´ ·¨° ¤ ¥E ²EII¥¥ ¸µ£² ¸¨¥ ¸ O±¸- ¶¥·¨³¥´E ²O´O³¨ ¤ ´´O³¨. ‚ · iµE¥ ¸¤¥² ´O ¶·¥¤¸± § ´¨O ¤²O ´¥°E·¨´´µ£µ O±¸¶¥·¨³¥´E ¢ ' ¤- iO·¨.