A New Solution of the Solar Neutrino Flux

We report a new solution to explain the observed deficit of the solar neutrino flux by Homestake, Kamiokande II and III, GALLEX and SAGE experiments. We use the matter mixing and the helicity oscillation in the twisting magnetic fields in the sun. Our model predicts the short (seasonal) and long (11 years) time variations of the solar neutrino flux. Three kinds of data observed by Homestake, Kamiokande, GALLEX and SAGE detectors are reproduced well if the mixing angle and the squared mass difference are in the small area around $\sin^2 2\theta \simeq 0.01$ and $\Delta m^2\simeq 1.3\times 10^{-8}{\rm eV}^2$.Comment: 13 pages and 4 figures (not included), in phyzzx, OU-HET-19

Supersymmetry of M-Branes at Angles

We determine the possible fractions of supersymmetry preserved by two intersecting M-5-branes. These include the fractions 3/32 and 5/32 which have not occurred previously in intersecting brane configurations. Both occur in non-orthogonal pointlike intersections of M-5-branes but 5/32 supersymmetry is possible only for specific fixed angles.Comment: 11 pages, Late

CO(J=6-5) Observations of the Quasar SDSS1044-0125 at z = 5.8

We present a result of the quasar CO(J=6-5) observations of SDSSp J104433.04-012502.2 at z = 5.8. Ten-days observations with the Nobeyama Millimeter Array yielded an rms noise level of ~ 2.1 mJy/beam in a frequency range from 101.28 GHz to 101.99 GHz at a velocity resolution of 120 km/s. No significant clear emission line was detected in the observed field and frequency range. Three sigma upper limit on the CO(J=6-5) luminosity of the object is 2.8 x 10^10 K km/s pc^2, corresponding to a molecular gas mass of 1.2 x 10^11 Solar Mass, if a conversion factor of 4.5 Solar Mass /(K km/s pc^2) is adopted. The obtained upper limit on CO luminosity is slightly smaller than those observed in quasars at z=4-5 toward which CO emissions are detected.Comment: 4 pages, 3 figures, LaTeX2e, to appear in Publication of Astronomical Society of Japan (PASJ), Postscript file available at ftp://ftp.kusastro.kyoto-u.ac.jp/pub/iwata/preprint/sdss1044/sdss.ps.g