Complex fluids : proceedings of the XII Sitges Conference, by Luis Garrido

By Luis Garrido

This set of survey talks provided to graduate scholars serves as an intensive exposition of the topic. The research of complicated fluids (with inner constitution) is necessary for theoretical reasons but in addition, and perhaps even extra so, for utilized study. The reader will locate papers on colloid combos, the constitution of DNA mesophases, ferrofluids, chain dynamics, liquid crystals, computing device simulations of macromolecules, fluidization, emulsions, relaxations and lots of different comparable issues.

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N. Bahcall (World Scientific, Singapore, 1995). 22. A. Cumming and W. C. Haxton, Phys. Rev. Lett. 77, 4286 (1996). 23. N. Hata and P. Langacker, Phys. Rev. D 56, 6107 (1997). 24. K. M. Heeger and R. G. H. Robertson, Phys. Rev. Lett. 77, 3720 (1996). 25. For a proper (wave packet) derivation see M. Nauenberg, submitted to Phys. Lett. B. 26. S. P. Mikheyev and A. Smirnov, Sov. J. Nucl. Phys. 42, 913 (1985); L. Wolfenstein, Phys. Rev. D 17, 2369 (1979). 27. H. Bethe, Phys. Rev. Lett. 56, 1305 (1986).

Phys. Lett. B 285, 376 (1992). 5. Y. Suzuki, Nucl. Phys. B 38, 54 (1995). 6. Y. Suzuki, talk presented at Neutrino ’98 (Takayama, Japan, June, 1998). 7. T. Kajita, talk presented at Neutrino ’98 (Takayama, Japan, June, 1998). 8. J. N. Bahcall, S. Basu, and M. H. Pinsonneault, Phys. Lett. B 433, 1 (1998). 9. A. S. Brun, S. Turck-Chieze, and P. Morel, Ap. J. 506, 913 (1998) and private communication; S. Turck-Chieze and I. Lopez, Ap. J. 408, 347 (1993). 10. This section taken from W. C. Haxton, nucl-th/9901037.

Unfortunately the upper bounds imposed on the neutrino mass are quite model dependent, ranging over (1-25) keV. The supernova cooling argument can also be repeated for axions. 01 eV (below this mass they are too weakly coupled to be produced on the timescale of supernova cooling). It is interesting that the supernova and red giant cooling limit on axions nearly meet: a small window may still exist around a few eV if the axion has no coupling to electrons. 4 Supernovae, Supernova Neutrinos, and Nucleosynthesis Consider a massive star, in excess of 10 solar masses, burning the hydrogen in its core under the conditions of hydrostatic equilibrium.

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