14. These calculations were performed with NH, absorption coefficients given by B. A. Thompson, P. Harteck, and R. R. Reeves, Jr. [J. Geophys. Res. 68, 6431 (1963)]; H2S absorption coefficients given by J. O. Sullivan and A. C. Holland [NASA Contractor Rep. 371, 150 (1966)]; and He scattering cross sections from A. Dalgarno and D. A. Williams [Astrophys. J. 136, 690 (1962)]. The NH, and H2S data were degraded to a resolution of 70 A to correspond to the observational data. 15. T. P. Stecher,

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... . Astrophys. 28, 788 (1965). 16. For reasonable NH., abundances, the calculated albedo increases rapidly below 2000 A. This increase continues with decreasing wavelength down to about 1450 A. Below this wavelength the albedo again decreases. 17. L. Trafton, Astrophys. J. 140, 1340 (1964). We thank R. Danielson for calling our attention to the efficacy of this approach in interpreting the atmospheric structure. Danielson and Savage (in preparation) have carried this type of analysis much further, but their purposes differ somewhat from ours. 18. An isothermal stratosphere compatible with Trafton's greenhouse model must have a temperature below 95?K. We have assumed an effective temperature of 105?K for the upper atmosphere of Jupiter [D. Taylor, Jcar Ls 4, 362 (1965)] and derived an iso-14. These calculations were performed with NH, absorption coefficients given by B. A. Thompson, P. Harteck, and R. R. Reeves, Jr. [J. Geophys. Res. 68, 6431 (1963)]; H2S absorption coefficients given by J. O. Sullivan and A. C. Holland [NASA Contractor Rep. 371, 150 (1966)]; and He scattering cross sections from A. Dalgarno and D. A. Williams [Astrophys. J. 136, 690 (1962)]. The NH, and H2S data were degraded to a resolution of 70 A to correspond to the observational data. 15. T. P. Stecher, Ann. Astrophys. 28, 788 (1965). 16. For reasonable NH., abundances, the calculated albedo increases rapidly below 2000 A. This increase continues with decreasing wavelength down to about 1450 A. Below this wavelength the albedo again decreases. 17. L. Trafton, Astrophys. J. 140, 1340 (1964). We thank R. Danielson for calling our attention to the efficacy of this approach in interpreting the atmospheric structure. Danielson and Savage (in preparation) have carried this type of analysis much further, but their purposes differ somewhat from ours. 18. An isothermal stratosphere compatible with Trafton's greenhouse model must have a temperature below 95?K. We have assumed an effective temperature of 105?K for the upper atmosphere of Jupiter [D. Taylor, Jcar Ls 4, 362 (1965)] and derived an iso- Abstract. In a study of the rate of production of four species of planktonic Foraminifera in the region of the California Current it was found that their life spans are of the order of 1 month. Reproduction seems to take place mainly in the upper hundred meters. Results are in contrast to previous evidence presented in favor of yearly life cycles and maturing at great depth in other species of Abstract. In a study of the rate of production of four species of planktonic Foraminifera in the region of the California Current it was found that their life spans are of the order of 1 month. Reproduction seems to take place mainly in the upper hundred meters. Results are in contrast to previous evidence presented in favor of yearly life cycles and maturing at great depth in other species of