Titlebook: Spatial Pattern in Plankton Communities; John H. Steele Book 1978 Springer Science+Business Media New York 1978 fields.nuclear physics.phy

ANTIC

Horizontal Dispersion and Critical Scales for Phytoplankton Patches,Planktonic organisms in the sea are subject to physical processes in addition to biological processes. It can be seen that physical effects become important in the distribution of organisms when the time scale of the process is comparable to (or smaller than) that of biological factors such as the time scale of organism reproduction.

chapel

OREX

變態(tài)

Akira Okubo are that gas giants form more readily at super-solar metallicities, although ～5% of sun-like stars have detectable companions. Lower mass stars also have planetary companions, as emphasised by the discovery of planets around Gl 876 and Gl 836, although the overall frequency of Jovian-mass gas giant

手術(shù)刀

G. E. B. Kullenbergcting that variations in the form of Ψ.(.) occur from one star-forming region to another. The strongest support for this hypothesis comes from comparing observations of dense, populous clusters, such as Orion and IC 348, against the low-density star-forming clouds in the Taurus-Auriga association. S

Magnitude

Trevor Platt are that gas giants form more readily at super-solar metallicities, although ～5% of sun-like stars have detectable companions. Lower mass stars also have planetary companions, as emphasised by the discovery of planets around Gl 876 and Gl 836, although the overall frequency of Jovian-mass gas giant

肉體

Kenneth L. Denman,David L. Mackasmperature can be estimated from the distribution of energy as a function of wavelength, and from the relative ionisation of different chemical species; individual spectral line profiles of various atoms allow us to estimate the density, gravity and gas pressure in the atmosphere; chemical compositio

ARENA

Incorporate

M. J. R. Fashamomparison with observations like density and abundance distributions, star-gas content, velocities, velocity dispersions, mass-luminosity relations and age distributions of stars. A detailed model will show, whether the initial conditions, the feedback mechanisms during the evolution or the environm

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