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acid amount aortic pressure appearance arithmetical progression Astr aurora aurora spectrum Australian band bile Binary Stars blood pressure bright lines Cambridge carbon band carbon fluting chemical chloric acid College colour comet cometary compound cool carbon Copeland corresponding curvature curve cylinder decomposition dorsal effect electric energy equation estuary excitation experiments F.R.S. Received fibrinogen ganglion gram Group hydrochloric acid hydrogen chloride hydrogen lines increase investigation iodine iron June liquid London lumbar lumbar vertebra magnesium magnetic manganese manganese absorption maximum measured meteoric meteorites mixture nebulae nerve nitrogen observations Observatory obtained paper perihelion perihelion passage plate potassium chlorate potassium iodide present Price probably produced Professor proportion quantity reaction refrangible rise Royal Society salt seen solution spectra spectroscopic starch substance surface swarm Table temperature thickness thiosulphate tion training walls Transactions tube variation velocity vertebra vibration Vogel wave-length whilst zinc
Page 398 - The tub contained 64-i pounds of butter, which lost 3| pounds in weight up to July 6, 1910. The weight of the container was the same at the end of the experiment as at the beginning. It was thoroughly soaked before the butter was packed in it and during the latter part of the period of observation it was wet in the storage room on account of melting ice on the floor. Of the five prints kept in cold storage and separately exposed (3) the loss ranged from 9.9 grams to 14.5 grams...
Page 14 - This is true of the swarm from which the solar system was formed, when it extended beyond the orbit of the planet Neptune. When the swarm was very widely dispersed, the arrangement of density and of velocity of agitation of the meteorites was that of an isothermaladiabatic sphere. Later in its history, when the swarm had contracted, it was probably throughout in convective equilibrium. . . The actual mean velocity of the meteorites is determinable in a swarm of given mass, when expanded to a given...
Page 128 - ... expressed as the sum of two terms, one simply as the velocity, and the other as the square of the velocity.
Page 135 - Two variable organs are said to be co-related when the variation of the one is accompanied on the average by more or less variation of the other, and in the same direction. Thus the length of the arm is said to be co-related with that of the leg, because a person with a long arm has usually a long leg, and conversely.
Page 15 - ... to present a fair approximation to the truth in the earlier stages of the evolution of the system. But later the majority of the meteors must have been absorbed by the central sun and its attendant planets, and amongst the meteors which remain free the relative motion of agitation must have been largely diminished. These free meteorites — the dust and refuse of the system — probably move in...
Page 135 - It is easy to see that co-relation must be the consequence of the variations of the two organs being partly due to common causes. If they were wholly due to common causes, the co-relation would be perfect, as is approximately the case with the symmetrically disposed parts of the body.
Page 200 - It is more than possible, I think, that the cometary spectrum, therefore, is not so simple as it has been supposed to be, and that the evidence in favour of mixed vapours is not to be neglected.
Page 56 - ... Royal Medal has been awarded to Professor Osborne Reynolds for his investigations in mathematical and experimental physics, and on the application of scientific theory to engineering. Professor Reynolds was among the first to refer the repulsion exhibited in that remarkable instrument of Mr. Crookes's, the radiometer, to a change in the molecular impact of the rarefied gas consequent upon the slight change of temperature of the...
Page 188 - The less refrangible line is much stronger, and a faint luminosity can be traced from it to a little beyond the second line 3870. There can be, therefore, no doubt that these lines represent the brightest end of the ultra-violet group which appears under certain circumstances in the spectra of the compounds of carbon. Professors Liveing and Dewar have found for the strong line at the beginning of this group the wave-length 3882-7, and for the second line 3870-5.