Contributions to solar physicsMacmillan and Company, 1874 - 676 pages |
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Common terms and phrases
absorption angle Ångström appearance astronomers Balfour Stewart bright lines brilliant Carrington centre CHAP chromosphere cloud colour Comptes Rendus continuous spectrum corona cyclone dark lines disc dispersion distance edge energy envelope evidence F line fact faculæ Father Secchi Faye Fraunhofer lines G. C. Lewis gaseous give glass heat Herschel Huggins hydrogen hydrogen lines incandescent instrument j'ai Janssen Kirchhoff les raies less light lignes limb Lockyer luminous magnesium masses matter ment method moon motion nences NOTE observed paper penumbra period phenomena photographs photosphere polariscope polarization poles portion position present prism Professor prominences protuberances question radiation rays red flames referred refraction refrangible region remark Respighi rotation Royal Society seen side slit sodium solar atmosphere solar spectrum spectra spectroscope sphere spots stratum sun-spots sun's atmosphere sun's surface taches telescope temperature theory tion total eclipse umbra vapour visible willow-leaves
Popular passages
Page iii - CONTRIBUTIONS TO SOLAR PHYSICS, i. A POPULAR ACCOUNT OF INQUIRIES INTO THE PHYSICAL CONSTITUTION OF THE SUN, WITH SPECIAL REFERENCE TO RECENT SPECTROSCOPIC RESEARCHES; II. COMMUNICATIONS TO THE ROYAL SOCIETY OF LONDON, AND THE FRENCH ACADEMY OF SCIENCES, WITH NOTES. BY J. NORMAN LOCKYER, FRS
Page 431 - May not the spectroscope afford us evidence of the existence of the ' red-flames' which total eclipses have revealed to us in the sun's atmosphere, although they escape all other methods of observation at other times ? and if so, may we not learn something from this of the recent outburst of the star in Corona
Page 223 - in eclipses. Here one is reminded, by the fleecy, infinitely delicate cloud-films, of an English hedge-row with luxuriant elms ; here of a densely intertwined tropical forest, the intimately interwoven branches threading in all directions, the prominences generally expanding as they mount upwards, and changing slowly, indeed almost imperceptibly. It does not at all follow that the largest prominences
Page 387 - crowded down, as it were, along the solar surface ;.later it rose almost pyramidally 50,000 miles in height; then its summit was drawn out into long filaments and threads which were most curiously rolled backwards and downwards, like the volutes of an Ionic capital; and finally it faded away, and by 2.30 had vanished like the other.
Page 147 - narrow pencil of light, four primary divisions of the prismatic spectrum may be seen with a degree of distinctness that I believe has not been described nor observed before. " If a beam of daylight be admitted into a dark room by a crevice
Page 557 - the sun's edge would be greatly reduced in intensity by the dispersion of the prisms, while the bright lines of the prominences, if such be present, would remain but little diminished in brilliancy. This principle has been carried out by various forms of prismatic apparatus, and also by other contrivances, but hitherto without success.
Page 147 - of an inch broad, and received by the eye, at the distance of ten or twelve feet, through a prism of flint glass free from veins, held near the eye, the beam is seen to be separated into the four following colours only : red, yellowish-green, blue, and violet ; in the proportions represented in Fig.
Page 147 - between red and green, in a certain position of the prism, is perfectly distinct ; so also are D and E, the two limits of violet ; but c, the limit of green and blue, is not so clearly marked as the rest : and there are also, on each side of this limit, other distinct dark lines, f and
Page 513 - that at the lower surface of the chromosphere itself the pressure is very far below the pressure of the earth's atmosphere. The bulbous appearance of the F line before referred to may be taken to indicate violent convective currents or local generations of heat, the condition of the chromosphere being doubtless one of the most intense action.
Page 23 - These flakes, be they what they may, and whatever may be said about the dashing of meteoric stones into the sun's atmosphere, &c., are evidently the immediate sources of the solar light and heat, by whatever mechanism or whatever processes they may be