The Principles of Hydrostatics: Designed for the Use of Students in the University
J. Smith, 1820 - Hydrostatics - 151 pages
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according altitude angle appears atmosphere attraction axis beginning body called cause circle comes comet compared computed conjunction consequently considered continue declination density describe determined diameter difference direction discovered distance draw earth eclipse effect equal equator experiment fall fixed stars fluid force given gives glass greater greatest happen heat hence horizon hour inches increase interval it's Jupiter latitude length less light longitude magnitude matter mean measured mercury meridian method moon moon's motion move nearly node observed opposition orbit parallax parallel passes periodic perpendicular planet pole position pressure PROP proportion quantity represent resistance respect right ascension ring rise satellite Saturn seen shadow side specific gravity star sun's supposed surface Tables tion Trig true tube varies velocity Venus vessel weight whole wind
Page 284 - Observer' at a salary of 100£ per annum, his duty being 'forthwith to apply himself with the most exact care and diligence to the rectifying the tables of the motions of the heavens and the places of the fixed stars, so as to find out the so much desired longitude of places for the perfecting the art of navigation.
Page 233 - ... and therefore there is a greater probability of seeing a lunar than a solar eclipse. Since the moon is as long above the horizon as below, every spectator may expect to see half the number of lunar eclipses which happen.
Page 267 - ... in diameter. The star is perfectly in the centre, and the atmosphere is so diluted, faint, and equal throughout, that there can be no surmise of its consisting of stars ; nor can there be a doubt of the evident connection between the atmosphere and the star. Another star not much less in brightness, and in the same field with the above, was perfectly free from any such appearance.
Page 208 - If the plane of the moon's orbit coincided with the plane of the ecliptic, there would be an eclipse at every...
Page 150 - ... it had a degree of brightness about as strong as that with which such a coal would be seen to glow in faint daylight.
Page 261 - ... sixteenth century Kepler discovered a new star near the heel of the right foot of Serpentarius, ' so bright and sparkling that it exceeded any thing he had ever seen before.
Page 208 - An eclipse is a partial, or total privation of the light of the sun or moon. An eclipse of the sun is caused by the interposition of the moon between the earth and the sun, and consequently must happen when the inoon is in conjunction with the sun, or at the new moon.
Page 230 - ... the sun was just coming out, a long and very narrow streak of a dusky but strong red light seemed to colour the dark edge of the moon...
Page 227 - ... seconds of time ; then part of the Sun's disc appeared all of a sudden, as bright as Venus was ever seen in the night ; nay, brighter ; and in that very instant gave a light and shadow to things as strong as the Moon uses to dod.
Page 218 - ... red color. An eclipse of the moon arising from a real deprivation of light, must appear to begin at the same instant of time to every place on that hemisphere of the Earth, which is next the moon. Hence, it affords a ready method of finding the longitudes of places upon the Earth's surface.