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 Introduction General Principles 1 Bases 5 Triangulation 10 Traverses 34 Subtense Methods and Tacheometry 51 PlaneTabling 56 Survey under Active Service Conditions 63 Levelling 74
 5 205 10 206 51 211 57 212 89 213 92 214 12 215 204 220

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Side 122 - Each planet moves in its orbit at such a speed that a line joining it to the sun sweeps over equal areas in equal times. 3. The square of the time...
Side 37 - All the interior angles of any rectilineal figure, together with four right angles, are equal to twice as many right angles as the figure has sides.
Side 129 - The mean solar day is divided into 24 hours, each hour into 60 minutes, and each minute into 60 seconds.
Side 129 - An apparent solar day is the interval between two successive transits of the sun's centre across the meridian of any place.
Side 122 - As the planet moves round the sun, its radius-vector (or the line joining it to the sun) passes over equal areas in equal times. To explain these laws, let PA (Fig. 20) be the ellipse in which the planet moves. Then the sun will not be in the cenFio.
Side 129 - A SIDEREAL DAY is the interval of time between two successive upper transits of the vernal equinox over the same meridian.
Side 204 - ... is equal to the probable error of a single observation divided by the square root of the number of observations. The probable error of the mean, hence, decreases as Vw increases.
Side 124 - The parsec is the distance at which a star would have a parallax of one second of arc.
Side 125 - The longitude of a place is the arc of the equator intercepted between the meridian of that place and some assumed meridian to which all others are referred.
Side 56 - triangle of error " is inside the triangle formed by the three fixed points, the position is inside the triangle of error ; and if outside, outside.