Introduction to Practical Astronomy; Designed as a Supplement to Olmsted's Astronomy
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Home > Art, Film & Photography > Introduction to Practical Astronomy; Designed as a Supplement to Olmsted's Astronomy: Containing Special Rules for the Adjustment and Use of Astronomical Instruments, Together with the Calculation of Eclipses and Occultations, and the
Introduction to Practical Astronomy; Designed as a Supplement to Olmsted's Astronomy: Containing Special Rules for the Adjustment and Use of Astronomical Instruments, Together with the Calculation of Eclipses and Occultations, and the

Introduction to Practical Astronomy; Designed as a Supplement to Olmsted's Astronomy: Containing Special Rules for the Adjustment and Use of Astronomical Instruments, Together with the Calculation of Eclipses and Occultations, and the


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About the Book

This historic book may have numerous typos and missing text. Purchasers can download a free scanned copy of the original book (without typos) from the publisher. Not indexed. Not illustrated. 1841 edition. Excerpt: ...poles on a globe or in fig. 18, to coincide with the horizon, and turning a colure from the zenith a very little over to the east. The error of inclination will then be expressed, of course, by the small arc of the primS vertical intercepted, which represent by b = error of inclination; + when, measured on the prime vertical, it inclines towards the east, --when towards the west; and expressed in seconds of time. The inclination being = b at the zenith, decreases towards the Any great circle, as the horizon, may be supposed to be divided into hours, minutes, and seconds, instead of degrees, minutes, and seconds. horizon either way, and the distance between the circles at any point is (Cor. 2, Note, Art. 63.) b x sin altitude =b x cos zen. dist. = b cos (p--i); and a star arriving at the transit plane at the time t, will cross it, and (allowing for its rate of motion as before) arrive on the meridian at the time t+b cos (p--S) sec 8. Now cos (p--S) does not change its sign when p--S becomes negative at the north of the meridian; and the reason is easily seen, --for the transit plane is in this case wholly to the east of the meridian from the north to the south point, or when b is negative wholly to the west. 71. Lastly, the telescope may not move in the meridian, but in a small circle parallel to the meridian, and every where a certain number of seconds (c) east of it. This will be the case if the optical axis, instead of being perpendicular to the horizontal axis, is inclined towards the eastern pivot a little. Let then c = the error of collimation; + when eastward, --when westward of the meridian, and reckoned in seconds of time. The distance from this circle to the meridian being constant at all points, a star arriving at the transit plane at the


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Product Details
  • ISBN-13: 9781130432862
  • Publisher: Rarebooksclub.com
  • Publisher Imprint: Rarebooksclub.com
  • Height: 246 mm
  • No of Pages: 46
  • Spine Width: 3 mm
  • Weight: 100 gr
  • ISBN-10: 1130432866
  • Publisher Date: 01 Jun 2012
  • Binding: Paperback
  • Language: English
  • Returnable: N
  • Sub Title: Containing Special Rules for the Adjustment and Use of Astronomical Instruments, Together with the Calculation of Eclipses and Occultations, and the
  • Width: 189 mm


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Introduction to Practical Astronomy; Designed as a Supplement to Olmsted's Astronomy: Containing Special Rules for the Adjustment and Use of Astronomical Instruments, Together with the Calculation of Eclipses and Occultations, and the
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