An Introduction to Astronomy Designed As a Textbook for the Use of Students in
An Introduction to Astronomy Designed As a Textbook for the Use of Students in
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In our eReader you can find the full English version of the book. Read An Introduction to Astronomy Designed As a Textbook for the Use of Students in Online - link to read the book on full screen. Our eReader also allows you to upload and read Pdf, Txt, ePub and fb2 books. In the Mini eReder on the page below you can quickly view all pages of the book - Read Book An Introduction to Astronomy Designed As a Textbook for the Use of Students in
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This line lies in various positions, and is of various lengths, according to the place of M. It is convenient to reduce it to two ele- 104: EVECTION.
ments called the radial and the tangential disturbing forces. Draw MO tangent to the orbit, and EM joining the earth and moon ; then, MET may be resolved into the radial force MP, increasing or diminishing the moon's gravity to the earth, and the tangential force MO, which increases or diminishes the velocity of the moon. In the figure, the positi...on of MH is such, that MP increases the gravity, and MO accelerates.
Near the quadratures, MP acts toward E ; and near the syzygies, it acts away from E. MO accelerates on the quad- rants DA and BC, and retards on AB and CD. , 185. Equations for correcting the moon's place. The moon's path being elliptical, and its motion being subject to several disturbances, its true longitude for a given time can not be found, except by applying various corrections.
186. The equation of the center. First suppose the moon to revolve uniformly in a circular orbit, and then, as in the case of the sun (Art.
What to read after An Introduction to Astronomy Designed As a Textbook for the Use of Students in?
You can find similar books in the "Read Also" column, or choose other free books by Denison Olmsted to read onlineMoreLess
To quickly assess the difficulty of the text, read a short excerpt:
This line lies in various positions, and is of various lengths, according to the place of M. It is convenient to reduce it to two ele- 104: EVECTION.
ments called the radial and the tangential disturbing forces. Draw MO tangent to the orbit, and EM joining the earth and moon ; then, MET may be resolved into the radial force MP, increasing or diminishing the moon's gravity to the earth, and the tangential force MO, which increases or diminishes the velocity of the moon. In the figure, the positi...on of MH is such, that MP increases the gravity, and MO accelerates.
Near the quadratures, MP acts toward E ; and near the syzygies, it acts away from E. MO accelerates on the quad- rants DA and BC, and retards on AB and CD. , 185. Equations for correcting the moon's place. The moon's path being elliptical, and its motion being subject to several disturbances, its true longitude for a given time can not be found, except by applying various corrections.
186. The equation of the center. First suppose the moon to revolve uniformly in a circular orbit, and then, as in the case of the sun (Art.
What to read after An Introduction to Astronomy Designed As a Textbook for the Use of Students in?
You can find similar books in the "Read Also" column, or choose other free books by Denison Olmsted to read onlineMoreLess
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