An Elementary Treatise on the Lunar Theory: With a Brief Sketch of the History of the Problem Up to the Time of NewtonMacmillan, 1859 - 119 σελίδες |
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Σελίδα vi
... referred , or again , in the same system , by choosing different quantities for independent variables . D'Alembert and Clairaut chose for coordinates the pro- jection of the radius vector on the plane of the ecliptic and the longitude ...
... referred , or again , in the same system , by choosing different quantities for independent variables . D'Alembert and Clairaut chose for coordinates the pro- jection of the radius vector on the plane of the ecliptic and the longitude ...
Σελίδα 10
... referred to its focus , the eccentricity being e , the semi - latus rectum h2 μ and the angle made by the apse line with the prime radius a . In the relative motion of the moon , or in that of the sun about the earth , the orbit would ...
... referred to its focus , the eccentricity being e , the semi - latus rectum h2 μ and the angle made by the apse line with the prime radius a . In the relative motion of the moon , or in that of the sun about the earth , the orbit would ...
Σελίδα 13
... referred . The plane which passes through the earth's centre and the direction of the sun's motion at any instant is called the true ecliptic ; and , as a first rough result of calculation , ob- tained on supposition of the sun and ...
... referred . The plane which passes through the earth's centre and the direction of the sun's motion at any instant is called the true ecliptic ; and , as a first rough result of calculation , ob- tained on supposition of the sun and ...
Σελίδα 34
... referred to , arrive at the result - - 0 = pt + & + 2e sin ( pt + e − a ) + že2 sin 2 ( pt + e − a ) + . which is correct only to the first order , since we have re- jected some terms of the second order by neglecting the disturbing ...
... referred to , arrive at the result - - 0 = pt + & + 2e sin ( pt + e − a ) + že2 sin 2 ( pt + e − a ) + . which is correct only to the first order , since we have re- jected some terms of the second order by neglecting the disturbing ...
Σελίδα 68
... and ordinate of an ellipse referred to its centre : for if Eex and d = y , then x2 y2 + ( 13me ) 2 † ( 11⁄2m ) 1 = 1 . + The acurate value is 31.8119 days . in the expression for the moon's longitude . ́0 = 68 LUNAR THEORY .
... and ordinate of an ellipse referred to its centre : for if Eex and d = y , then x2 y2 + ( 13me ) 2 † ( 11⁄2m ) 1 = 1 . + The acurate value is 31.8119 days . in the expression for the moon's longitude . ́0 = 68 LUNAR THEORY .
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Συχνά εμφανιζόμενοι όροι και φράσεις
accelerating forces Algebra angle angular velocity annual equation apogee approximation apse line argument astronomers attraction Author has endeavoured body calculated CAMBRIDGE CLASS BOOKS centre chapter cloth coefficient Collection of Examples connexion considered correction cos2 Crown 8vo determine differential equations distance disturbing force E-Ma E+Ma earth eccentricity ecliptic elliptic inequality epicycle equal evection expression fixed plane h2u³ higher order Hipparchus inclination ISAAC TODHUNTER John's College late Fellow Latin latitude Lunar M.A. Fellow mean motion mean place mean value method moon moon's mean longitude moon's motion moon's orbit nearly node numerous Examples observations obtained octants order of approximation particle perigee periodical terms position Ps-S Ptolemy quadrature quantity radius vector revolution Schools Second Edition second order shew sidereal month solution sphere student syzygy Theory third order tions true anomaly true longitude Tycho Brahé V₁ variation že²
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