Results 231 to 240 of about 4,012,092 (280)
Some of the next articles are maybe not open access.
2010
Gravitational forces dominate the orbital motion of celestial bodies and unpowered vehicles. All the stars, planets, moons and dark matters, moving around in the universe, contribute mutually to the field of gravitational forces.
openaire +2 more sources
Gravitational forces dominate the orbital motion of celestial bodies and unpowered vehicles. All the stars, planets, moons and dark matters, moving around in the universe, contribute mutually to the field of gravitational forces.
openaire +2 more sources
2004
The goal of this chapter is to derive Kepler's laws of planetary motion from Newton's laws of motion and gravitation. We will analyze the motion of two massive particles (such as the sun and Mars), assuming that all forces other than mutual gravitational attraction are negligible. We want to find explicit formulas allowing us to predict motions.
+5 more sources
The goal of this chapter is to derive Kepler's laws of planetary motion from Newton's laws of motion and gravitation. We will analyze the motion of two massive particles (such as the sun and Mars), assuming that all forces other than mutual gravitational attraction are negligible. We want to find explicit formulas allowing us to predict motions.
+5 more sources
Electromagnetic Two-Body Problem
Physical Review, 1963The circular motion of two classical point charges interacting through their time-symmetric electromagnetic fields is determined with complete relativistic rigor. Expressions are obtained for the total energy and angular momentum of this two-body system, which include the contributions of the field.
openaire +1 more source
2016
Assume that the masses are spherically symmetrical and homogeneous in concentric layers.
Pini Gurfil, P. Kenneth Seidelmann
openaire +2 more sources
Assume that the masses are spherically symmetrical and homogeneous in concentric layers.
Pini Gurfil, P. Kenneth Seidelmann
openaire +2 more sources
Open Relativistic Two-body Problem
International Journal of Theoretical PhysicszbMATH Open Web Interface contents unavailable due to conflicting licenses.
openaire +1 more source
2017
Astrodynamics is defined by Kaplan (Modern spacecraft dynamics and control. Wiley, New York [1]) as “the study of controlled flight paths of man-made spacecraft”. This discipline is also defined in a more detailed manner by the American Institute of Aeronautics and Astronautics [2] as “the determination, prediction, physical adjustment, and ...
openaire +2 more sources
Astrodynamics is defined by Kaplan (Modern spacecraft dynamics and control. Wiley, New York [1]) as “the study of controlled flight paths of man-made spacecraft”. This discipline is also defined in a more detailed manner by the American Institute of Aeronautics and Astronautics [2] as “the determination, prediction, physical adjustment, and ...
openaire +2 more sources
1995
Abstract As we have stated in the introduction to the last chapter (§57), a watershed was reached in the development of the Principia at the end of Section IX. In resuming the main development, after a brief pause in Section X, Newton writes: I have hitherto been treating of the attractions of bodies towards an immovable centre; though ...
openaire +1 more source
Abstract As we have stated in the introduction to the last chapter (§57), a watershed was reached in the development of the Principia at the end of Section IX. In resuming the main development, after a brief pause in Section X, Newton writes: I have hitherto been treating of the attractions of bodies towards an immovable centre; though ...
openaire +1 more source
1991
One of the major successes of the Dirac theory—as we have seen in Chapter 3—was the explanation of the energy spectrum of hydrogen-like atoms, including the fine structure. And in the preceding chapter we began to achieve an understanding of additional features in the spectrum on a quantitative level.
openaire +1 more source
One of the major successes of the Dirac theory—as we have seen in Chapter 3—was the explanation of the energy spectrum of hydrogen-like atoms, including the fine structure. And in the preceding chapter we began to achieve an understanding of additional features in the spectrum on a quantitative level.
openaire +1 more source