An eccentricity of exactly 1 is a parabolic orbit and anything greater than that is a hyperbolic orbit. The orbits of the planets are almost circular with the exception of Mercury (0.206) and Mars to a lesser extent. The Earth has an eccentricity of 0.017. Most asteroids have orbital ...
Eccentricity is a measure of how an orbit deviates from circular. A perfectly circular orbit has an eccentricity of zero; higher numbers indicate more elliptical orbits. Neptune, Venus, and Earth are the planets in our solar system with the least eccentric orbits. Pluto and Mercury are the ...
The eccentricity function of the orbit of Jupiter presents large oscillations with periods of about 60 and 900- 960 years, mostly due to the interaction with Saturn. These oscillations also correspond to oscillations found in several geophysical records. The eccentricity functions of Uranus and ...
1 demonstrated for the first time the presence of 104–105 year astronomical cycles in Pleistocene deep-sea sediments, confirming Milankovitch’s theory that Earth’s climate is modulated by periodicities in perturbations of Earth’s orbit around the Sun and Earth’s spin axis2. Apart from the ...
We first show that three main sources of Earth-crossers which are, according to recent simulations, the 3/1 and 谓 6 resonances in the main belt, and the Mars-crosser population, are not able to produce as many bodies on SEAs-like orbits compared to other Earth-crossing orbits as has ...
This is of particular interest for planets with polar icecaps (or lakes and seas), like Mercury, Earth, and Mars (or Titan). The nearly 600 exoplanets now with known eccentricities span a wide range of eccentricity from essentially zero up to near unity; but their obliquities are still ...
This note analyzes the effects of the actual irradiance on low-eccentricity orbits as an introductory work to much more complex cases such as sailcraft-Mars rendezvous. Two special orbits are considered: (1) a circular warning orbit and (2) a transfer orbit between Earth and Mars. It turns ...
Many trajectories of the third body are integrated numerically in a modified elliptical restricted three body problem (ERTBP), in which the eccentricity, e ′, of the orbit of the second primary varies sinusoidally with time. It is found that, in the case of the 2:1 resonance, the ...