enow.com Web Search

Search results

  1. Results from the WOW.Com Content Network
  2. List of gravitationally rounded objects of the Solar System

    en.wikipedia.org/wiki/List_of_gravitationally...

    Vesta (radius 262.7 ± 0.1 km), the second-largest asteroid, appears to have a differentiated interior and therefore likely was once a dwarf planet, but it is no longer very round today. [74] Pallas (radius 255.5 ± 2 km ), the third-largest asteroid, appears never to have completed differentiation and likewise has an irregular shape.

  3. Gravity of Mars - Wikipedia

    en.wikipedia.org/wiki/Gravity_of_Mars

    The gravity of Mars is a natural phenomenon, due to the law of gravity, or gravitation, by which all things with mass around the planet Mars are brought towards it. It is weaker than Earth's gravity due to the planet's smaller mass. The average gravitational acceleration on Mars is 3.728 m/s 2 (about 38% of the gravity of Earth) and it varies. [1]

  4. Characteristic energy - Wikipedia

    en.wikipedia.org/wiki/Characteristic_energy

    The InSight mission to Mars launched with a C 3 of 8.19 km 2 /s 2. [5] The Parker Solar Probe (via Venus) plans a maximum C 3 of 154 km 2 /s 2. [6] Typical ballistic C 3 (km 2 /s 2) to get from Earth to various planets: Mars 8-16, [7] Jupiter 80, Saturn or Uranus 147. [8] To Pluto (with its orbital inclination) needs about 160–164 km 2 /s 2. [9]

  5. Mars - Wikipedia

    en.wikipedia.org/wiki/Mars

    At the bottom of the mantle lies a basal liquid silicate layer approximately 150–180 km thick. [44] [54] Mars's iron and nickel core is completely molten, with no solid inner core. [55] [56] It is around half of Mars's radius, approximately 1650–1675 km, and is enriched in light elements such as sulfur, oxygen, carbon, and hydrogen. [57] [58]

  6. Standard gravitational parameter - Wikipedia

    en.wikipedia.org/wiki/Standard_gravitational...

    μ = Gm 1 + Gm 2 = μ 1 + μ 2, where m 1 and m 2 are the masses of the two bodies. Then: for circular orbits, rv 2 = r 3 ω 2 = 4π 2 r 3 /T 2 = μ; for elliptic orbits, 4π 2 a 3 /T 2 = μ (with a expressed in AU; T in years and M the total mass relative to that of the Sun, we get a 3 /T 2 = M) for parabolic trajectories, rv 2 is constant and ...

  7. List of Solar System objects by size - Wikipedia

    en.wikipedia.org/wiki/List_of_Solar_System...

    For example, if a TNO is incorrectly assumed to have a mass of 3.59 × 10 20 kg based on a radius of 350 km with a density of 2 g/cm 3 but is later discovered to have a radius of only 175 km with a density of 0.5 g/cm 3, its true mass would be only 1.12 × 10 19 kg.

  8. Two-body problem in general relativity - Wikipedia

    en.wikipedia.org/wiki/Two-body_problem_in...

    In (1+1) dimensions, i.e. a space made of one spatial dimension and one time dimension, the metric for two bodies of equal masses can be solved analytically in terms of the Lambert W function. [11] However, the gravitational energy between the two bodies is exchanged via dilatons rather than gravitons which require three-space in which to ...

  9. Equations for a falling body - Wikipedia

    en.wikipedia.org/wiki/Equations_for_a_falling_body

    The first equation shows that, after one second, an object will have fallen a distance of 1/2 × 9.8 × 1 2 = 4.9 m. After two seconds it will have fallen 1/2 × 9.8 × 2 2 = 19.6 m; and so on. On the other hand, the penultimate equation becomes grossly inaccurate at great distances.