Oblateness
Ratio of the difference between the equatorial and polar radii to the equatorial radius. Oblateness usually is an indication of how fast the body is rotating.
Oblique Rotator ...
Oblateness The ratio of a planet's polar to its equatorial diameter.
Obliquity The degree of inclination (or tilt) of a planet's equator to its orbital plane.
Occultation The disappearance of one celestial body behind another.
Oblateness- the degree of flattening at the poles of a celestial body
Occulation- the covering up of one celestial object by another, such as the Moon passing in front of a star or planet as seen from Earth ...
Oblateness
The flattening of a spherical body; usually caused by rotation
Occultation ...
Oblateness
a measure of flattening at the poles of a planet or other celestial body.
Obliquity
the angle between a body's equatorial plane and orbital plane.
Oblateness. The measure of how much a rotating object deviates from being a perfect sphere. A perfect sphere would have an oblateness of 0.0 (0%). The Earth for example is oblate to a factor of 0.
Oblateness - A departure from spherical shape of a body in which the body's polar diameter is smaller than its equatorial diameter ...
[edit] Oblateness and surface temperature
Image of the rapidly rotating star Altair, made with the MIRC imager on the CHARA array on Mt. Wilson ...
Oblateness:
The depature of a planet from spherical form because of the centrifugal force of the rotation.
Oblateness is a measure of how the planet's figure departs from a sphere.
The Rotation Period for each planet is the period relative to the stars. This is slightly different from the period relative to the Sun, which for the Earth we call the day.
7 × 109 cm; oblateness (from Pioneer 10) 0.065. Surface gravity 2.7 that of Earth; Vesc 61 km s-1; mean density 1.33 g cm-3. Rotational period 9h50m at equator; 9h55m at polar regions (see Systems I and II longitude). Semi-major axis 5.203AU, e = 0.
This response is expressed in terms of the planet's oblateness. By measuring the degree of flattening at the poles as compared with the speed of rotation, one can infer the density distribution inside the planet.
The Sun is a near-perfect sphere, with an oblateness estimated at about 9 millionths, which means that its polar diameter differs from its equatorial diameter by only 10 km (6 mi).
Notes: Mass is given in Earth masses (1 ME = 5.977 × 1024 kilograms); diameter is the ``volumetric mean diameter'' that takes into account the planet's oblateness; ...
This permitted Charles Augustus Young to attempt a careful measurement of the oblateness (polar compression) of Mars during the 1879 event. He obtained the value 1/219, or 0.0046.
The moon's gravity primarily, and to a lesser degree the sun's gravity, act on Earth's oblateness to move the axis perpendicular to the plane of Earth's orbit.
Mean Orbital Velocity in kilometers per second Axial incl Inclination of the rotation axis in degrees (obliquity) Oblate Oblateness Ascend Longitude of the ascending node Perihelion Longitude of perihelion Equilib Equilibrium temperature in Kelvins ...
The oblateness of Jupiter was noted through the telescope by Giovanni Cassini (1625-1712), director of the Paris observatory, However, he and his son also claimed that Earth was different, ...
The pressure at the center of Neptune is millions of times more than that on the surface of Earth. Comparing its rotational speed to its degree of oblateness indicates that it has its mass less concentrated towards the center than does Uranus.
The longitudes and latitudes thus defined are geocentric, and the latitude is slightly different from that in ordinary use for geographic purposes. The difference arises from the oblateness of the earth, and need not be considered here.
 See also: Earth, Rotation, Planet, Sun, Orbit
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