What is the distance around the earth in kilometers12.05.2021
Jun 16, · Measured at the equator, the Earth has a circumference of 40, km or 24, miles. But measured from pole to pole, that is to say, along the . Mar 02, · Circumference of the Earth The circumference of the Earth in kilometers is 40, km, and the circumference of the Earth in miles is 24, In .
The kilkmeters of the Earth in kilometers is 40, km, and the circumference of the Earth in miles is 24, The formula for calculating the circumference of a sphere is 2 x pi x radius. So, the radius of the Earth is km. Plug that into the formula, and you get 2 x 3. It would be more accurate if you use more digits for pi. You might be interested to know that the circumference of the Earth is different depending on how you measure it. But if you measure it from diztance to pole, you get 40, km.
The Earth is a flattened sphere, and so the distance around the equator is further than the circumference around the poles.
Want some comparison? The circumference of the Moon is 10, km, and the circumference of Jupiter iskm. Here are a bunch of measurements for you: Circumference of the Earth in kilometers: 40, km Circumference of the Earth in meters: 40, meters Circumference of the Earth in centimeters: 4,, centimeters. Circumference of the Earth in miles: 24, miles Circumference of the Earth in feet: , feet Circumference of the Earth in how to tighten saggy stomach after pregnancy 1,, inches.
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Earth's circumference (the distance all the way around the equator) is 24, miles (40, kilometers). Its diameter (the distance from one side to the other through Earth's center) is 7, miles (about 12, kilometers). Earth is slightly smaller when measured between the North and South Poles which gives a diameter of 7, miles (12, kilometers). Sep 15, · Earth's polar radius is 3, miles (6, km) — a difference of 13 miles (22 km). Using those measurements, the equatorial circumference of Earth is about 24, miles (40, km). AU or million km / 66 million mi: Earth: AU or million km / 93 million mi: AU or million km / 94 million mi: AU or million km / 91 million mi: Mars: AU or million km / million mi: AU or million km / million mi: AU or million km / million mi: Jupiter: AU or million km / million mi.
Earth orbits the Sun at an average distance of From a vantage point above the north pole of either the Sun or Earth, Earth would appear to revolve in a counterclockwise direction around the Sun.
From the same vantage point, both the Earth and the Sun would appear to rotate also in a counterclockwise direction about their respective axes. Heliocentrism is the scientific model that first placed the Sun at the center of the Solar System and put the planets, including Earth, in its orbit.
Historically, heliocentrism is opposed to geocentrism , which placed the Earth at the center. Aristarchus of Samos already proposed a heliocentric model in the third century BC. In the sixteenth century, Nicolaus Copernicus ' De revolutionibus presented a full discussion of a heliocentric model of the universe  in much the same way as Ptolemy had presented his geocentric model in the second century.
This " Copernican revolution " resolved the issue of planetary retrograde motion by arguing that such motion was only perceived and apparent. Because of Earth's axial tilt often known as the obliquity of the ecliptic , the inclination of the Sun's trajectory in the sky as seen by an observer on Earth's surface varies over the course of the year. For an observer at a northern latitude, when the north pole is tilted toward the Sun the day lasts longer and the Sun appears higher in the sky.
This results in warmer average temperatures, as additional solar radiation reaches the surface. When the north pole is tilted away from the Sun, the reverse is true and the weather is generally cooler. North of the Arctic Circle and south of the Antarctic Circle , an extreme case is reached in which there is no daylight at all for part of the year, and continuous daylight during the opposite time of year.
This is called polar night and midnight sun , respectively. This variation in the weather because of the direction of the Earth's axial tilt results in the seasons.
By astronomical convention, the four seasons are determined by the solstices the two points in the Earth's orbit of the maximum tilt of the Earth's axis, toward the Sun or away from the Sun and the Equinoxes the two points in the Earth's orbit where the Earth's tilted axis and an imaginary line drawn from the Earth to the Sun are exactly perpendicular to one another. The solstices and equinoxes divide the year up into four approximately equal parts.
In the northern hemisphere winter solstice occurs on or about December 21; summer solstice is near June 21; spring equinox is around March 20, and autumnal equinox is about September In modern times, Earth's perihelion occurs around January 3, and the aphelion around July 4 for other eras, see precession and Milankovitch cycles. The changing Earth-Sun distance results in an increase of about 6. Since the southern hemisphere is tilted toward the Sun at about the same time that the Earth reaches the closest approach to the Sun, the southern hemisphere receives slightly more energy from the Sun than does the northern over the course of a year.
However, this effect is much less significant than the total energy change due to the axial tilt, and most of the excess energy is absorbed by the higher proportion of surface covered by water in the southern hemisphere. The Hill sphere gravitational sphere of influence of the Earth is about 1,, kilometers 0.
Objects orbiting the Earth must be within this radius, otherwise, they may become unbound by the gravitational perturbation of the Sun. The following diagram shows the relation between the line of the solstice and the line of apsides of Earth's elliptical orbit. The orbital ellipse goes through each of the six Earth images, which are sequentially the perihelion periapsis — nearest point to the Sun on anywhere from January 2 to January 5, the point of March equinox on March 19, 20, or 21, the point of June solstice on June 20, 21, or 22, the aphelion apoapsis — the farthest point from the Sun on anywhere from July 3 to July 5, the September equinox on September 22, 23, or 24, and the December solstice on December 21, 22, or In , Jacques Laskar 's work indicated that the Earth's orbit as well as the orbits of all the inner planets can become chaotic and that an error as small as 15 meters in measuring the initial position of the Earth today would make it impossible to predict where the Earth would be in its orbit in just over million years' time.
From Wikipedia, the free encyclopedia. Not to be confused with Earth orbit. Trajectory of Earth around the Sun. Main article: Heliocentrism. Main article: Season. Main article: Stability of the Solar System. Earth portal Astronomy portal. Astronomical unit Barycenter Earth's axial tilt Earth phase Earth's rotation Geocentric orbit — the orbit of any object orbiting the Earth, such as the Moon or an artificial satellite Spaceship Earth.
Thus, the Sun will appear to move across the sky relative to the stars by that same amount. The quantities given are the values at the instant J Subtracting from that Solar System Exploration. National Aeronautics and Space Administration. Archived from the original on July 3, Retrieved July 29, See Ellipse Circumference. The formula by Ramanujan is accurate enough. Retrieved 17 March Johannes Petreius. NASA ". Retrieved 22 January See the "Orbital characteristics" table. Due to the inverse square law, the radiation at perihelion is about Retrieved 21 March February Astronomy and Astrophysics.
Allen's Astrophysical Quantities. ISBN In Murdin, Paul ed. Encyclopedia of Astronomy and Astropvhysics. Bristol: Institute of Physics Publishing. Deep simplicity : bringing order to chaos and complexity 1st U. New York: Random House. Gravitational orbits. T Orbital period n Mean motion v Orbital speed t 0 Epoch. Bi-elliptic transfer Collision avoidance spacecraft Delta-v Delta-v budget Gravity assist Gravity turn Hohmann transfer Inclination change Low energy transfer Oberth effect Phasing Rocket equation Rendezvous Transposition, docking, and extraction.
Celestial coordinate system Characteristic energy Escape velocity Ephemeris Equatorial coordinate system Ground track Hill sphere Interplanetary Transport Network Kepler's laws of planetary motion Lagrangian point n -body problem Orbit equation Orbital state vectors Perturbation Retrograde motion Specific orbital energy Specific relative angular momentum Two-line elements.
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