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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 ...
On Earth, seasons are the result of the axial parallelism of Earth's tilted orbit around the Sun. [2] [3] [4] In temperate and polar regions, the seasons are marked by changes in the intensity of sunlight that reaches the Earth's surface, variations of which may cause animals to undergo hibernation or to migrate, and plants to be dormant ...
Given the different Sun incidence in different positions in the orbit, it is necessary to define a standard point of the orbit of the planet, to define the planet position in the orbit at each moment of the year w.r.t such point; this point is called with several names: vernal equinox, spring equinox, March equinox, all equivalent, and named considering northern hemisphere seasons.
The seasons are quadrants of the Earth's orbit, marked by the two solstices and the two equinoxes. Kepler's second law states that a body in orbit traces equal areas over equal times; its orbital velocity is highest around perihelion and lowest around aphelion. [ 13 ]
By astronomical convention, the four seasons can be determined by the solstices—the points in the orbit of maximum axial tilt toward or away from the Sun—and the equinoxes, when Earth's rotational axis is aligned with its orbital axis.
The exact time of the equinox varies from year to year due to leap years and the Earth's elliptical-shaped orbit around the sun. ... meteorological seasons were created because traditional seasons ...
Earth currently has an axial tilt of about 23.44°. [7] This value remains about the same relative to a stationary orbital plane throughout the cycles of axial precession. [8] But the ecliptic (i.e., Earth's orbit) moves due to planetary perturbations, and the obliquity of the ecliptic is not a
The revamped system had 365 days, with a leap year added every four years, based on the understanding at the time that it took 365.25 days for the Earth to orbit the Sun.