Why does the earth have a season

 Season

A season is a division of the year, marked by changes in weather, ecology, and hours of daylight.
Seasons result from the yearly revolution of the Earth around the Sun and the tilt of the Earth's axis relative to the plane of revolution. 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 go into hibernation or to migrate, and plants to be dormant.
During May, June and July, the northern hemisphere is exposed to more direct sunlight because the hemisphere faces the sun. The same is true of the southern hemisphere in November, December and January. It is the tilt of the Earth that causes the Sun to be higher in the sky during the summer months which increases the solar flux. However, due to seasonal lag, June, July and August are the hottest months in the northern hemisphere and December, January and February are the hottest months in the southern hemisphere.
In temperate and subpolar regions generally four calendar-based seasons are recognized: spring (adj. vernal), summer (adj. estival), autumn (adj. autumnal), and winter (adj. hibernal). However, ecologists are increasingly using a six-season model for temperate climate regions that includes pre-spring (adj. prevernal) and late summer (adj. seritonal) as distinct seasons along with the traditional four (See Ecological Seasons below).
In some tropical and subtropical regions it is more common to speak of the rainy (or wet, or monsoon) season versus the dry season, because the amount of precipitation may vary more dramatically than the average temperature. For example, in Nicaragua, the dry season (October to May) is called 'summer' and the rainy season (April to November) is called 'winter', even though it is located in the northern hemisphere.
In other tropical areas a three-way division into hot, rainy and cool season is used.
In some parts of the world, special "seasons" are loosely defined based upon important events such as a hurricane season, tornado season or a wildfire season.
Chinese seasons are traditionally based on 24 periods known as solar terms, and begin at the midpoint of solstices and equinoxes.

Astronomical

The following diagram shows the relation between the line of solstice and the line of apsides of Earth's elliptical orbit. The orbital ellipse (with eccentricity exaggerated for effect) goes through each of the six Earth images, which are sequentially the perihelion (periapsis—nearest point to the sun) on anywhere from 2 January to 5 January, the point of March equinox on 20 or 21 March, the point of June solstice on 20 or 21 June, the aphelion (apoapsis—farthest point from the sun) on anywhere from 4 July to 7 July, the September equinox on 22 or 23 September, and the December solstice on 21 or 22 December.

Longitude and latitude

Longitude

Longitude is the angular distance of a point's meridian from the Prime (Greenwich) Meridian. It is usually expressed in degrees, minutes, and seconds. Lines of longitude are often referred to as meridians , identified by the Greek letter lamba lambda (λ), is the geograpic coordinate most commonly used in cartography and global navigation for east-west measurement. Constant longitude is represented by lines running from north to south. The line of longitude (meridian) that passes through the Royal Observatory, Greenwich, in England, establishes the meaning of zero degrees of longitude, or the Prime Meridian. Any other longitude is identified by the east-west angle, referenced to the center of the Earth as vertex, between the intersections with the Equator of the meridian through the location in question and the Prime Meridian. A location's position along a meridian is given by its latitude, which is identified by the north-south angle between the local vertical and theplane of the Equator.

Latitude

Latitude, usually denoted by the Greek letter phi (φ) gives the location of a place on Earth (or other planetary body) north or south of the equator. Lines of Latitude are the imaginary horizontal lines shown running east-to-west (or west to east) on maps (particularly so in the Mercator projection) that run either north or south of the equator. Technically, latitude is an angular measurement in degrees (marked with °) ranging from 0° at the equator (low latitude) to 90° at the poles (90° N or +90° for the North Pole and 90° S or −90° for the South Pole). The latitude is approximately the angle between straight up at the surface (the zenith) and the noonday sun when it is at the equinox. The complementary angle of a latitude is called the colatitude.
All locations of a given latitude are collectively referred to as a circle of latitude or line of latitude or parallel, because they are coplanar, and all such planes are parallel to the equator. Lines of latitude other than the Equator are approximately small circles on the surface of the Earth; they are not geodesics since the shortest route between two points at the same latitude is a path that (when drawn on most small-scale maps) seems to bulge toward the nearest pole, first moving farther away from and then back toward the equator (see great circle).

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