Astronomical seasons

This is an educational model of the Sun, Earth, and Earth's orbit to illustrate and clarify why and when seasons change. Astronomical seasonsThe reason seasons exist is Earth's orbital tilt, i.e. its axis tilt of about 23,5 degrees to the plane in which it orbits the Sun (ecliptic plane). [The reason for the seasons is not Earth's distance to the Sun, which is a fairly common misconception.] Because of the tilt Earth's northern (or southern) hemisphere is sometimes inclined towards (Summer) or away from the Sun (Winter). The seasons start at the solstices or equinoxes (more about it can be found here), and interestingly enough the Earth is closer to the Sun during Winter than during Summer (at the northern hemisphere). Its closest point to the Sun is around January 5th (perihelion), and the furthest around July 5th (aphelion).The model in a few wordsEarth's elliptical orbit and characteristic points in the orbit (aphelion, perihelion, solstices and equinoxes) are in