Second episode of the deep dives into the measurements of the universe around us. The first one was about the Earth and the Moon.
This one is about the Solar System, that is, the bodies that orbit the Sun, our star.
The planets classified as such are, in order of increasing orbital radius: Mercury, Venus, Earth, Mars, Jupiter, Saturn, Uranus, Neptune (see Figure 1). Besides these main bodies there are many secondary ones, such as dwarf planet, moons, asteroids, and comets, but we will focus only on the main objects.
Figure 1 – drawing of the sequence of planets of the solar system

Since Kepler (1571–1630) we know that orbits are ellipses (see Figure 2), with the Sun located at one of the foci. In reality, eccentricity (i.e. a – b with reference to Figure 2) is quite low, about 3% for Earth and modest for all the planets except Mercury. Other celestial bodies orbiting in the Solar System, such as asteroids (larger ‘rocks’ measuring a few hundred kilometers), also exhibit significant eccentricity (which measures how much their orbit deviates from a circle). For simplicity we will consider circular orbits and a single radius.
Figure 2 – An ellipse is a plane curve surrounding two focal points, such that for all points on the curve, the sum of both distances to the two focal points is a constant ( FP + PF’ = constant for each P on the curve); in this example, the eccentricity is very large, while for the planets it is much smaller; the F points are called foci, a is the semi-major axis, b is the semi-minor axis.

We will not list all of the measurements for these objects, but only a few reference ones. It is important to understand the need to change the reference scale, moving to a larger one, we can no longer use the soccer ball from the previous post. Now let us imagine Earth as a tiny grain of fine sand (0.09 mm), and its distance from the Sun as 1 meter (the radius of its orbit, usually called the astronomical unit, AU). On this scale, the planet closest to the Sun is Mercury (with a radius 0.38 that of Earth), at about 38 cm. Mars (with a radius 0.52 that of Earth) orbits at about 1.5 m; the gas giants Jupiter (radius 11 times that of Earth, i.e., 0.9 mm on the adopted scale) at about 5 m, and Saturn (radius 9.5 times that of Earth) at about 9.5 m. Uranus and Neptune are very far away, at about 19 m and 30 m respectively. See Figure 3 for a scale diagram.
Figure 3 – a scale diagram of distances in the Solar System

But what does this one meter of distance, taken as a reference for Earth’s orbit, correspond to? It is about 149 million km, a distance that would take roughly 170 years to cover by car traveling at 100 km/h. Light, which travels at 300,000 km/s (more than 1 billion km/h), takes about 8 minutes to go from the Sun to Earth, and more than 4 hours to reach Neptune.
And how big is the Sun? Its radius is about 670,000 km, so compared with the Earth as a soccer ball model, it would be a sphere with a radius of 11.60 m, roughly the volume of a a five-story building of 400 square meters per floor. Compared with the Earth as a grain of fine sand model, it would be a ‘grain’ of almost 1 cm (9.3 mm).
Earth has one large moon, the Moon; Mars has two small ones, Phobos and Deimos. Jupiter has four major moons (Io, Europa, Ganymede, Callisto, discovered in 1609 by Galileo Galilei, 1564–1642) and 91 smaller ones. Saturn has as many as 146 in total! Practically all moons are in synchronous rotation, meaning they always show the same face to their planet, like our Moon.
Saturn’s rings (Figure 4), made up of countless particles of ice and rock, are more than 30,000 km wide (three times Earth’s diameter) but extremely thin, ranging from a few tens of meters to a few hundreds of meters. For this reason, when they are seen edge-on (about every 15 Earth years), they reflect almost no sunlight and are not visible from Earth.
Figure 4 – Saturn photo by HST (source: NASA, ESA, STScI, Amy Simon NASA-GSFC)

Beyond the orbit of Neptune, or on our scale between 30 and 50 meters, lies the Kuiper Belt (named after Gerrit Pieter Kuiper, 1905-1973), which contains thousands of icy bodies, remnants of the formation of the Solar System, including dwarf planets like Pluto, essentially distributed in a volume squashed on the plane of the ecliptic. The so-called heliosphere ends here. An even more external region, the Oort Cloud (named after Jan Oort, 1900-1992), between 2 and 200 km on our scale, has been hypothesized to contain an immense diffusion of ice and rocks, the reservoir from which comets are drawn by the Sun. We can consider it as the outer boundary of the Solar System.
Next episodes:
Understanding the Sizes : 3 – Milky Way
Understanding the Sizes : 4 – galaxy clusters and beyond
Previous episode:
Understanding the Sizes : 1 – Earth and Moon