Mass:330,104,000,000,000 billion kg (0.055 x Earth)
Equatorial Diameter:4,879 km
Polar Diameter:4,879 km
Equatorial Circumference:15,329 km
Known Moons:None
Notable Moons:None
Orbit Distance:57,909,227 km (0.39 AU)
Orbit Period:87.97 Earth days
Surface Temperature:-173 to 427°C
First Record:14th Century BC
Recorded By:Assyrian astronomers

Mercury is the closest planet to the Sun and is also the smallest of the eight planets in our solar system. For every 2 orbits of the Sun, which takes around 88 Earth days, Mercury completes three rotations of its axis. It is gravitationally locked and this rotation is unique to the solar system.

Every seven years or so, Mercury can be seen from Earth passing across the face of the Sun. This happens because Mercury’s orbit is inclined by 7 degrees to the plane of Earth’s orbit and its known as a transit. The next transit of Mercury is on May 9, 2016 and will be visible from Europe after noon.

It is named for the Roman god Mercury, the messenger to the gods – most likely related to the orbiting speed of the planet.


Side by side comparison of the size of Mercury vs Earth
Side by side comparison of the size of Mercury vs Earth


  • Mercury has been known to humanity since ancient times and although its discovery date is unknown, the first mentions of the planet are believed to be around 3000 BC by the Sumerians.
  • A year in Mercury is 88 days, yet a Mercury day is 176 Earth days. Mercury is nearly tidally locked to the Sun – also known as a gravitational lock – and over time this has slowed the rotation of the planet to almost match its orbit around the Sun.
  • Mercury orbits so quickly around the Sun that early civilizations believed it was actually two different stars – one which appeared in the morning and another which appeared in the evening.
  • Mercury is the smallest planet in the solar system with a diameter of 4,879 km and is one of five planets that is visible to the naked eye.
  • After the Earth, Mercury is the second densest planet. Despite its small size, Mercury is very dense because it is composed mainly of heavy metals and rock – the main characteristic of terrestrial planets.
  • Mercury is named after the messenger of the Roman gods, who is also known as Hermes in Greek mythology. This is because of the speed in which Mercury orbits the Sun and the speed with which Mercury the Roman deity was able to deliver messages.
  • Astronomers didn’t realize that Mercury was a planet until 1543 when Copernicus published his Sun-centered model of the Solar System – putting the Sun as the centre of the solar system rather than the previously believed centre, the Earth.
  • The planet has just 38% of the gravity on Earth. This means that Mercury isn’t able to hold the atmosphere it has and it instead gets blown away by solar winds. However those same solar winds are also bringing in new gases, radioactive decay and dust from micrometeorites – replenishing the atmosphere.
  • Mercury has no moons or rings because of its low gravity and lack of atmosphere.
  • It was once believed that a planet called Vulcan existed between the orbit of Mercury and the Sun – however the existence of such a planet was never found.
  • The orbit of Mercury is an ellipse rather than circular. It has the most eccentric orbit in the solar system and the least circular of all of the planets, according to scientists and astronomers.
  • Mercury is only the second hottest planet. Venus, though farther from the Sun than Mercury, actually experiences higher temperatures. This is because Mercury has no atmosphere to regulate temperature and results in the most extreme temperature change of all the planets – ranging from -170°C (-280°F) during the night to 430°C (800°F) during the day.
  • Mercury does not experience any seasons. The axis of Mercury has the smallest tilt of all other planets, and this results in a lack of seasons on its surface.
  • Mercury is the only planet which doesn’t rotate exactly once every year – instead rotating three times for every two orbits of the Sun. This is because it is nearly tidally locked to the Sun.
  • The orbit of Mercury was important in proving Albert Einstein’s theory of General Relativity.
  • Mercury has a large iron core that is around 40% of its volume (compared to a core volume of 17% for Earth) in its centre whose radius is 1800 to 1900 kilometers (1100 to 1180 miles). Scientists believe the core of Mercury is probably molten.
  • The outer shell of Mercury is only 500 to 600 kilometers (310 to 375 miles) thick. Earth’s outer shell (the mantle and crust) is 2930 kilometers (1819 miles) thick.
  • Mercury has a very thin atmosphere, which is made up of atoms from the surface of the planet that have been blown away by solar winds. As Mercury is so hot, these atoms quickly escape into space and so its atmosphere is constantly being replenished.
  • Mercury has a weak magnetic field whose strength is about 1% of the magnetic field on Earth.
  • Only two spacecraft have ever visited Mercury. It is difficult to reach the planet due to its proximity to the Sun and any spacecraft visiting would need to travel 91 million kilometers into the Sun’s gravitational potential well. The Mariner 10 visited during 1974-75, flying by Mercury three times and mapping half its surface. On March 24, 1975 it ran out of fuel and is still believed to be orbiting the Sun. The MESSENGER probe was launched in 2004 to explore Mercury’s high density, its geological history, the nature of its magnetic field and more. Another mission, BepiColombo, is to be launched in 2015 by the European Space Agency and Japan is expected to reach Mercury in 2019.
  • Mercury has more craters and impact marks that any other planet. The surface is similar to that of the Moon, as unlike most planets, Mercury isn’t geologically active and cannot “self heal” from impacts with asteroids and comets. Most of the Mercurian craters are named after famous writers and artists. If a crater is larger than 250 km in diameter, it is known as a Basin. The largest Basin on Mercury, the Caloris Basin, is around 1,550 km in diameter and was discovered by the Mariner 10.


What remains intriguing about Mercury is how scant our knowledge has been regarding some of its key details until recently. For example, it was only in 1974 that the Mariner 10 spacecraft captured the first images providing any specific detail of the Mercurial surface. Within the last several years, unexpected discoveries regarding Mercury’s atmosphere and interior have challenged previously accepted theories.

Now is an exciting time of discovery and new understanding of Mercury. On March 18,2011, the MESSENGER spacecraft achieved orbit around Mercury in what will be a year-long mission. Hopefully, many of our questions will be answered, and, almost certainly, new ones will arise.


The Mercurial atmosphere is so thin that it is virtually non-existent. In fact, at approximately 1015 times less dense than the Earth’s atmosphere, Mercury’s is closer to a true vacuum than any man-made vacuum ever created.

The explanation behind the lack of substantial atmosphere is twofold. Firstly, with a gravity only about 38% that of the Earth’s, Mercury is simply unable to retain much of an atmosphere. Secondly, Mercury’s close proximity to the Sun causes it to be constantly bombarded by solar winds, which carries off most of what little atmosphere does accumulate.

However, as meagre as its atmosphere is, Mercury does have one. According to NASA, its chemical composition is thought to be as follows: 42% oxygen (O2), 29% sodium, 22% hydrogen (H2), 6% helium, .5% potassium, and possibly trace amounts of argon, carbon dioxide, water, nitrogen, xenon, krypton, neon, calcium (Ca, Ca+), and magnesium.

A notable result of such a sparse atmosphere is the extreme temperatures found on the planet’s surface. With a low temperature of approximately -180° C and high of approximately430° C. Mercury has the largest range of surface temperatures found on any planet. The extreme highs present on the side facing the Sun are due to the insufficient atmosphere, for it is unable to absorb the solar radiation. As for the extreme colds on the side facing away from the Sun, without a substantial atmsophere to trap solar radiation, all heat is lost to space.


Until 1974, the Mercurial surface remained, in large part, a mystery to scientists due to Mercury’s close proximity to the Sun. Being so close to the Sun restricts Mercury’s visibility to just before dawn or right after dusk. At these times, unfortunately, the angle at which we see Mercury from the ground takes our line of sight through a significant amount of the Earth’s atmosphere, greatly obstructing our view.

However, during its three fly-bys of Mercury in 1974, the Mariner 10 spacecraft captured clear and stunning photographs of the planet’s surface. Amazingly, Mariner 10 photographed almost half of the planet’s surface during its mission! The results revealed that Mercury’s surface has three significant features.

The first feature is the huge number of impact craters that have accrued over billions of years. Caloris Basin is the largest of these with a diameter of 1,550 km. The second feature is the plains found between craters. These are smooth areas of the surface, hypothesized to have been created from ancient lava flows. The third feature is the cliffs (also known as scarps), which run anywhere from tens to thousands of kilometers in length and from one hundred meters to two kilometers in height.

The importance of these two features lies in what they imply. By the presence of ancient lava fields, it is clear that there was volcanic activity at one time. However, given the number and age of the craters, scientists have concluded that Mercury has been geologically inactive for a significant period.

The third of the surface features tells us something of great interest as well. Essentially, the scarps found on the surface are huge cliffs caused by the buckling of the planet’s crust. What is significant about the buckling on Mercury is what it implies. To understand the significance, we must use a comparison. The buckling on Earth is due to the shifting of tectonic plates, whereas the buckling on Mercury is due to the shrinking of its core. The implication is that because Mercury’s core is shrinking so, too, is the planet as a whole. Recent estimates show that Mercury’s diameter has decreased in excess of 1.5 kilometers.


Broadly speaking, Mercury’s interior is composed of three distinct layers: a crust, mantle, and core.

The planet’s crust is estimated to be between 100 and 300 kilometers in thickness. Mercury’s surface is part of the crust, so the presence of the previously mentioned scarps indicates that the crust is solid and brittle.

With a thickness of approximately 600 kilometers, Mercury’s mantle is relatively thin. Supposedly, its mantle has not always been this thin. Mercury used to have a much thicker mantle, but the leading theory explains that during formation of the Solar System, a large planetesimal collided with the planet, launching most of the mantle into space.

Mercury’s core has been the focus of much research. With an estimated diameter of 3,600 kilometers, the core gives the planet some ineteresting properties. The most obvious of these properties is Mercury’s extreme density for its size. With a planetary diameter of 4,878 kilometers, Mercury is smaller than the Jovian moon Ganymede and the Saturnian moon Titan, whose diameters are 5,270 km and 5,152 km, respectively. However, with a mass of 3.3 x 1023 kg, Mercury’s density of 5,540 kg/m3.

One debate that has recently be resolved regarding Mercury’s core is whether or not it is solid or liquid. By measuring how radio waves bounced off of the planet, scientists were able to determine that the core is, in fact, liquid. More specifically, the data gathered help to measure the amount of wobble in Mercury’s rotation. With a solid core the rotation would be rigid, whereas with a liquid core there are small amounts of variation in the rotation due to the liquid inside “sloshing” around.


With Mercury being so much closer to the Sun than any other planet, it naturally takes the shortest time to complete one full orbit. As a result, a Mercurial year is only about 88 Earth days in length.

A significant feature of Mercury’s orbit is its high eccentricity as compared to other planets. Furthermore, of all the planetary orbits, Mercury’s is the least circular. What this effectively means is that the difference between Mercury’s perihelion&#8212the closet orbital distance to the Sun&#8212of 4.60 x 107 km and its aphelion&#8212farthest orbital distance from the Sun&#8212of 6.98 x 107 km is rather large when contrasted with that of the other planets.

This eccentricity, along with the lack of a substantial atmosphere, helps to explain why Mercury’s surface experiences a wider range of temperature extremes than any other planet in the Solar System. Simply put, Mercury’s surface is much hotter at perihelion than at aphelion due to the large difference between the two distances. Conversely, the temperatures of other planets remain relatively stable because their aphelion and perphelion are virtually the same.

Mercury’s orbit is also significant in that it provides a beautiful example of modern physics. Over time the orbit of Mercury shifts slightly around the Sun (See Figure 1). This process is known as precession.

Though Newtonian mechanics (i.e., classical physics) does a fairly good job of predicting the speed of this precession, it still cannot predict it precisely. This was a persistent problem for astronomers in the late nineteenth and early twentieth century. Many theories were introduced to explain the difference between the actual and theoretical rates. One theory even suggested the existence of a unknown planet closer to the Sun than Mercury. However, the truth was finally revealed when Einstein published his general theory of relativity. As a consequence of this theory, Mercury’s orbital precession was finally described exactly.

Though it was long believed that Mercury’s spin-orbit resonance (the number of rotations per orbit) was 1:1, it was discovered in the mid-twentieth century that it is, in fact, 3:2. This resonance produces what would be fascinating phenomena for a witness on the planet’s surface. For example, the Sun would appear to rise to the highest point in the sky, then reverse its course and set in the same direction from where it rose.


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