We all know that equation for surface gravity is

$$ g = \frac{4\pi}{3} G \rho r $$

So if we want Earth-like surface gravity of $ g = 9.81 $, then the equation for radius is

$$ r = \frac{3 g}{4\pi G \rho } $$

where $\rho$ is mean density of a planet.

So what's the smallest radius, or highest density we can reasonably find in space to give us Earth-like gravity? By reasonable, I mean that it does not have to be common or even normal. I mean that:

  • It could, theoretically, occur naturally
  • First reaction of scientists should be "what a coincidence!" and not "it's an alien construct!" or "we have a serious problem with our methodology, this can't be!"

Sadly, Earth seems to be the densest body in the solar system, on the "above 400km" table here, and I don't know how could we get any denser.

Note: I'm avare of other questions about small planets but here I don't care for life, tectonics, civilizations etc. I want baseline, canonical answer about smallest size for given gravity.

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    $\begingroup$ when asteroids collide… very small chance to occur only with osmium asteroid, but space is too big, so … "what a coincidence!" $\endgroup$
    – Jan Ivan
    Commented Apr 3, 2017 at 9:02
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    $\begingroup$ Isn't the answer simply the densest possible “normal” matter? $\endgroup$
    – JDługosz
    Commented Apr 3, 2017 at 9:29
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    $\begingroup$ @Mołot So at 0.08µm my fragment of neutronium caused by some sort of glancing blow of a neutron star is going to win the smallest natural planet. But it won't last long! Heh. Not long at all :-D $\endgroup$
    – Konchog
    Commented Apr 3, 2017 at 19:42
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    $\begingroup$ +1 just for including "first reaction of scientists" as a criterion in your definition of "reasonable." An amusing concept. $\endgroup$
    – Wildcard
    Commented Apr 4, 2017 at 3:18
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    $\begingroup$ Yea… a quick look at Wikipedia says osmium is “stable” but we know that's not exactly true. I expect everything higher than bismuth to have a half life shorter than bismuth’s 2×10^19 years. $\endgroup$
    – JDługosz
    Commented Apr 4, 2017 at 14:17

6 Answers 6


The densest reasonable material for a planet is iron

The wikipedia page for the abundance of chemical elements breaks it down a dozen different ways, but any way you split it, by far the most common dense material is iron. In the solar system, Fe-56 is estimated to be the sixth most common nuclide by mass fraction, after H-1, He-4, O-16, C-12, and Ne-20. It occupies the same position in estimates of the Milky Way galaxy.

Any answer that suggests a different material to form a planet out of, must give a reasonable explanation for why that other material won't be mixed with iron, which is at least two orders of magnitude more common than anything denser than it.

You can check out relative abundances here and densities here. The only thing close is Nickel which is also a constituent in the Earth's core. Lead is five orders of magnitude less abundant than Iron; Osmium, Iridium, and Platinum are closer to six.

Making an iron planet

Earth's core is mostly an iron-nickel alloy that has a density in the 10000-13000 kg/m$^3$ range. However, the planet's density is lower, because of the lower density mantle, composed of periodite and olvine and other lower density rocks. The easiest way to make an all-iron planet is to remove the mantle.

How do we remove the mantle? I would suggest one of two ways: a massive collision or formation close to a variable star. Both of these are theories about the formation of Mercury.

The massive collision would be somewhat like the impact that formed the moon. In that collision, much mantle material was blasted off to make the moon. We would need to adjust the collision to blow of all the mantle materials, to leave just an iron core to coalesce. A similar explanation has been proposed for Mercury, which actually has a higher iron content than Earth. However, being less massive, it is not as compressed and therefore less dense.

The other theory for Mercury's formation is that Mercury formed before the proto-sun had fully contracted. The temperatures at Mercury reached 2500K or even 10000K and turned much of the planet into vaporized the rock. The lightest 'rock vapor' was then carried away by the solar wind. A variable star could have, early in its life, pulse melted and then stripped lighter materials from a planet. If the star cooled later in its life, or became less variable, the planet could have solidified into an iron mass.

How big is a 1g Iron planet?

Earth's core density is listed above, and Iron at standard temps and pressure has a density 7870 kg/m$^3$. I'm not exactly sure the density gradient through the mantle, but my estimate is an overall density of about 9500 kg/m$^3$ for a planet with the same composition as Earth's core.

This gives a radius of about 3700 km.

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    $\begingroup$ I'll wait a few days before accepting, but for now I think you nailed it. $\endgroup$
    – Mołot
    Commented Apr 3, 2017 at 19:26
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    $\begingroup$ Beware that this planet will have a hard time holding onto an atmosphere because it's escape velocity is low. $\endgroup$ Commented Apr 4, 2017 at 0:17
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    $\begingroup$ @LorenPechtel: Keeping surface gravity constant, it turns out that escape velocity v ∝ √r, so a 3700 km radius planet with Earth's surface gravity will be only have an escape velocity ~25% lower than for Earth, or around 8.5 km/s. This is closer to the escape velocity for Earth (11.2 km/s) and Venus (10.4 km/s) than it is to Mars (5.03 km/s). The probability of monatomic oxygen reaching 8.5 km/s at 300K is rather low, on the order of 10^-100, so if we can assume a strong magnetic field to protect from solar wind (hey! iron planet is probably very magnetic) then it should keep an atmosphere. $\endgroup$ Commented Apr 4, 2017 at 4:19
  • $\begingroup$ @LorenPechtel This was planned to be a follow-up question $\endgroup$
    – Mołot
    Commented Apr 4, 2017 at 10:08
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    $\begingroup$ @imallett Regarding 16 Psyche, wikipedia says it is almost pure iron-nickel, yet also gives its density as 3300 kg/m$^3$, similar to the Moon or Earth's mantle. Something has to give there. $\endgroup$
    – kingledion
    Commented Apr 5, 2017 at 0:37

Pulsar planets are made from only the heavy elements.

Like PSR B1257+12:

The planets are believed to be the result of a second round of planetary system formation as a result of two white dwarfs merging with each other into a pulsar and a resulting disk of material in orbit around the star.

or 4U 0142+61:

This may prove that pulsar planets are common around neutron stars. The debris disk is likely to be composed of mainly heavier metals.

Now disrupting white dwarfs will cause the spilled material to expand back into normal matter, but will it be mostly iron or what? More generally, a debris cloud made of those elements which did not blow away will be enriched in “heavy metals” so consider osmium, lead, platinum, etc.

An object made from this mix would be expected based on what we know, not taken as artificial. To be more surprising, but still presumed natural with better formation models needed, would be that this heavy metal disk was sorted by weight so that planets formed with different fractions, including one that’s made almost completely out of the heaviest elements.

Maybe the magnetic fields of the pulsar causes separation by element, so you get one planet made of iron, one of lead, two made from the platnum group elements, etc. All the “like” (weight and magnetic moment) material in the cloud is herded into separate bunches in a cosmic scale mass spectrometer, and each bunch ends of forming a planet.

Mołot calculates that the osmium world would be 1553 km, and lead 3094 km, to match Earth’s surface gravity.

Period 5 (Ru, Rh, Pd) and period 6 (Os,Ir,Pt) have different weights.

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    $\begingroup$ White dwarfs are made of carbon and oxygen. The threshold to fuse above that level requires a star large enough to supernova. $\endgroup$ Commented Apr 3, 2017 at 13:05
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    $\begingroup$ This is a periodic table showing the cosmonogenic origin of the Elements. The pulsar production from merging White Dwarfs you propose should produce nothing denser than Iron. You would need to merge neutron stars in order to get anything heavier. That, however, sounds like it would make a black hole. $\endgroup$
    – kingledion
    Commented Apr 3, 2017 at 15:03
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    $\begingroup$ Careful: to an astronomer, a "heavier metal" could be anything above beryllium on the periodic table. It'd be nice to see a scientific article discussing what metals are probably involved, rather than just a Wikipedia article. $\endgroup$ Commented Apr 3, 2017 at 20:08
  • $\begingroup$ @kingledion Well, now a neutron star merger has been observed, and it produced many earth masses worth of gold, platinum, etc. $\endgroup$
    – JDługosz
    Commented Apr 5, 2019 at 22:16


So, it's pretty exotic to have a pure osmium planet, which is why other answers have avoided it. But exotic happens in the universe.

Under normal pressure, Osmium is 22.5g/cm3, whereas the earth itself averages 5.51g/cm3.

At surface pressure, WolframAlpha suggests a radius of 1,560km

But the vast majority of earth is not under normal pressure. Real proper bods have looked at the compressibility of Osmium (it's not very compressible!) and they produced this diagram diagram of osmium under pressure

Google tells us that the pressure at the centre of the earth is about 360GPa, so we can read off the volume from the graph at around 40 angstroms^3 vs. 60 at normal pressures, which gives us 2/3 the volume: 33.75g/cm3.

So again our friendly calculator gives us a minimum radius 1,040km.


So now imagine that a chip of neutronium has split off a neutron star and (impossibly) remains stable. It wouldn't be comfortable (we would rapidly die) for us to walk on, but...

Neutronium has a density of about 4.0×10^14g/cm3, so it's wildly more dense than Osmium, and you would get a sphere of pure neutronium with a radius of about 8 hundredths of a micrometer.

So, as long as your planet has a neutronium core, you should be able to have a planet of any radius (bigger than micrometer) you choose, just by wrapping the core in a shield something to stabilise the neutronium.

Little Prince Huge Kudos to Dietrich-Epp for noticing my terrible maths

  • $\begingroup$ Is the osmium density calculation assuming that it has the same density throughout, even nearer the surface? $\endgroup$ Commented Apr 3, 2017 at 12:56
  • $\begingroup$ @trichoplax, well yes but the difference is going to be quite negligible bearing in mind the degree of rounding we are looking at. Given the graph above It should be pretty trivial to derive a reasonable function of density from pressure at a given radius. $\endgroup$
    – Konchog
    Commented Apr 3, 2017 at 13:16
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    $\begingroup$ Unfortunately any small mass of neutronium (smaller than a neutron star) would almost certainly no longer be able to hold itself together without gravity forcing neutron degeneracy. $\endgroup$
    – Murphy
    Commented Apr 3, 2017 at 15:12
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    $\begingroup$ @kingledion, certainly in our region of the galaxy, Osmium is rare. But the galaxy is huge - and the universe more so. The fourth word of my answer is 'exotic'! $\endgroup$
    – Konchog
    Commented Apr 3, 2017 at 16:11
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    $\begingroup$ obligatory xkcd reference $\endgroup$
    – Mołot
    Commented Apr 3, 2017 at 19:28

So I approached this in a more experimental way than theory and plotted the density from a list of the planets we know of and searching for the densest one (that isn't a gas giant).

So we have:

55 Cancri e $$Radius = 1.990 \times R_{E}$$ $$Mass = 8.347 \times M_{E}$$

So sticking these into the density equation: $$\rho_{C55e} = \frac{M_{C55e}}{\frac{4}{3} \pi R^{3}_{C55e}} = \frac{1}{\frac{4}{3} \pi} 1.059 M_{E}R_{E}^{-3}$$

And we know earth would be $$\rho_{E} = \frac{1}{\frac{4}{3} \pi} M_{E}R_{E}^{-3}$$

Then we stick it into your $$r=\frac{3g}{4\pi G \rho}$$ and rearrange for: $$r\rho=\frac{3g}{4\pi G}$$ Where, in units of $R_{E}$ and $\rho_{E}$, this is equal to $\frac{3}{4\pi}$, so our new planet with density $\rho_{K52c}$ would have a radius: $$r \rho_{K52c} = r \frac{3}{4 \pi} 1.06=\frac{3}{4\pi} $$ $$r=\frac{1}{1.06} R_{E} = 6010 km$$

Not very far off the radius of earth ($6371km$), but cited as the densest known rocky planet - perhaps this will at least give some guide-lines for what is seen.

  • $\begingroup$ I guess a pure Nickel-Iron planet (density under gravity ~8g/cm³ will be a good canditate for the smallest plausible planet as specified in the question. $\endgroup$ Commented Apr 3, 2017 at 9:54
  • $\begingroup$ @jknappen are there any pure iron-nickel bodies? If so, and if Lio won't find any to use with his approach, feel free and encouraged to post that as an answer. $\endgroup$
    – Mołot
    Commented Apr 3, 2017 at 9:58
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    $\begingroup$ @Mołot At least as meteorites they occur in our solar system $\endgroup$ Commented Apr 3, 2017 at 10:06
  • $\begingroup$ @Mołot something with a history similar to Mercuries but even more abused would be a candidate. It's core is large enough that the most plausible theory for its current state is that one or more collisions with large planetesimals have stripped off most of its mantle. Bombard it more heavily and you could end up with a ball of Iron with just a veneer of lighter material on top. $\endgroup$ Commented Apr 3, 2017 at 13:09

Reasonable as in unusual but not breaking any laws of physics?

Without anything really exotic

About the size of the earths moon.

If we had a body with a core containing a really quite remarkable quantity of Gold, Tungsten, Americium, Uranium, Rhenium, Platinum, Iridium and Osmium with a thin crust of rock over the surface then the density could be in the region of 20g/cc.

A sphere with radius of about 1750 km would have a surface gravity of 9.78

This is almost exactly the radius of earths moon, it would be about 14th of earths total mass, a little heavier than mercury.

Rare-ish elements but not so rare that a big chunk couldn't be explained as an unusually pure chunk or the heaviest elements from the core of a larger destroyed body or some such.

You might want to cut out the radioactives there since it could cause super-critical complications.

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    $\begingroup$ The problem is that those heavy elements won't be in the core of a prior body. They don’t mix with iron/nickle, but do form minerals with light elements. So they are mantle loving and not separated. $\endgroup$
    – JDługosz
    Commented Apr 3, 2017 at 10:26
  • $\begingroup$ @JDługosz gold is pretty nonreactive, Iridium and Osmium are apparently not very mantle-loving. $\endgroup$
    – Murphy
    Commented Apr 3, 2017 at 15:09

A recent study [1] has found that, despite showing ostensible differences in mass and size, a considerable number of the extrasolar planets discovered so far have a surface gravity very similar to that of Earth.

Firstly, the surface gravity of the small bodies in the Solar System and rocky planets smaller than Venus grows with the square root of the mass. Secondly, in the case of gaseous giant exoplanets, the surface gravity linearly grows with the mass. And surprisingly, in the transition zone (between 1 and 100 land masses), we find some sort of plateau that shows a constant surface gravity roughly similar to that of Earth.

So, it seems to exist a correlation between mass and radius of the planets in order to sustain this plateau. So, from the figure the answer to your question is: Earth is the smallest reasonable natural planet with Earth-like surface gravity, or Venus if you want do give some concession.

enter image description here

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    $\begingroup$ Hi atMalkyor, and welcome to Worldbuilding. I see you have posted what appears to be the exact same answer on another question. While we certainly encourage newcomers to participate, it's also usually better if you tailor the answer to the specific question, even if you are referencing the same source material. $\endgroup$
    – user
    Commented Nov 12, 2017 at 18:32
  • $\begingroup$ Erm - I hesitate to say it but we are in the very early days of extra-solar planetary discovery and, while there does seem there may be a plateau of sorts, there's not a terrific sample to depend upon when looking at planets that are the size of earth - as they are not yet detectable. Likewise, super-earths - on your diagram also - show up to 7-8G, and there's lots we don't know about the rocky/gas transition. $\endgroup$
    – Konchog
    Commented Aug 29, 2019 at 7:43

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