Do any of the planets have a Roche limit that is strong enough to be felt by an astronaut whilst in orbit?


Roche limit happens where the gravity of the object, trying to pull the object together, becomes smaller than the tidal force (trying to pull the object apart).

But the astronaut is bound by not gravity, rather by the electromagnetic interaction between his/her atoms. The own gravity of the astronaut is negligible, compared to the electromagnetic interaction.

However, the tidal force affecting an astronaut, should require a little calculation. We can derive the formula of the gravitational acceleration around a point-like body ($F=\frac{GM}{r^2}$), we get


(We can ignore the sign on obvious reasons.)

Here $G$ is the gravitational constant, $M$ is the mass of the body, and $r$ is the distance.

Substituting the values of the Sun, we get $\frac{2\cdot 6.67 \cdot 10^{-11} \cdot 2 \cdot 10^{30}}{(7\cdot 10^8)^3} \approx 7.78\cdot 10^{-7} \frac{\mathrm{m/s^2}}{\mathrm{m}} \approx \underline{\underline{8 \cdot 10^{-8} \frac{g}{\mathrm{m}}}}$.

More clearly, if we are orbiting the Sun just above its surface, a roughly 2m long astronaut feel that his head and foot are pulled apart by around $1.6\cdot 10^{-7}g$ weight. In the case of a $70\:\mathrm{kg}$ astronaut, it is around the weight of $0.0112$ gram on the Earth.

The astronaut wouldn't feel it, but not very sensitive sensors could already measure it.

This calculation sometimes used $\mathrm{g}$ for "gram", as unit of mass, and $g$ as the (non-standard) unit of acceleration.

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    $\begingroup$ Ignoring the obvious fact that any astronaut or instrument that close to the sun would be instantly vaporized of course... $\endgroup$ – Darrel Hoffman Jul 14 '18 at 17:01
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    $\begingroup$ @DarrelHoffman The Sun gives $\approx$ 6000K thermal radiation, which is hard but not chanceless to protect against it. I think some strong defense, for example well-polished tungsten mirrors, maybe combined with some cooling from behind, could handle it. The Parker Solar Probe will near the Sun to 8 solar radii. $\endgroup$ – peterh Jul 15 '18 at 14:00

The Roche limit is where the tidal forces exerted on an orbiting object are sufficient to overcome the self-gravity of that object.

The "self-gravity" of an astronaut is tiny. We can estimate it as something like $\sim GM^2/4h^2$, where $M$ is the mass of the astronaut (+ equipment) and $h$ is their size (height). Assuming $M=100$ kg and $h=2$ m, then the self-gravity all force is $4\times 10^{-8}$ N. This is a force that is too small to feel.

The problem with this calculation is that astronauts are not held together by self-gravity and a tidal field at the Roche limit has a negligible effect on a small body that is actually held together by atomic forces.

In order to experience a tidal field that can be felt on astronaut scales, let's say larger than 10 N (imagine hanging a 1 kg weight from your ankle on Earth), you would have to get much closer to the source of gravity.

The tidal field scales as $m/r^3$, where $m$ is now the mass of the massive body and $r$ is your distance from its centre. Assuming a fixed mass, then you would need to get about 600 times closer than the Roche limit in order to feel the tidal force. For solar system bodies (including the Sun and Jupiter) this would put you well inside that body, which isn't possible and in any case we could not assume that $m$ was fixed in that case, because it is the mass interior to $r$ that counts.

The only way that an astronaut could "feel" a tidal force would be to approach a compact star - a high density neutron star, white dwarf or black hole. There you can generate a very strong tidal field and, because they are compact, an astronaut could get close enough to feel it.


Expanding on Peterh's answer, we could try to find how should be an astronomical object for the tidal forces be felt by an astronaut orbiting it.

I don't have any reliable data on how strong need the tidal force to be felt. However, with a big simplification, we can very roughly model the upper and lower body of an astronaut as two masses placed about 1 meter apart. For a 70 kg astronaut under a tidal force of $0.1·g$ per meter (where $g$ is the acceleration of gravity), the difference of pull between those two 35 kg masses would be $0.1·35 kg = 3.5 kg$. Those force would stretch the astronaut's waist and would be clearly noticeably (maybe a force ten times weaker would be noticeable, too, but I'll will stick to $0.1m^{-1}·g$).

From Peterh's formulas:


For a 1 solar mass object:

$$r=\sqrt[3]{\frac{2·6.67·10^{-11}·2·10^{30}}{0.1·g}}=6481168 m = 6481 km$$

That an astronaut orbiting a sun-sized mass at a distance similar to Earth's radius, would clearly feel tide forces when their head or feet point to the object. Of course the object would need to be a black hole or a neutron star to fit inside of the orbit.

With a more massive object the orbit could be larger, but given that mass is inside a cubic root, radius would grow very slowly.

  • $\begingroup$ You don't need a black hole for this. A neutron star is quite enough (typical mass: one solar mass, typical radius: 10 km). $\endgroup$ – Martin Bonner Jul 15 '18 at 9:35
  • $\begingroup$ @MartinBonner Thank you. Neutron stars added. $\endgroup$ – Pere Jul 15 '18 at 9:44
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    $\begingroup$ Might also refer to Niven's Neutron Star $\endgroup$ – DJohnM Jul 15 '18 at 15:52
  • $\begingroup$ @DJohnM ack you ninja'd me. Sorry for posting my comment against the OP $\endgroup$ – Carl Witthoft Jul 16 '18 at 17:55
  • $\begingroup$ @DJohnM I don't understand the reference to the Niven's Neutron Star? $\endgroup$ – Muze Jul 17 '18 at 4:14

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