Deriving the Roche limit(d) for body of mass M and satellite m

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So i recently studied some basic gravitation and tried deriving the roche limit(d) for body of mass M and satellite m but when i used the custom formula to get the roche limit of earth and moon , i was off by 195 km , is that normal or is my formula incorrect or is it because newtonian gravity becomes inaccurate at planetary scale?
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1. It's definitely not a problem with Newtonian gravity. In the planetary regime it's completely kosher.
2. Are you comparing your result with the value that used to be on Wikipedia (as this page does: https://www.astronomicalreturns.com/2021/06/roche-limit-radius-of-disintegration.html)? It's not there any longer, as isn't their derivation, and I don't feel like dredging the edit history as to why. But I it was divergent from what you can find elsewhere (e.g. Zelik & Gregory, Astronomy and Astrophysics, similar derivation here: https://www.astro.umd.edu/~hamilton/ASTR630/handouts/RocheLimit.pdf) - it had a 2 under a cube root in one place, instead of 3, giving too low a value. Possibly because it ignored orbital motion, but it's just a guess. You ignore that too, but it's not the main issue.
3. Even using the ex-Wiki value, you're not off by 195 km, you're off by 195km-6370km. Your d is distance above Earth's surface, not the distance from the centre that the ~9500 km indicates.
4. If I see correctly what you did there, the mistake in the derivation is that you've set up the initial equation for where the gravity between the two bodies is equal. This is not the condition for disintegration, as the satellite can very well be accelerated in its entirety by such gravitational potential and not suffer for it, as long as it's done uniformly. You need to set up the equation by comparing the tidal forces on the edge of the satellite to its self-gravity. Check the references above for example derivations.
 
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Bandersnatch said:
1. It's definitely not a problem with Newtonian gravity. In the planetary regime it's completely kosher.
2. Are you comparing your result with the value that used to be on Wikipedia (as this page does: https://www.astronomicalreturns.com/2021/06/roche-limit-radius-of-disintegration.html)? It's not there any longer, as isn't their derivation, and I don't feel like dredging the edit history as to why. But I it was divergent from what you can find elsewhere (e.g. Zelik & Gregory, Astronomy and Astrophysics, similar derivation here: https://www.astro.umd.edu/~hamilton/ASTR630/handouts/RocheLimit.pdf) - it had a 2 under a cube root in one place, instead of 3, giving too low a value. Possibly because it ignored orbital motion, but it's just a guess. You ignore that too, but it's not the main issue.
3. Even using the ex-Wiki value, you're not off by 195 km, you're off by 195km-6370km. Your d is distance above Earth's surface, not the distance from the centre that the ~9500 km indicates.
4. If I see correctly what you did there, the mistake in the derivation is that you've set up the initial equation for where the gravity between the two bodies is equal. This is not the condition for disintegration, as the satellite can very well be accelerated in its entirety by such gravitational potential and not suffer for it, as long as it's done uniformly. You need to set up the equation by comparing the tidal forces on the edge of the satellite to its self-gravity. Check the references above for example derivations.
Hmm it seems i need to study more , i am in high school still so i am not aware of calculations and formulae regarding tidal forces but ill try to understand that. Also wasnt aware of wiki article , i just spontaneously decided to do it without any previous references .
 
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My comment about the Wiki was just me trying to track down where you got the ~9500km number from, that you were comparing your own result to. I should have just asked you instead of playing detective.

BTW, you don't need to learn anything more than what you used in your attempt to follow what's being done (check that second link). It's pretty much just a matter of setting up the forces properly, followed by some algebra.
 
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Oh i got that 9500 number from google and some pdf by nasa if i remember it was like 9496 km or something.I saw the Rochelimit pdf and it helped a lot i was not using it correctly enough sorry👍
 
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FAQ: Deriving the Roche limit(d) for body of mass M and satellite m

What is the Roche limit?

The Roche limit is the minimum distance at which a celestial body, such as a moon or satellite, can approach a larger body, like a planet, without being torn apart by the larger body's tidal forces. It is a critical concept in astrophysics, particularly in understanding the formation and stability of rings and moons around planets.

How is the Roche limit derived?

The Roche limit can be derived using the balance of gravitational forces and tidal forces acting on the smaller body. The formula for the Roche limit (d) is given by d = R (2(M/m))^(1/3), where R is the radius of the larger body, M is its mass, and m is the mass of the smaller body. This derivation considers the gravitational attraction of the larger body and the differential gravitational force experienced by the smaller body due to its size.

What factors influence the Roche limit?

The Roche limit is influenced by several factors, including the densities of both the larger body and the smaller body, as well as their masses. A denser larger body will have a smaller Roche limit, while a less dense smaller body will have a larger Roche limit. Additionally, the shape and structural integrity of the smaller body can affect how it responds to tidal forces.

What happens if a satellite crosses the Roche limit?

If a satellite crosses the Roche limit, it may experience significant tidal forces that can lead to its disintegration. The gravitational pull from the larger body can create stresses that exceed the structural integrity of the smaller body, resulting in fragmentation and potentially forming rings or debris around the larger body.

Are there exceptions to the Roche limit?

Yes, there are exceptions to the Roche limit. Some bodies may be able to survive within the Roche limit if they are sufficiently strong or cohesive, such as solid, rocky bodies. Additionally, the Roche limit is also affected by the rotation of the smaller body and other forces, such as radiation pressure or interactions with other celestial bodies, which can alter its stability and behavior.

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