<p>Gaseous planets would tidally lock, just as binary stars do.  That would occur in addition to convection-- tidal effects are weak and operate on very long timescales, convection is strong and operates on much shorter timescales.  It is true that a gaseous planet conforms more easily to the tidal potential even if it is rotating, so there is less of a turning of the tidal bulges, but the tidal bulges are larger because they fill the equipotential, whereas solid surfaces don't.  So the rapid response of gas could make the locking process either faster or slower, depending on which effect dominates.  But you are probably right to focus on energy dissipation as the key requirement, and gas is probably less dissipative, so I would guess the locking time is longer for gas.  Still, there is energy dissipation, there is a delay as the gas flows, and there is a tidal locking effect, all going on on timescales much slower than convection.</p>

CC BY-SA 3.0
2016-12-02T12:11:45.753Z
So if I understand correctly, both the two processes are not mutually exclusive. This implies that there is a certain region within the planet that does mostly obey tidal locking, in addition to a region that is overpowered by convection. My guess then is that the tidal locking begins at the core of the planet, and slowly grows outward until it reaches a stable balance point where convection becomes the dominant mechanism driving the planet's motion.
Ryan Franz
CC BY-SA 3.0
2016-12-02T14:59:54.083Z
I'd say it's better not to think of locking and convection as either/or that are in competition, but rather two independent processes going on over different timescales.  It's like the orbit of the Moon around the Earth-- the gravity of the Sun imposes an orbit around the Sun over the year, and the gravity of the Earth imposes an orbit around the Earth over each month.  The two processes don't compete, they simply occur hand-in-hand.
Ken G
CC BY-SA 3.0
2016-12-02T20:25:07.280Z
That makes sense physically, but it makes me question how we define "tide lock". I had imagined tidal locking as "always showing one face towards the center of rotation." That's not true if convection is moving parts of the planet around. If gaseous objects can be tide locked, I guess it must mean "the average gas molecule travels once around the planet per orbital period of the planet." Though I'm not sure how we could measure a property like that in a practical manner.
Ryan Franz
CC BY-SA 3.0
2016-12-02T21:56:02.237Z
Yes, you are right that it is nontrivial to define the rotation period of gas giants!  Even for the Sun, it's not so obvious what is meant by the rotation period, exactly.
Ken G
CC BY-SA 3.0
2016-12-01T15:44:11.210Z
2016-12-01T15:44:11.210Z
Ken G
<p>Supposing a planet is made entirely of gas, is it possible for the planet to become tidally locked with the star it orbits? </p>

<p>I know when a terrestrial planet orbits a star in a different amount of time than the length of its day, the planet warps continuously, resulting in tidal heating. This heating takes energy from the planet's rotation until it stabilizes in a tide-locked formation. </p>

<p>I believe a purely gaseous planet would also have some sort of internal heating for the same reason. But because the "surface" of a gas planet is fluid, it must also obey thermodynamic principles.</p>

<p>As a basic example, the side of the planet facing a star gets hot, and the side facing away gets cold. The hot gas expands and the cold gas contracts and you get convection, Hadley cycles, prevailing winds, and chaotic weather patterns.</p>

<p>So it seems like there's a battle between gravity, which wants the gas to stop moving and become tide-locked, and thermodynamics, which wants the surface to roil with convection.</p>

<p>Does one process dominate over the other? Does one process slowly take over as the other fades away? Can it go either way?</p>

<star><planet><orbit><gravity>
How can a gas planet become tidally locked with a star?
Ryan Franz
# How can a gas planet become tidally locked with a star?

(Asked by: username_0 on 2016-12-01)

Supposing a planet is made entirely of gas, is it possible for the planet to become tidally locked with the star it orbits?

I know when a terrestrial planet orbits a star in a different amount of time than the length of its day, the planet warps continuously, resulting in tidal heating. This heating takes energy from the planet's rotation until it stabilizes in a tide-locked formation.

I believe a purely gaseous planet would also have some sort of internal heating for the same reason. But because the "surface" of a gas planet is fluid, it must also obey thermodynamic principles.

As a basic example, the side of the planet facing a star gets hot, and the side facing away gets cold. The hot gas expands and the cold gas contracts and you get convection, Hadley cycles, prevailing winds, and chaotic weather patterns.

So it seems like there's a battle between gravity, which wants the gas to stop moving and become tide-locked, and thermodynamics, which wants the surface to roil with convection.

Does one process dominate over the other? Does one process slowly take over as the other fades away? Can it go either way?

**Tags:** star, planet, orbit, gravity


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## 1 answers

### Answer by username_1 on 2016-12-01. Score: 3 | Accepted answer

Gaseous planets would tidally lock, just as binary stars do. That would occur in addition to convection-- tidal effects are weak and operate on very long timescales, convection is strong and operates on much shorter timescales. It is true that a gaseous planet conforms more easily to the tidal potential even if it is rotating, so there is less of a turning of the tidal bulges, but the tidal bulges are larger because they fill the equipotential, whereas solid surfaces don't. So the rapid response of gas could make the locking process either faster or slower, depending on which effect dominates. But you are probably right to focus on energy dissipation as the key requirement, and gas is probably less dissipative, so I would guess the locking time is longer for gas. Still, there is energy dissipation, there is a delay as the gas flows, and there is a tidal locking effect, all going on on timescales much slower than convection.

> **Comments:**
> **username_0**: So if I understand correctly, both the two processes are not mutually exclusive. This implies that there is a certain region within the planet that does mostly obey tidal locking, in addition to a region that is overpowered by convection. My guess then is that the tidal locking begins at the core of the planet, and slowly grows outward until it reaches a stable balance point where convection becomes the dominant mechanism driving the planet's motion.  
> **username_1**: I'd say it's better not to think of locking and convection as either/or that are in competition, but rather two independent processes going on over different timescales.  It's like the orbit of the Moon around the Earth-- the gravity of the Sun imposes an orbit around the Sun over the year, and the gravity of the Earth imposes an orbit around the Earth over each month.  The two processes don't compete, they simply occur hand-in-hand.  
> **username_0**: That makes sense physically, but it makes me question how we define "tide lock". I had imagined tidal locking as "always showing one face towards the center of rotation." That's not true if convection is moving parts of the planet around. If gaseous objects can be tide locked, I guess it must mean "the average gas molecule travels once around the planet per orbital period of the planet." Though I'm not sure how we could measure a property like that in a practical manner.  
> **username_1**: Yes, you are right that it is nontrivial to define the rotation period of gas giants!  Even for the Sun, it's not so obvious what is meant by the rotation period, exactly.  

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