<p>Let us begin with the basics. If an exterior perturber generates the potential W, then an originally spherical planet gets distorted. Owing to this distortion, its potential acquires an increment U which is usually called the additional tidal potential or, simply, the tidal potential.</p>

<p>Now let us fix a point on the surface of the planet. Let <span class="math-container">$\gamma$</span> be the angular separation between the planetocentric vectors aimed at this point and the perturber.</p>

<p>The perturbing potential W in that point can be expanded into a series over the Legendre polynomials <span class="math-container">$P_l(\cos\gamma)$</span>. This is an almost trivial fact, see equations (9 - 11) in 
<a href="https://link.springer.com/article/10.1007%2Fs10569-009-9204-7" rel="nofollow noreferrer">https://link.springer.com/article/10.1007%2Fs10569-009-9204-7</a></p>

<p><a href="https://arxiv.org/abs/0803.3299" rel="nofollow noreferrer">https://arxiv.org/abs/0803.3299</a></p>

<p>In those equations, <span class="math-container">$r^*$</span> is the position of the perturber, while R is the surface point.</p>

<p>As it turns out, a degree-<span class="math-container">$l$</span> term in that equation contains a factor of <span class="math-container">$(R/r^*)^{l}$</span>. </p>

<p>The additional tidal potential U in that point can be expanded over the same <span class="math-container">$P_l(\cos\gamma)$</span>.</p>

<p>Moreover, you can write down the potential U in a point r located right above R (i.e., having the same angular separation from <span class="math-container">$r^*$</span> as R has).  This expansion is rendered by equation (19). In that equation, you need only the first line. Ignore the rest for now.</p>

<p>As we see from this formula, the degree-<span class="math-container">$l$</span> term of U is equal to the degree-<span class="math-container">$l$</span> term of W multiplied by <span class="math-container">$(R/r)^{l + 1}$</span> and by an additional factor <span class="math-container">$k_{l}$</span> named the degree-<span class="math-container">$l$</span> Love number.</p>

<p>Derivation of this formula is boring. It is a solution to a boundary-value problem for an elastic medium, and the factors <span class="math-container">$k_{l}$</span> emerge as some functions of the shear elastic modulus of the material of which the planet is composed.</p>

<p>This is how it is for static tides. In real life we, of course, have tides evolving in time, and all this machinery has to be generalised. We have to expand both W and U into Fourier harmonics and to write down all this formalism for each harmonic separately.
Then you get different lags for different harmonics involved. Also, the dynamical analogues of the Love numbers will be functions of other rheological parameters (like the viscosity).  However, the central idea will be more or less the same.  I can give you more references, if you are interested.</p>

<p>Jérémy Leconte in his work tried to substitute the degree-2 part of U with an equivalent potential generated by two equal masses located oppositely. You can think of this as two tidal bulges approximated with point masses. This was done for illustrative purposes solely and, in my opinion, bears no practical value.   </p>

CC BY-SA 4.0
2019-10-22T08:02:11.043Z
2019-10-22T08:02:11.043Z
Michael_1812
<p>My question refers to page 165 of <a href="https://tel.archives-ouvertes.fr/tel-00707629v2/document" rel="nofollow noreferrer">this paper</a>. Specifically, how does one derive the equation <span class="math-container">$\delta m = \frac{1}{2}k_2M_2\lbrace\frac{R_1}{r_\star}\rbrace^3$</span> for the mass of a tidal bulge? A full derivation would be much appreciated, and also an explanation as to where Love's number <span class="math-container">$k_2$</span> comes from. </p>

CC BY-SA 4.0
2019-10-05T07:03:29.193Z
`+1` I'd *love* to see an answer that explained Love's numbers! They show up in many answers (usually DH's) but I haven't a clue what they are!
uhoh
CC BY-SA 4.0
2019-10-05T09:34:22.993Z
Without any level of rigour it seems a kind of elasticity. Something like that. Being all amounts equal we get not bulge with k = 0. Higher value would be a less rigid planet. Though it should be a kind of volumetric costant and density cancel somewhere during derivation. Just a hint waiting for answer. But I see it as a force constant of a volumetric spring.
Alchimista
CC BY-SA 4.0
2019-10-05T22:35:01.533Z
Yes, that was my initial thought. Though this is more of an analogy and when learning something new I usually like to read outside of the literature to see the intuition behind how these things work. I'm still looking for an answer, as I still haven't found a helpful explanation online.
wrb98
CC BY-SA 4.0
2019-10-06T08:26:04.867Z
Pdf crashes . There should be a reference there. Check it again. It would be strange if they place that in a thesis out of black.
Alchimista
CC BY-SA 4.0
2019-10-06T17:35:05.617Z
Works fine for me. You could try a different browser or paste the address into google
wrb98
CC BY-SA 4.0
2019-10-07T00:34:08.837Z
@Alchimista I can load the pdf from anywhere, it's not paywalled at least. Can you see the referring page https://tel.archives-ouvertes.fr/tel-00707629v2 and then click the link to the pdf (red button, also one on the right)?
uhoh
CC BY-SA 4.0
2019-10-07T21:00:47.767Z
Can anyone provide an answer to the question? I've started a bounty.
wrb98
CC BY-SA 4.0
2019-10-11T03:04:43.910Z
Love's numbers: https://en.wikipedia.org/wiki/Love_number. The Love numbers h, k, and l are dimensionless parameters that measure the rigidity of a planetary body and the susceptibility of its shape to change in response to a tidal potential.
Natsfan
<astrophysics><binary-star><tidal-locking><tidal-forces>
Where does Love's number come from in $\delta m = \frac{1}{2}k_2M_2\lbrace\frac{R_1}{r_\star}\rbrace^3$, the formula for the mass of a tidal bulge?
wrb98
# Where does Love's number come from in $\delta m = \frac{1}{2}k_2M_2\lbrace\frac{R_1}{r_\star}\rbrace^3$, the formula for the mass of a tidal bulge?

(Asked by: username_0 on 2019-10-04)

My question refers to page 165 of [this paper](https://tel.archives-ouvertes.fr/tel-00707629v2/document). Specifically, how does one derive the equation $\delta m = \frac{1}{2}k\_2M\_2\lbrace\frac{R\_1}{r\_\star}\rbrace^3$ for the mass of a tidal bulge? A full derivation would be much appreciated, and also an explanation as to where Love's number $k\_2$ comes from.

**Tags:** astrophysics, binary-star, tidal-locking, tidal-forces

> **Comments:**
> **username_1**: `+1` I'd *love* to see an answer that explained Love's numbers! They show up in many answers (usually DH's) but I haven't a clue what they are!  
> **username_2**: Without any level of rigour it seems a kind of elasticity. Something like that. Being all amounts equal we get not bulge with k = 0. Higher value would be a less rigid planet. Though it should be a kind of volumetric costant and density cancel somewhere during derivation. Just a hint waiting for answer. But I see it as a force constant of a volumetric spring.  
> **username_0**: Yes, that was my initial thought. Though this is more of an analogy and when learning something new I usually like to read outside of the literature to see the intuition behind how these things work. I'm still looking for an answer, as I still haven't found a helpful explanation online.  
> **username_2**: Pdf crashes . There should be a reference there. Check it again. It would be strange if they place that in a thesis out of black.  
> **username_0**: Works fine for me. You could try a different browser or paste the address into google  
> **username_1**: @username_2 I can load the pdf from anywhere, it's not paywalled at least. Can you see the referring page https://tel.archives-ouvertes.fr/tel-00707629v2 and then click the link to the pdf (red button, also one on the right)?  
> **username_0**: Can anyone provide an answer to the question? I've started a bounty.  
> **username_3**: Love's numbers: https://en.wikipedia.org/wiki/Love_number. The Love numbers h, k, and l are dimensionless parameters that measure the rigidity of a planetary body and the susceptibility of its shape to change in response to a tidal potential.  

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## 1 answers

### Answer by username_4 on 2019-10-22. Score: 4

Let us begin with the basics. If an exterior perturber generates the potential W, then an originally spherical planet gets distorted. Owing to this distortion, its potential acquires an increment U which is usually called the additional tidal potential or, simply, the tidal potential.

Now let us fix a point on the surface of the planet. Let $\gamma$ be the angular separation between the planetocentric vectors aimed at this point and the perturber.

The perturbing potential W in that point can be expanded into a series over the Legendre polynomials $P\_l(\cos\gamma)$. This is an almost trivial fact, see equations (9 - 11) in
<https://link.springer.com/article/10.1007%2Fs10569-009-9204-7>

<https://arxiv.org/abs/0803.3299>

In those equations, $r^\*$ is the position of the perturber, while R is the surface point.

As it turns out, a degree-$l$ term in that equation contains a factor of $(R/r^\*)^{l}$.

The additional tidal potential U in that point can be expanded over the same $P\_l(\cos\gamma)$.

Moreover, you can write down the potential U in a point r located right above R (i.e., having the same angular separation from $r^\*$ as R has). This expansion is rendered by equation (19). In that equation, you need only the first line. Ignore the rest for now.

As we see from this formula, the degree-$l$ term of U is equal to the degree-$l$ term of W multiplied by $(R/r)^{l + 1}$ and by an additional factor $k\_{l}$ named the degree-$l$ Love number.

Derivation of this formula is boring. It is a solution to a boundary-value problem for an elastic medium, and the factors $k\_{l}$ emerge as some functions of the shear elastic modulus of the material of which the planet is composed.

This is how it is for static tides. In real life we, of course, have tides evolving in time, and all this machinery has to be generalised. We have to expand both W and U into Fourier harmonics and to write down all this formalism for each harmonic separately.
Then you get different lags for different harmonics involved. Also, the dynamical analogues of the Love numbers will be functions of other rheological parameters (like the viscosity). However, the central idea will be more or less the same. I can give you more references, if you are interested.

Jérémy Leconte in his work tried to substitute the degree-2 part of U with an equivalent potential generated by two equal masses located oppositely. You can think of this as two tidal bulges approximated with point masses. This was done for illustrative purposes solely and, in my opinion, bears no practical value.


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