# Best way to quantify the tidal stress on an exoplanet?

I'm trying to assess the tidal stresses different exoplanets experience during their orbits. The known parameters are usually mass $$M$$, radius $$R$$, eccentricity $$e$$, orbital period $$T$$, and semi-major axis $$a$$ (where the mass and radius of the host star are known as well). The most straightforward way I can think of is using the tidal force imposed on the surface of the planet by the star:

$$F_{tidal}= -2G\frac{M_*M_p}{\bar{r}^3}R_p$$

Where subscripts $$*$$ and $$p$$ represent the star and planet respectively. $$\bar{r}$$ is the mean distance:

$$\bar{r} = a \left( 1+ \frac{e^2}{2} \right)$$

and then dividing it by the surface area of the planet:

$$\tau_{tidal}= \frac{F_{tidal}}{4\pi r_p^2}$$

However, I'm not sure if there is a better (and more appropriate) way to estimate the tidal stress.

A solution to this problem, along with some applications, is provided in the paper The Ability of Significant Tidal Stress to Initiate Plate Tectonics'' by Zanazzi & Triaud.