**2. Study area**

Models of the internal structure of Enceladus reveals an ocean on average 26– 31 km in depth below an ice layer between 21 and 26 km of thickness [39]. Salinity geochemistry simulations of the ocean of Enceladus show values nearly similar to Earth, around 20 g/kg [40, 41]. The quantity of water vapor ejected from the plumes is around 150–300 kg/s [42]. This ejection of particles supply the composition of the ring E of Saturn, with <10% of the material catching into it, also suggesting a liquid origin [43, 44]. **Figure 1** shows the distribution of the plumes along the south pole of Enceladus.

#### **Figure 1.**

*Digital elevation model (DEM) of the plumes called "Tiger stripes" located in the south pole of Enceladus. It was used the images taken by the Cassini Mission. This DEM was developed using the software TopoCal 2022 v.9.0.811.*

**Figure 2.** *Elevation profile of the DEM from top to bottom.*

**Figure 3.** *Elevation profile of the DEM to the center from left to right.*

Beneath the south pole the composition of the particles is mainly salt rich, implying that those salts are larger than salt-poor grains and they are expelled with lower escape velocity. The escape speed of particles from the plumes in Enceladus is on average 1.85–2.25 km/s, according to the measures from the dusty plume by the flyby of the Cassini spacecraft [45]. **Figures 2** and **3** show the longitudinal (y axis) and transversal (x axis) height profiles of the plumes of Enceladus from **Figure 1**. The longitudinal axis of **Figure 2** presents a radius in the central plume of 190 m, besides, the transversal axis of **Figure 3** shows a radius of 90 m. The distribution of the fissures along the plumes seems to be aligned in the y axis.
