$\rho_{2}\left(\mathbf{r}\right)$ are the two mass distributions, one for each different mass eigenstate. Since these two distributions travel at different velocities, $\triangle E_{G}^{j,k}$ has a dependence on the traveled distance $L'$ (see Eq. (14) of [@Ch]). Following the computation done in [@Ch] and keeping all constants explicit, one finds: $$\Lambda_{G}^{j,k}\simeq8\pi \frac{G}{\hbar c}\left[\frac{3\left(m_{j}+m_{k}\right)\hbar^{2}}{5G_{F}}-\frac{m_{j}m_{k}E}{2\pi\hbar c}\ln\left(\frac{6\left(m_{j}+m_{k}\right)\pi\hbar^{3}c}{5m_{j}m_{k}G_{F}E}\right)\right]L$$ where $G_{F}$ is the Fermi constant and $m_{j}, m_k$ are the neutrino masses. In the case of cosmogenic neutrinos which have an energy of about $E=10^{19}$eV and travel a distance $L\simeq10^{25}$m, the magnitude of the damping factor $\Lambda_G^{j,k}$ lies between 1 and $10^{-2}$, depending on the mass of the neutrino. Therefore, for the Diosi-Penrose model damping effect is by far stronger than that computed with the CSL model. This does not come as a surprise, because—as we stated in the introduction—it is well known that the model predicts, for single elementary constituents, a too-strong collapse of the wave function, which is incompatible with known experimental data [@Gpd]. The reason is the following. It is clear that the model gives rise to divergences in the point-like limit, therefore one has to introduce a cutoff [@Dg2]. One way of doing it, is to consider elementary particles as spherical mass-distributions with 