Crossing of Phantom Divide Line in Model of Interacting Tsallis Holographic Dark Energy

Round 1

Reviewer 1 Report

Comments for author File: Comments.pdf

Author Response

We would like to thank referee for pointing out on our errors. These errors and some misprints are fixed. We also add some text in conclusion about coincidence problem and some references in introduction about connecting between THDE and generalized Nojiri-Odintsov HDE. 

Reviewer 2 Report

The Authors consider the model of the Universe evolution, in which the formula for the energy density of the cosmic dark energy substratum is constructed using the ideas outlined in the Tsallis Holographic Dark Energy theory. The interest of the Authors is focused on the numerical modeling of the Universe evolution. The main result is connected with the phantomization of the dark energy.

The manuscript deserves publication, but some changes are necessary.

1. On the page 2, line 56 there is the reference [36], which is absent in the List of references.
2. There are typos, e.g., see the top line of the page 3.
3. I recommend to add (e.g., into Conclusions) a paragraph about the Coincidence Problem.

Author Response

We would like to thank referee for useful comments.
1. We deleted missing ref. and also add some papers about connection between Nojiri-Odintsov generlaized HDE and Tsallis HDE. 

2. We re-read the text of the article and corrected the typos and errors which were found.

3. We add following about coincidence problem in Conclusion: 

In conclusion one need to say few words about coincidence problem in considered model. In the $\Lambda$CDM model observational fact that the present fractions of dark energy and dark matter are of the same order of magnitude shows that we are currently living in a very special period. For Tsallis HDE without interaction we also need to explain why in present epoch dark energy and matter density are close to each other. But interaction in some cases changes behaviour of relation $\rho_{de}/\rho_m$ dramatically. For a case of $C=1$ and for appropriate $d^2$ we have a quasi-de Sitter evolution but fraction of dark energy tends to $\Omega_{de}<1$ (see Fig. 2). Moreover this limit can be close to current value and therefore there is nothing surprising in the fact of $\rho_{de}/\rho_{m}\sim \mathcal{O}(1)$. Only in past $\rho_{m}>>\rho_{de}$. Even for scenario with big rip singularity in future interaction can lead to that for most of cosmological evolution $\rho_{de}/\rho_{m}\sim \mathcal{O}(1)$ (Fig. 4, case $d^2=0.2$). The same picture is repeated for quintessence-mimicked THDE with interaction (C>1).