Anisotropic Quark Stars with an Interacting Quark Equation of State within the Complexity Factor Formalism

Round 1

Reviewer 1 Report

The paper is interesting but I rathere see it as a mathematical exercise with small relevance  for observations. I think that the paper can pbe published after introducing some changes. 

These are:

1. A more in depth discussion of the physical examples of anisotropic pressure matter.

2. In section 4 we see what is the value of P_r used but what is os P_\perp. This should be rpresented in detail

3. IN section 4 a mre detailed discussion is needed with specific relation and pointing to Figures. As I see it now it is a loose discussion and it is difficult to understand. 

4. Last but not least. When considering solutions of stars and claiming their realty is is of utmost importane to discuss the stability of the solutions. The authors should show whether the solutions are stable at least to radial perturbations. The existence of perprendicular pressure also begs for non radial y by this may be too much for this exploratory work. 

 

Author Response

We wish to thank the reviewer for valuable comments and suggestions. Our response is included as a separate file.

Author Response File: Author Response.pdf

Reviewer 2 Report

  The report on paper entitled  “Anisotropic quark stars with an interacting quark equation of state within the complexity factor formalism”  by Ángel Rincón , Grigoris Panotopoulos, Ilídio Lopes         

                          

The paper considers an effect of anisotropies in an ultra-dense quark matter on structure of strange quark stars . The mass-to-radius relationships are obtained by making use of the complexity formalism and a certain form for the anisotropic factor. The results are well compared to another more conventional approaches.  

I can recommend publication after minor corrections.

In particular.

In line 26 “formed during the final stages of stellar evolution”

It is worthy to mention the type of SN explosion and expected mass of progenitor.   

The equation-of-state can be also affected by, e.g., stellar magnetic fields (Kondratyev, Universe, 2021; 7, 487) as well. Such phenomena should be also discussed.

Author Response

We wish to thank the reviewer for useful comments and suggestions. Our response is included as a separate file.

Author Response File: Author Response.pdf

Reviewer 3 Report

In this manuscript, the authors numerically obtained solutions of generalized TOV equation for anisotropic quark matter with EOS (39) under the constraint (38) which comes from the vanishing complexity condition. It is interesting. However, before I recommend it for publication, some points should be addressed:

1)   The problem is a boundary value problem with boundary conditions (20)-(22), However, the authors say In the abstract, that they “integrate the structure equations numerically imposing appropriate initial conditions at the center of the stars”.  why? Is there any other free parameters?

2)   I don’t think it do a good comparison between the results from the two approaches with the figures at present form.  It will be better to incorporate the lines into one figure.

3)   In the figures, R seems to represent the radius of the surface of the star. However, in Line 111, the radius has already be denoted by r_{\Sigma}. They should be consistent.

4)   In Line 111, what does "cte" mean?

5)   Line 143，is it true that {Y，Z， X} is a set of scalars?  

6)   In Figure 2, why are there 4 lines in the left panel? 

 

 

Author Response

We wish to thank the reviewer for valuable comments and suggestions. Our response is included as a separate file.

Author Response File: Author Response.pdf

Round 2

Reviewer 1 Report

Thank you very much for your changes. 

The paper is now ready to be published.