Energy Conditions in Symmetric Teleparallel Gravity
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| Number of Parts | 43 | |
| Author | 0000-0003-2570-2335 (ORCID) | |
| Contributors | 0000-0003-2570-2335 (ORCID) | |
| License | CC Attribution 3.0 Germany: You are free to use, adapt and copy, distribute and transmit the work or content in adapted or unchanged form for any legal purpose as long as the work is attributed to the author in the manner specified by the author or licensor. | |
| Identifiers | 10.5446/49861 (DOI) | |
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| Producer | 0000-0003-2570-2335 (ORCID) | |
| Production Year | 2020 | |
| Production Place | Hyderabad |
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Transcript: English(auto-generated)
00:02
Hello everyone, this is Sanjay Mandal from Department of Mathematics of Birla Institute of Technology and Science, Hyderabad, India. So, firstly, I would like to thank the organizers of International Selection of Physics 2020 for giving us an opportunity to present our work.
00:23
Now, I am going to talk about on the topic, Energy Conditions in Symmetric Telephoral Gravity. As we know so far, the Einstein theory of relativity was a successful theory. And it has also passed so many observations like LIGO, Virgo and the Blackwell image from the Event Horizon telescopes.
00:46
And it was a very fundamental and successful theory so far. Also, besides this, there are some alternative theories like Teleparallel Gravity and Symmetric Teleparallel Gravity. Here, in this paper, we have studied the Symmetric Teleparallel Gravity and we basically focused on its energy condition.
01:07
And it has come to the motion equation. We have taken the action as presented in equation 1 also. We have taken the perfect fluid for the matter and the FLRW matrix. And for this FLRW matrix and the non-matricity term Q, which represents the
01:27
motion equations in symmetric teleparallel gravity, which takes Q is equal to 6h square. And using equation 1, 2 and 3, we got the motion equations 4 and 5. And again, we reorder 4 and 5 in analogy with Zr.
01:44
We got the 3h square is equal to here, rho, delta and phi delta represent the effective pressure and density of our model. And as we know, energy condition is an important tool to study the time-like space-like and the light-like behaviour of our universe.
02:07
And in order to study the energy condition, first we found the weak energy condition, non-energy condition and dominant energy condition using the G-standard G-air condition. And we got the, and collaborating with the work of Capecillo, we found the strong energy condition as shown in equation 10.
02:27
As we know, the cosmological parameters such as Hubble parameter and deceleration parameter, jerk parameter, snack parameter can be written like this. And also, we using equation 11, we reorder it into S dot and S double dot.
02:44
And from using 12 and 13, we found the expression for all the energy condition like strong energy condition, non-energy, weak energy and dominant energy condition. After that, in order to study some cosmological model, we have taken the first case as an algebraic function of Q.
03:04
And then, in order to constrain the model parameters M and we have taken here the present observational values of S dot and Q dot from flying data and another paper. As you can see here, energy density, weak energy condition, dominant energy condition satisfied whereas the strong energy condition violated.
03:26
And which is represent and which is an agreement with the present scenario of our universe. For our second model, we have taken Fq as a logarithmic function and you can see in this paper which is published in Physically Review recently.
03:43
And in order to compare our model with lambda CDM model, here we have compared and as you can know the Fq is equal to minus Q represent the lambda CDM model and here we have expressed the energy condition. If one can see this, if you will put the present value of Hubble parameter and
04:05
deceleration parameter at that stage, the strong energy condition will violate and another will be satisfied. And also, this is an agreement with our, like our model is satisfied the lambda CDM model. And as you can see, know the Planck collaboration and lambda CDM model present the present
04:27
cosmological scenario with the value of equation of state parameter as omega nearly equal to minus one. Here also, we have presented our omega for our model. As you can see, it is very nearly close to minus one and slightly deviated because of its modification.
04:46
And here we have found some conclusions like we have constrained the model parameters Mn against the observational data which shows the accelerator expansion of the universe and it is compactable with the lambda CDM as well as the observational data.
05:03
And this result allows us to evaluate the different familiar of Q models. And here are some references and thank you so much for your kind attention.