Krishna P. B.
Current Organizations / Institutes
The organizations/institutes from the scholar's latest article
Research Subjects
Krishna P. B. has a total of 11 co-authors. Here are the top co-authors by number of shared publications:
- Titus K. Mathew
Cochin University of Science and Technology
20 shared publications - Hassan Basari V. T.
Department of Physics Cochin University of Science and Technology 682022 Kochi Kerala India
6 shared publications - M. Mahith2 shared publications
- Priyesh K. V.
Department of Physics, St. Paul’s College, Kalamasseri, Kochi-03, India
2 shared publications - Adithya P S
South Australia
1 shared publication Adithya P․s․
1 shared publication
Latest Publications
- 20 August 2026
- Published by IOP Publishing in Classical and Quantum Gravity
- Vol. 43 (16) , 165008
Emergence of cosmic space, horizon thermodynamics and the fluctuations in horizon energy in the brane world scenarios
Expansion of the Universe can be interpreted as a tendency for achieving the holographic equipartition. This principle, the law of emergence, first postulated in the context of Einstein’s gravity has been extended successfully to more general gravity theories like Gauss–Bonnet and Lovelock gravity. We derive the law of emergence for brane world models of gravity, starting from the more fundamental and well established principle, the first law of thermodynamics. More specifically, we derive the law of emergence in the context of RS II brane world, warped Dvali, Gabadadze and Porrati model and Gauss–Bonnet brane world model, with the help of corresponding Friedmann equations. We further show that the law of emergence leads to the maximization of horizon entropy in all these brane world models. Our results suggest that the horizon thermodynamics is the backbone of the law of emergence in the brane world scenarios. Following this, we analyze the evolution of the horizon energy fluctuations in the context of brane world gravity. Interestingly, the fluctuations in horizon energy attain a constant value in the long run, when ω = − 1 , which corresponds to an equilibrium state of maximum entropy.
- 20 August 2026
- Published by IOP Publishing in Classical and Quantum Gravity
- Vol. 43 (16) , 165008
Emergence of cosmic space, horizon thermodynamics and the fluctuations in horizon energy in the brane world scenarios
Expansion of the Universe can be interpreted as a tendency for achieving the holographic equipartition. This principle, the law of emergence, first postulated in the context of Einstein’s gravity has been extended successfully to more general gravity theories like Gauss–Bonnet and Lovelock gravity. We derive the law of emergence for brane world models of gravity, starting from the more fundamental and well established principle, the first law of thermodynamics. More specifically, we derive the law of emergence in the context of RS II brane world, warped Dvali, Gabadadze and Porrati model and Gauss–Bonnet brane world model, with the help of corresponding Friedmann equations. We further show that the law of emergence leads to the maximization of horizon entropy in all these brane world models. Our results suggest that the horizon thermodynamics is the backbone of the law of emergence in the brane world scenarios. Following this, we analyze the evolution of the horizon energy fluctuations in the context of brane world gravity. Interestingly, the fluctuations in horizon energy attain a constant value in the long run, when ω = − 1 , which corresponds to an equilibrium state of maximum entropy.
- 16 January 2026
- Published by Elsevier in Physics of the Dark Universe
- Vol. 51
Evolution of fluctuations in horizon energy and its dependence on the degrees of freedom
- 16 January 2026
- Published by Elsevier in Physics of the Dark Universe
- Vol. 51
Evolution of fluctuations in horizon energy and its dependence on the degrees of freedom
- 20 February 2024
- Published by Elsevier in Physics of the Dark Universe
- Vol. 44
Emergence of cosmic space and the maximization of horizon entropy
- 20 February 2024
- Published by Elsevier in Physics of the Dark Universe
- Vol. 44
Emergence of cosmic space and the maximization of horizon entropy
- 8 March 2023
- Published by American Physical Society (APS) in Physical Review D
- Vol. 107 (6) , 063511
Unified formalism for the law of emergence from the first law of thermodynamics
We derive a unified expansion law for our Universe from the first law of thermodynamics on the apparent horizon, where entropic evolution depicts the emergence of cosmic space. The derivation advances a general form for degrees of freedom on the surface and bulk, which provides a natural generalization for the expansion law proposed by Padmanabhan. The general expression for the surface degrees of freedom differs from the natural expectation, in the emergent gravity paradigm for general theories of gravity. The derivation also provides justification for the selection of Gibbons-Hawking temperature in the original expansion law and for the use of areal volume in the nonflat Friedmann-Robertson-Walker universe. Since the unified expansion law exclusively depends on the form of entropy, the method is applicable to obtain the expansion law in any gravity theory without any additional ad hoc assumptions. From the general expansion law, we have obtained the expansion law corresponding to different theories of gravity like () Einstein, Gauss-Bonnet, Lovelock, and Hořava-Lifshitz. We also obtained the expansion law for nonextensive entropy like Tsallis entropy from the unified expansion law.- 8 March 2023
- Published by American Physical Society (APS) in Physical Review D
- Vol. 107 (6) , 063511
Unified formalism for the law of emergence from the first law of thermodynamics
We derive a unified expansion law for our Universe from the first law of thermodynamics on the apparent horizon, where entropic evolution depicts the emergence of cosmic space. The derivation advances a general form for degrees of freedom on the surface and bulk, which provides a natural generalization for the expansion law proposed by Padmanabhan. The general expression for the surface degrees of freedom differs from the natural expectation, in the emergent gravity paradigm for general theories of gravity. The derivation also provides justification for the selection of Gibbons-Hawking temperature in the original expansion law and for the use of areal volume in the nonflat Friedmann-Robertson-Walker universe. Since the unified expansion law exclusively depends on the form of entropy, the method is applicable to obtain the expansion law in any gravity theory without any additional ad hoc assumptions. From the general expansion law, we have obtained the expansion law corresponding to different theories of gravity like () Einstein, Gauss-Bonnet, Lovelock, and Hořava-Lifshitz. We also obtained the expansion law for nonextensive entropy like Tsallis entropy from the unified expansion law.- Open Access
Unified formalism for the emergence of space from the first law of thermodynamics
We derive a unified expansion law for our universe from the first law of thermodynamics on the apparent horizon, where entropic evolution depicts the emergence of cosmic space. The derivation advances a general form for degrees of freedom on the surface and bulk, which provides a natural generalization for the expansion law proposed by Padmanabhan. The general expression for the surface degrees of freedom differs from the natural expectation, $ N_{sur }= 4S $ in the emergent gravity paradigm for general theories of gravity. The derivation also provides justification for the selection of Gibbons-Hawking temperature in the original expansion law and for the use of areal volume in the non-flat FRW universe. Since the unified expansion law exclusively depends on the form of entropy, the method is applicable to obtain the expansion law in any gravity theory without any additional ad hoc assumptions. From the general expansion law, we have obtained the expansion law corresponding to different theories of gravity like (n+1) Einstein, Gauss-Bonnet, Lovelock, and Horava-Lifshitz. We also obtained the expansion law for non-extensive entropy like Tsallis entropy from the unified expansion law.Open AccessUnified formalism for the emergence of space from the first law of thermodynamics
We derive a unified expansion law for our universe from the first law of thermodynamics on the apparent horizon, where entropic evolution depicts the emergence of cosmic space. The derivation advances a general form for degrees of freedom on the surface and bulk, which provides a natural generalization for the expansion law proposed by Padmanabhan. The general expression for the surface degrees of freedom differs from the natural expectation, $ N_{sur }= 4S $ in the emergent gravity paradigm for general theories of gravity. The derivation also provides justification for the selection of Gibbons-Hawking temperature in the original expansion law and for the use of areal volume in the non-flat FRW universe. Since the unified expansion law exclusively depends on the form of entropy, the method is applicable to obtain the expansion law in any gravity theory without any additional ad hoc assumptions. From the general expansion law, we have obtained the expansion law corresponding to different theories of gravity like (n+1) Einstein, Gauss-Bonnet, Lovelock, and Horava-Lifshitz. We also obtained the expansion law for non-extensive entropy like Tsallis entropy from the unified expansion law. - Open Access
Emergence of space and expansion of universe
According to the principle of emergence, the expansion of the universe can be explained as the emergence of space with the progress of cosmic time. We have analytically solved the equation of emergence proposed by Padmanabhan by assuming the Komar energy density $\rho+3P$ as a function of the Hubble parameter. The resulting model describes the evolution of the universe, which proceeds towards a final de Sitter state. Model parameters have been extracted using the cosmological observational data. Further, the horizon entropy evolution of the model has been studied. The model predicts a universe having a transition from a prior decelerated epoch to a late accelerated epoch and reasonably predicts the cosmological constant.Open AccessEmergence of space and expansion of universe
According to the principle of emergence, the expansion of the universe can be explained as the emergence of space with the progress of cosmic time. We have analytically solved the equation of emergence proposed by Padmanabhan by assuming the Komar energy density $\rho+3P$ as a function of the Hubble parameter. The resulting model describes the evolution of the universe, which proceeds towards a final de Sitter state. Model parameters have been extracted using the cosmological observational data. Further, the horizon entropy evolution of the model has been studied. The model predicts a universe having a transition from a prior decelerated epoch to a late accelerated epoch and reasonably predicts the cosmological constant. - 14 June 2022
- Published by Springer Nature in General Relativity and Gravitation
- Vol. 54 (6) , 1-35
Emergence of cosmic space and its connection with thermodynamic principles
- 14 June 2022
- Published by Springer Nature in General Relativity and Gravitation
- Vol. 54 (6) , 1-35
Emergence of cosmic space and its connection with thermodynamic principles
- 18 May 2022
- Published by IOP Publishing in Classical and Quantum Gravity
- Vol. 39 (11) , 115012
Emergence of space and expansion of Universe
According to the principle of emergence, the expansion of the Universe can be explained as the emergence of space with the progress of cosmic time. We have analytically solved the equation of emergence proposed by Padmanabhan by assuming the Komar energy density ρ + 3P as a function of the Hubble parameter. The resulting model describes the evolution of the Universe, which proceeds towards a final de Sitter state. Model parameters have been extracted using the cosmological observational data. Further, the horizon entropy evolution of the model has been studied. The model predicts a Universe having a transition from a prior decelerated epoch to a late accelerated epoch and reasonably predicts the cosmological constant.
- 18 May 2022
- Published by IOP Publishing in Classical and Quantum Gravity
- Vol. 39 (11) , 115012
Emergence of space and expansion of Universe
According to the principle of emergence, the expansion of the Universe can be explained as the emergence of space with the progress of cosmic time. We have analytically solved the equation of emergence proposed by Padmanabhan by assuming the Komar energy density ρ + 3P as a function of the Hubble parameter. The resulting model describes the evolution of the Universe, which proceeds towards a final de Sitter state. Model parameters have been extracted using the cosmological observational data. Further, the horizon entropy evolution of the model has been studied. The model predicts a Universe having a transition from a prior decelerated epoch to a late accelerated epoch and reasonably predicts the cosmological constant.
- Open Access
Emergence of space from non-equilibrium thermodynamics in f(R) gravity
It has shown that the accelerated expansion of the FRW Universe can be explained as the quest towards the holographic equipartition ($N_{sur} = N_{bulk}$), satisfies the expansion law $\frac{dV}{dt} = l_{P}^{2} \left( N_{sur} - \epsilon N_{bulk} \right)$, from which one can derive the Friedmann equation of the FRW Universe in Einstein gravity \cite{paddy2012jun}. We introduce a generic derivation of the expansion law from the generalized first law of thermodynamics $-dE=TdS$ and $dE=TdS + WdV$. The generic derivation provides an expression for $N_{sur}$ in terms of entropy $S$ and the expansion law consistent with gravity theories having different entropy $S$, like Gauss-Bonnet and more general Lovelock gravity. We extended the same idea to the non-equilibrium situation and obtained the expansion law in f(R) gravity as a specific case. For this, we used the first law of thermodynamics in non-equilibrium description having the extra entropy production term $Td_{i}S.$Open AccessEmergence of space from non-equilibrium thermodynamics in f(R) gravity
It has shown that the accelerated expansion of the FRW Universe can be explained as the quest towards the holographic equipartition ($N_{sur} = N_{bulk}$), satisfies the expansion law $\frac{dV}{dt} = l_{P}^{2} \left( N_{sur} - \epsilon N_{bulk} \right)$, from which one can derive the Friedmann equation of the FRW Universe in Einstein gravity \cite{paddy2012jun}. We introduce a generic derivation of the expansion law from the generalized first law of thermodynamics $-dE=TdS$ and $dE=TdS + WdV$. The generic derivation provides an expression for $N_{sur}$ in terms of entropy $S$ and the expansion law consistent with gravity theories having different entropy $S$, like Gauss-Bonnet and more general Lovelock gravity. We extended the same idea to the non-equilibrium situation and obtained the expansion law in f(R) gravity as a specific case. For this, we used the first law of thermodynamics in non-equilibrium description having the extra entropy production term $Td_{i}S.$ - Open Access
Emergence of cosmic space and the maximization of horizon entropy
The spatial expansion of the universe can be described as the emergence of space with the progress of cosmic time, through a simple equation, $\Delta V = \Delta t\left(N_{surf}- N_{bulk}\right)$. This law of emergence suggested by Padmanabhan in the context of general relativity for a flat universe has been generalized by Sheykhi to Gauss Bonnet and Lovelock gravity for a universe with any spacial curvature. We investigate whether this generalized holographic equipartition effectively implies the maximization of horizon entropy. First, we obtain the constraints imposed by the maximization of horizon entropy in Einstein, Gauss Bonnet and Lovelock gravities for a universe with any spacial curvature. We then analyze the consistency of the law of emergence in \cite{Sheykhi}, with these constraints obtained. Interestingly, both the law of emergence and the horizon entropy maximization demands an asymptotically de Sitter universe with $\omega \geq -1$. More specifically, when the degrees of freedom in the bulk $( N_{bulk})$ becomes equal to the degrees of freedom on the boundary surface $(N_{surf}),$ the universe attains a state of maximum horizon entropy. Thus, the law of emergence can be viewed as a tendency for maximizing the horizon entropy, even in a non flat universe. Our results points at the deep connection between the law of emergence and horizon thermodynamics, beyond Einstein gravity irrespective of the spacial curvature.Open AccessEmergence of cosmic space and the maximization of horizon entropy
The spatial expansion of the universe can be described as the emergence of space with the progress of cosmic time, through a simple equation, $\Delta V = \Delta t\left(N_{surf}- N_{bulk}\right)$. This law of emergence suggested by Padmanabhan in the context of general relativity for a flat universe has been generalized by Sheykhi to Gauss Bonnet and Lovelock gravity for a universe with any spacial curvature. We investigate whether this generalized holographic equipartition effectively implies the maximization of horizon entropy. First, we obtain the constraints imposed by the maximization of horizon entropy in Einstein, Gauss Bonnet and Lovelock gravities for a universe with any spacial curvature. We then analyze the consistency of the law of emergence in \cite{Sheykhi}, with these constraints obtained. Interestingly, both the law of emergence and the horizon entropy maximization demands an asymptotically de Sitter universe with $\omega \geq -1$. More specifically, when the degrees of freedom in the bulk $( N_{bulk})$ becomes equal to the degrees of freedom on the boundary surface $(N_{surf}),$ the universe attains a state of maximum horizon entropy. Thus, the law of emergence can be viewed as a tendency for maximizing the horizon entropy, even in a non flat universe. Our results points at the deep connection between the law of emergence and horizon thermodynamics, beyond Einstein gravity irrespective of the spacial curvature.