TY - JOUR

T1 - Sign of the amount of nonconservation energy in entropic cosmology

AU - Lepe, Samuel

AU - Peña, Francisco

N1 - Funding Information:
Acknowledgements This work was supported by FONDECYT Grant No. 1110076 (SL), VRIEA-DI-PUCV No. 037.492/2013, Vice Rectoría de Investigación y Estudios Avanzados, Pontificia Universi-dad Católica de Valparaíso (SL) and DIUFRO DI12-0006, Dirección de Investigación y Desarrollo, Universidad de La Frontera (FP). One of us (SL) acknowledges the hospitality of the Departamento de Ciencias Físicas de la Universidad de La Frontera, where part of this work was done. We would like to thank Helen Lowry for reviewing the English.

PY - 2014/3

Y1 - 2014/3

N2 - In the framework of Friedmann-Lemaitre-Robertson-Walker cosmology modified by entropic issues, the sign change of the inhomogeneous term associated with the nonconservation energy equation for cosmic fluid is discussed; specifically, this is a bare/effective study of the equation of state for this fluid through a bare (ω)/effective (ωeff) description. In the bare case, where there is a nonconserved equation of state, the change in the sign of the inhomogeneous term at different times of the cosmic evolution is described. By redefining the adiabatic ω-parameter, the usual scheme for cosmic evolution can be recovered. In the effective case, if evolution is driven by dust or the cosmological constant, the universe evolves towards thermal equilibrium. However, by incorporating a quantum correction, only the cosmological constant can lead to thermal equilibrium. This correction avoids the future singularity that is present when it is not incorporated.

AB - In the framework of Friedmann-Lemaitre-Robertson-Walker cosmology modified by entropic issues, the sign change of the inhomogeneous term associated with the nonconservation energy equation for cosmic fluid is discussed; specifically, this is a bare/effective study of the equation of state for this fluid through a bare (ω)/effective (ωeff) description. In the bare case, where there is a nonconserved equation of state, the change in the sign of the inhomogeneous term at different times of the cosmic evolution is described. By redefining the adiabatic ω-parameter, the usual scheme for cosmic evolution can be recovered. In the effective case, if evolution is driven by dust or the cosmological constant, the universe evolves towards thermal equilibrium. However, by incorporating a quantum correction, only the cosmological constant can lead to thermal equilibrium. This correction avoids the future singularity that is present when it is not incorporated.

KW - Cosmology

KW - Entropic

KW - Modified gravity

UR - http://www.scopus.com/inward/record.url?scp=84896728501&partnerID=8YFLogxK

U2 - 10.1007/s10509-013-1750-5

DO - 10.1007/s10509-013-1750-5

M3 - Article

AN - SCOPUS:84896728501

SN - 0004-640X

VL - 350

SP - 401

EP - 406

JO - Astrophysics and Space Science

JF - Astrophysics and Space Science

IS - 1

ER -