TY - JOUR

T1 - Dark energy interacting with dark matter and a third fluid

T2 - Possible EoS for this component

AU - Cruz, Norman

AU - Lepe, Samuel

AU - Peña, Francisco

N1 - Funding Information:
The authors acknowledge Prof. Ulrich Raff for the critical reading of our manuscript. N.C. and S.L. acknowledge the hospitality of the Physics Department of Universidad de La Frontera where part of this work was done. S.L. acknowledges the hospitality of the Physics Department of Universidad de Santiago de Chile . We thanks the suggestion given by the referee, in order to improve the presentation of this Letter. We acknowledge the support to this research by CONICYT through grants Nos. 1110840 (N.C.) and 1110076 (S.L.). This work was also supported from DIUFRO DI10-0009 , of Dirección de Investigación y Desarrollo, Universidad de La Frontera (F.P.) and DICYT 040831 CM, Universidad de Santiago de Chile (N.C.).

PY - 2011/5/9

Y1 - 2011/5/9

N2 - A cosmological model of dark energy interacting with dark matter and another general component of the universe is considered. The equations for the coincidence parameters r and s, which represent the ratios between dark energy and dark matter and the other cosmic fluid respectively, are analyzed in terms of the stability of stationary solutions. The obtained general results allow to shed some light on the equations of state of the three interacting fluids, due to the constraints imposed by the stability of the solutions. We found that for an interaction proportional to the sum of the dark energy density and the third fluid density, the hypothetical fluid must have positive pressure, which leads naturally to a cosmological scenario with radiation, unparticle or even some form of warm dark matter as the third interacting fluid.

AB - A cosmological model of dark energy interacting with dark matter and another general component of the universe is considered. The equations for the coincidence parameters r and s, which represent the ratios between dark energy and dark matter and the other cosmic fluid respectively, are analyzed in terms of the stability of stationary solutions. The obtained general results allow to shed some light on the equations of state of the three interacting fluids, due to the constraints imposed by the stability of the solutions. We found that for an interaction proportional to the sum of the dark energy density and the third fluid density, the hypothetical fluid must have positive pressure, which leads naturally to a cosmological scenario with radiation, unparticle or even some form of warm dark matter as the third interacting fluid.

KW - Cosmology

KW - Dark matter

KW - Equation of state

KW - Interacting dark energy

UR - http://www.scopus.com/inward/record.url?scp=79954969726&partnerID=8YFLogxK

U2 - 10.1016/j.physletb.2011.03.049

DO - 10.1016/j.physletb.2011.03.049

M3 - Article

AN - SCOPUS:79954969726

SN - 0370-2693

VL - 699

SP - 135

EP - 140

JO - Physics Letters, Section B: Nuclear, Elementary Particle and High-Energy Physics

JF - Physics Letters, Section B: Nuclear, Elementary Particle and High-Energy Physics

IS - 3

ER -