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 -