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Limits on decaying dark energy density models from the CMB temperature-redshift relation


Jetzer, P; Puy, D; Signore, M; Tortora, C (2011). Limits on decaying dark energy density models from the CMB temperature-redshift relation. General Relativity and Gravitation, 43(4):1083-1093.

Abstract

The nature of the dark energy is still a mystery and several models have been proposed to explain it. Here we consider a phenomenological model for dark energy decay into photons and particles as proposed by Lima (Phys Rev D 54:2571, 1996). He studied the thermodynamic aspects of decaying dark energy models in particular in the case of a continuous photon creation and/or disruption. Following his approach, we derive a temperature redshift relation for the cosmic microwave background (CMB) which depends on the effective equation of state w eff and on the "adiabatic index" γ. Comparing our relation with the data on the CMB temperature as a function of the redshift obtained from Sunyaev-Zel'dovich observations and at higher redshift from quasar absorption line spectra, we find w eff = -0.97 ± 0.03, adopting for the adiabatic index γ = 4/3, in good agreement with current estimates and still compatible with w eff = -1, implying that the dark energy content being constant in time.

The nature of the dark energy is still a mystery and several models have been proposed to explain it. Here we consider a phenomenological model for dark energy decay into photons and particles as proposed by Lima (Phys Rev D 54:2571, 1996). He studied the thermodynamic aspects of decaying dark energy models in particular in the case of a continuous photon creation and/or disruption. Following his approach, we derive a temperature redshift relation for the cosmic microwave background (CMB) which depends on the effective equation of state w eff and on the "adiabatic index" γ. Comparing our relation with the data on the CMB temperature as a function of the redshift obtained from Sunyaev-Zel'dovich observations and at higher redshift from quasar absorption line spectra, we find w eff = -0.97 ± 0.03, adopting for the adiabatic index γ = 4/3, in good agreement with current estimates and still compatible with w eff = -1, implying that the dark energy content being constant in time.

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Additional indexing

Item Type:Journal Article, refereed, original work
Communities & Collections:07 Faculty of Science > Institute for Computational Science
Dewey Decimal Classification:530 Physics
Language:English
Date:April 2011
Deposited On:19 Feb 2012 19:01
Last Modified:05 Apr 2016 14:55
Publisher:Springer
ISSN:0001-7701 (P) 1572-9532 (E)
Additional Information:The original publication is available at www.springerlink.com
Publisher DOI:10.1007/s10714-010-1091-4
Related URLs:http://arxiv.org/abs/1007.2325
Permanent URL: http://doi.org/10.5167/uzh-48325

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