Non-linear coupling in the dark sector as a running vacuum model

In this work we study a phenomenological non-gravitational interaction between dark matter and dark energy. The scenario studied in this work extends the usual interaction model proportional to the derivative of the dark component density adding to the coupling a non-linear term of the form Q= ρ′/ 3...

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Guardado en:
Detalles Bibliográficos
Publicado: 2018
Materias:
Cosmology
Interacting dark sector
Linear perturbations
Running vacuum
Acceso en línea:https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00017701_v50_n8_p_DeSantiago
http://hdl.handle.net/20.500.12110/paper_00017701_v50_n8_p_DeSantiago
Aporte de:
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
id paper:paper_00017701_v50_n8_p_DeSantiago
record_format dspace
spelling paper:paper_00017701_v50_n8_p_DeSantiago2023-06-08T14:21:40Z Non-linear coupling in the dark sector as a running vacuum model Cosmology Interacting dark sector Linear perturbations Running vacuum In this work we study a phenomenological non-gravitational interaction between dark matter and dark energy. The scenario studied in this work extends the usual interaction model proportional to the derivative of the dark component density adding to the coupling a non-linear term of the form Q= ρ′/ 3 (α+ βρDark) This dark sector interaction model could be interpreted as a particular case of a running vacuum model of the type Λ (H) = n0+ n1H2+ n2H4 in which the vacuum decays into dark matter. For a flat FRW Universe filled with dark energy, dark matter and decoupled baryonic matter and radiation we calculate the energy density evolution equations of the dark sector and solve them. The different sign combinations of the two parameters of the model show clear qualitative different cosmological scenarios, from basic cosmological insights we discard some of them. The linear scalar perturbation equations of the dark matter were calculated. Using the CAMB code we calculate the CMB and matter power spectra for some values of the parameters α and β and compare it with Λ CDM. The model modify mainly the lower multipoles of the CMB power spectrum remaining almost the same the high ones. The matter power spectrum for low wave numbers is not modified by the interaction but after the maximum it is clearly different. Using observational data from Planck, and various galaxy surveys we obtain the constraints of the parameters, the best fit values obtained are the combinations α= (3.7 ± 7) × 10 - 4, -(1.5×10-5eV-1)4≪β<(0.07eV-1)4. © 2018, Springer Science+Business Media, LLC, part of Springer Nature. 2018 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00017701_v50_n8_p_DeSantiago http://hdl.handle.net/20.500.12110/paper_00017701_v50_n8_p_DeSantiago
institution Universidad de Buenos Aires
institution_str I-28
repository_str R-134
collection Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
topic Cosmology
Interacting dark sector
Linear perturbations
Running vacuum
spellingShingle Cosmology
Interacting dark sector
Linear perturbations
Running vacuum
Non-linear coupling in the dark sector as a running vacuum model
topic_facet Cosmology
Interacting dark sector
Linear perturbations
Running vacuum
description In this work we study a phenomenological non-gravitational interaction between dark matter and dark energy. The scenario studied in this work extends the usual interaction model proportional to the derivative of the dark component density adding to the coupling a non-linear term of the form Q= ρ′/ 3 (α+ βρDark) This dark sector interaction model could be interpreted as a particular case of a running vacuum model of the type Λ (H) = n0+ n1H2+ n2H4 in which the vacuum decays into dark matter. For a flat FRW Universe filled with dark energy, dark matter and decoupled baryonic matter and radiation we calculate the energy density evolution equations of the dark sector and solve them. The different sign combinations of the two parameters of the model show clear qualitative different cosmological scenarios, from basic cosmological insights we discard some of them. The linear scalar perturbation equations of the dark matter were calculated. Using the CAMB code we calculate the CMB and matter power spectra for some values of the parameters α and β and compare it with Λ CDM. The model modify mainly the lower multipoles of the CMB power spectrum remaining almost the same the high ones. The matter power spectrum for low wave numbers is not modified by the interaction but after the maximum it is clearly different. Using observational data from Planck, and various galaxy surveys we obtain the constraints of the parameters, the best fit values obtained are the combinations α= (3.7 ± 7) × 10 - 4, -(1.5×10-5eV-1)4≪β<(0.07eV-1)4. © 2018, Springer Science+Business Media, LLC, part of Springer Nature.
title Non-linear coupling in the dark sector as a running vacuum model
title_short Non-linear coupling in the dark sector as a running vacuum model
title_full Non-linear coupling in the dark sector as a running vacuum model
title_fullStr Non-linear coupling in the dark sector as a running vacuum model
title_full_unstemmed Non-linear coupling in the dark sector as a running vacuum model
title_sort non-linear coupling in the dark sector as a running vacuum model
publishDate 2018
url https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00017701_v50_n8_p_DeSantiago
http://hdl.handle.net/20.500.12110/paper_00017701_v50_n8_p_DeSantiago
_version_ 1768545763379380224

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