3-Form Cosmology: Phantom Behaviour, Singularities and Interactions
The latest cosmological observations by the Planck collaboration (and combined with others) are compatible with a phantom-like behaviour ( w < − 1 ) for the dark energy equation of state that drives the current acceleration of the Universe. With this mindset, we look into models where d...
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| Format: | Article |
| Language: | English |
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MDPI AG
2017-03-01
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| Series: | Universe |
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| Online Access: | http://www.mdpi.com/2218-1997/3/1/21 |
| _version_ | 1811187262719787008 |
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| author | João Morais Mariam Bouhmadi-López João Marto |
| author_facet | João Morais Mariam Bouhmadi-López João Marto |
| author_sort | João Morais |
| collection | DOAJ |
| description | The latest cosmological observations by the Planck collaboration (and combined with others) are compatible with a phantom-like behaviour ( w < − 1 ) for the dark energy equation of state that drives the current acceleration of the Universe. With this mindset, we look into models where dark energy is described by a 3-form field minimally coupled to gravity. When compared to a scalar field, these models have the advantage of more naturally accommodating a cosmological-constant and phantom-like behaviours. We show how the latter happens for a fairly general class of positive-valued potentials, and through a dynamical system approach, we find that in such cases the 3-form field leads the Universe into a Little Sibling of the Big Rip singular event into the future. In this work, we explore the possibility of avoiding such singularity via an interaction in the dark sector between cold dark matter and the 3-form field. For the kind of interactions considered, we deduce a condition for replacing the LSBR by a late time de Sitter phase. For specific examples of interactions that meet this condition, we look for distinctive imprints in the statefinder hierarchy { S 3 ( 1 ) ; S 4 ( 1 ) } , { S 3 ( 1 ) ; S 5 ( 1 ) } , and in the growth rate of matter, ϵ ( z ) , through the composite null diagnostic (CND). |
| first_indexed | 2024-04-11T13:59:21Z |
| format | Article |
| id | doaj.art-6651295aa6864e048e8686036e91f4cf |
| institution | Directory Open Access Journal |
| issn | 2218-1997 |
| language | English |
| last_indexed | 2024-04-11T13:59:21Z |
| publishDate | 2017-03-01 |
| publisher | MDPI AG |
| record_format | Article |
| series | Universe |
| spelling | doaj.art-6651295aa6864e048e8686036e91f4cf2022-12-22T04:20:10ZengMDPI AGUniverse2218-19972017-03-01312110.3390/universe3010021universe30100213-Form Cosmology: Phantom Behaviour, Singularities and InteractionsJoão Morais0Mariam Bouhmadi-López1João Marto2Department of Theoretical Physics, University of the Basque Country UPV/EHU, P.O. Box 644, 48080 Bilbao, SpainDepartment of Theoretical Physics, University of the Basque Country UPV/EHU, P.O. Box 644, 48080 Bilbao, SpainDepartamento de Física, Universidade da Beira Interior, Rua Marquês D’Ávila e Bolama, 6201-001 Covilhã, PortugalThe latest cosmological observations by the Planck collaboration (and combined with others) are compatible with a phantom-like behaviour ( w < − 1 ) for the dark energy equation of state that drives the current acceleration of the Universe. With this mindset, we look into models where dark energy is described by a 3-form field minimally coupled to gravity. When compared to a scalar field, these models have the advantage of more naturally accommodating a cosmological-constant and phantom-like behaviours. We show how the latter happens for a fairly general class of positive-valued potentials, and through a dynamical system approach, we find that in such cases the 3-form field leads the Universe into a Little Sibling of the Big Rip singular event into the future. In this work, we explore the possibility of avoiding such singularity via an interaction in the dark sector between cold dark matter and the 3-form field. For the kind of interactions considered, we deduce a condition for replacing the LSBR by a late time de Sitter phase. For specific examples of interactions that meet this condition, we look for distinctive imprints in the statefinder hierarchy { S 3 ( 1 ) ; S 4 ( 1 ) } , { S 3 ( 1 ) ; S 5 ( 1 ) } , and in the growth rate of matter, ϵ ( z ) , through the composite null diagnostic (CND).http://www.mdpi.com/2218-1997/3/1/21dark energy 3-formsDM-DE interactionfuture singularitiescosmographystatefinders approachgrowth ratedynamical systems |
| spellingShingle | João Morais Mariam Bouhmadi-López João Marto 3-Form Cosmology: Phantom Behaviour, Singularities and Interactions Universe dark energy 3-forms DM-DE interaction future singularities cosmography statefinders approach growth rate dynamical systems |
| title | 3-Form Cosmology: Phantom Behaviour, Singularities and Interactions |
| title_full | 3-Form Cosmology: Phantom Behaviour, Singularities and Interactions |
| title_fullStr | 3-Form Cosmology: Phantom Behaviour, Singularities and Interactions |
| title_full_unstemmed | 3-Form Cosmology: Phantom Behaviour, Singularities and Interactions |
| title_short | 3-Form Cosmology: Phantom Behaviour, Singularities and Interactions |
| title_sort | 3 form cosmology phantom behaviour singularities and interactions |
| topic | dark energy 3-forms DM-DE interaction future singularities cosmography statefinders approach growth rate dynamical systems |
| url | http://www.mdpi.com/2218-1997/3/1/21 |
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