Viscous self interacting dark matter cosmology for small redshift

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dc.contributor.author Atreya, Abhishek
dc.contributor.author Bhatt, Jitesh R.
dc.contributor.author Mishra, Arvind Kumar
dc.date.accessioned 2018-11-16T06:05:54Z
dc.date.available 2018-11-16T06:05:54Z
dc.date.issued 2018-10
dc.identifier.citation Atreya, Abhishek; Bhatt, Jitesh R. and Mishra, Arvind Kumar, "Viscous self interacting dark matter cosmology for small redshift", arXiv, Cornell University Library, DOI: arXiv:1810.11666, Oct. 2018. en_US
dc.identifier.uri http://arxiv.org/abs/1810.11666
dc.identifier.uri https://repository.iitgn.ac.in/handle/123456789/3996
dc.description.abstract The viscosity of dark matter in cosmological models may cause an accelerated expansion and when this effect is sufficiently large, it can explain the dark energy. In this work, attributing the origin of viscosity to self-interaction of dark matter, we study the viscous cosmology at small redshift (0?z?2.5). Assuming the cluster scale to be virialized and by modeling a power law behavior of velocity gradients, we calculate the Hubble expansion rate, H(z) and the deceleration parameter, q(z). We then perform a ?2 analysis to estimate the best fit model parameters. By using the best fit values, we explain the cosmic chronometer and type Ia supernova data. We conclude that if the dissipative effects become prominent only at the late time of cosmic evolution and are smaller at higher redshift, we can explain the observational data without requiring any dark energy component. Our analysis is independent of any specific model of self interacting dark matter.
dc.description.statementofresponsibility by Abhishek Atreya, Jitesh R. Bhatt and Arvind Kumar Mishra
dc.language.iso en en_US
dc.publisher Cornell University Library en_US
dc.subject Cosmology en_US
dc.subject Nongalactic en_US
dc.subject Astrophysics en_US
dc.subject High Energy Physics en_US
dc.subject Phenomenology en_US
dc.title Viscous self interacting dark matter cosmology for small redshift en_US
dc.type Preprint en_US


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