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dc.contributor.authorCLIFTON, TAen_US
dc.date.accessioned2016-11-22T14:18:08Z
dc.date.issued2013-03en_US
dc.date.submitted2016-11-07T16:36:51.219Z
dc.identifier.other133004
dc.identifier.other133004
dc.identifier.other133004
dc.identifier.other133004
dc.identifier.other133004en_US
dc.identifier.other133004en_US
dc.identifier.urihttp://qmro.qmul.ac.uk/xmlui/handle/123456789/17821
dc.description.abstractWe introduce the concept of back-reaction in relativistic cosmological modeling. Roughly speaking, this can be thought of as the difference between the large-scale behavior of an inhomogeneous cosmological solution of Einstein’s equations, and a homogeneous and isotropic solution that is a best-fit to either the average of observables or dynamics in the inhomogeneous solution. This is sometimes paraphrased as “the effect that structure has of the large-scale evolution of the universe.” Various different approaches have been taken in the literature in order to try and understand back-reaction in cosmology. We provide a brief and critical summary of some of them, highlighting recent progress that has been made in each case.en_US
dc.languageEng.en_US
dc.publisherhttp://www.worldscientific.com/doi/pdfplus/10.1142/S0218271813300048en_US
dc.relation.ispartofInternational Journal of Modern Physics D: Gravitation, Astrophysics and Cosmologyen_US
dc.rightsThis is a pre-copyedited, author-produced PDF of an article accepted for publication in International Journal of Modern Physics D following peer review. The version of record is available http://www.worldscientific.com/doi/abs/10.1142/S0218271813300048
dc.titleBACK-REACTION IN RELATIVISTIC COSMOLOGYen_US
dc.typeArticle
dc.rights.holder© 2016 World Scientific Publishing Co Pte Ltd
dc.identifier.doi10.1142/S0218271813300048en_US
pubs.issue3en_US
pubs.notesNot knownen_US
pubs.publication-statusPublisheden_US
pubs.volume22en_US


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