dc.contributor.author Kral, Quentin dc.contributor.author Krivov, Alexander V dc.contributor.author Defrere, Denis dc.contributor.author Lieshout, Rik van dc.contributor.author Bonsor-Matthews, Amy dc.contributor.author Augereau, Jean-Charles dc.contributor.author Thebault, Philippe dc.contributor.author Ertel, Steve dc.contributor.author Lebreton, Jeremy dc.contributor.author Absil, Olivier dc.date.accessioned 2018-10-10T05:17:19Z dc.date.available 2018-10-10T05:17:19Z dc.date.issued 2017-04-03 dc.identifier.issn 2167-2857 dc.identifier.uri https://www.repository.cam.ac.uk/handle/1810/283370 dc.description.abstract A warm/hot dust component (at temperature $>$ 300K) has been detected around $\sim$ 20% of stars. This component is called "exozodiacal dust" as it presents similarities with the zodiacal dust detected in our Solar System, even though its physical properties and spatial distribution can be significantly different. Understanding the origin and evolution of this dust is of crucial importance, not only because its presence could hamper future detections of Earth-like planets in their habitable zones, but also because it can provide invaluable information about the inner regions of planetary systems. In this review, we present a detailed overview of the observational techniques used in the detection and characterisation of exozodiacal dust clouds ("exozodis") and the results they have yielded so far, in particular regarding the incidence rate of exozodis as a function of crucial parameters such as stellar type and age, or the presence of an outer cold debris disc. We also present the important constraints that have been obtained, on dust size distribution and spatial location, by using state-of-the-art radiation transfer models on some of these systems. Finally, we investigate the crucial issue of how to explain the presence of exozodiacal dust around so many stars (regardless of their ages) despite the fact that such dust so close to its host star should disappear rapidly due to the coupled effect of collisions and stellar radiation pressure. Several potential mechanisms have been proposed to solve this paradox and are reviewed in detail in this paper. The review finishes by presenting the future of this growing field. dc.language en dc.publisher Informa UK Limited dc.rights Attribution 4.0 International dc.rights.uri https://creativecommons.org/licenses/by/4.0/ dc.title Exozodiacal clouds: Hot and warm dust around main sequence stars dc.type Article prism.endingPage 111 prism.issueIdentifier 2 prism.publicationDate 2017 prism.publicationName Astronomical Review prism.startingPage 69 prism.volume 13 dc.identifier.doi 10.17863/CAM.30738 rioxxterms.versionofrecord 10.1080/21672857.2017.1353202 rioxxterms.licenseref.uri http://www.rioxx.net/licenses/all-rights-reserved rioxxterms.licenseref.startdate 2017-04-03 dc.contributor.orcid Bonsor-Matthews, Amy [0000-0002-8070-1901] dc.identifier.eissn 2167-2865 rioxxterms.type Journal Article/Review pubs.funder-project-id European Research Council (279973) pubs.funder-project-id Royal Society (DH150088) cam.issuedOnline 2017-09-07
﻿

### This item appears in the following Collection(s)

Except where otherwise noted, this item's licence is described as Attribution 4.0 International