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http://hdl.handle.net/20.500.12386/24040
Titolo: | Fast-moving features in the debris disk around AU Microscopii | Autori: | Boccaletti, Anthony Thalmann, Christian Lagrange, Anne-Marie Janson, Markus Augereau, Jean-Charles Schneider, Glenn Milli, Julien Grady, Carol Debes, John Langlois, Maud Mouillet, David Henning, Thomas Dominik, Carsten Maire, Anne-Lise Beuzit, Jean-Luc Carson, Joseph Dohlen, Kjetil Engler, Natalia Feldt, Markus Fusco, Thierry Ginski, Christian Girard, Julien H. Hines, Dean Kasper, Markus Mawet, Dimitri Ménard, François Meyer, Michael R. Moutou, Claire Olofsson, Johan Rodigas, Timothy Sauvage, Jean-Francois Schlieder, Joshua Schmid, Hans Martin TURATTO, Massimo Udry, Stephane Vakili, Farrokh Vigan, Arthur Wahhaj, Zahed Wisniewski, John |
Data pubblicazione: | 2015 | Rivista: | NATURE | Numero: | 526 | Fascicolo: | 7572 | Da pagina:: | 230 | Abstract: | In the 1980s, excess infrared emission was discovered around main-sequence stars; subsequent direct-imaging observations revealed orbiting disks of cold dust to be the source. These `debris disks' were thought to be by-products of planet formation because they often exhibited morphological and brightness asymmetries that may result from gravitational perturbation by planets. This was proved to be true for the β Pictoris system, in which the known planet generates an observable warp in the disk. The nearby, young, unusually active late-type star AU Microscopii hosts a well-studied edge-on debris disk; earlier observations in the visible and near-infrared found asymmetric localized structures in the form of intensity variations along the midplane of the disk beyond a distance of 20 astronomical units. Here we report high-contrast imaging that reveals a series of five large-scale features in the southeast side of the disk, at projected separations of 10-60 astronomical units, persisting over intervals of 1-4 years. All these features appear to move away from the star at projected speeds of 4-10 kilometres per second, suggesting highly eccentric or unbound trajectories if they are associated with physical entities. The origin, localization, morphology and rapid evolution of these features are difficult to reconcile with current theories. | Acknowledgments: | SPHERE was built by a European consortium led by IPAG (France). SPHERE was funded by the ESO, with additional contributions from CNRS, MPIA, INAF, FINES and NOVA. SPHERE also received funding from the European Commission FP6 and FP7 programmes as part of OPTICON under grant numbers RII3-Ct-2004-001566 (FP6), 226604 (FP7) and 312430 (FP7). French co-authors are supported by ANR-14-CE33-0018. Part of this work has been carried out within the framework of the National Centre for Competence in Research PlanetS supported by the Swiss National Science Foundation. C.T. and M.R.M. acknowledge the financial support of the SNSF.This study is based on observations from program 60.A-9249(C) at ESO Very Large Telescope and from program number 12228 made with the NASA/ESA Hubble Space Telescope, obtained at STScI, which is operated by AURA Inc. under NASA contract NAS 5-26555. We are also grateful to the ESO for releasing the commissioning data for publication. Finally, we thank P. Zarka, N. Meyer-Vernet, B. Stelzer and Q. Kral for discussions. J.S. is a NASA Postdoctoral Program Fellow. | URI: | http://hdl.handle.net/20.500.12386/24040 | URL: | https://www.nature.com/articles/nature15705 | ISSN: | 0028-0836 | DOI: | 10.1038/nature15705 | Bibcode ADS: | 2015Natur.526..230B | Fulltext: | open |
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