{ "id": "1510.06612", "version": "v1", "published": "2015-10-22T13:04:43.000Z", "updated": "2015-10-22T13:04:43.000Z", "title": "Light curves of the latest FUor: Indication of a close binary", "authors": [ "M. Hackstein", "M. Haas", "Á. Kóspál", "F. -J. Hambsch", "R. Chini", "P. Ábrahám", "A. Moór", "F. Pozo Nuñez", "M. Ramolla", "Ch. Westhues", "L. Kaderhandt", "Ch. Fein", "A. Barr Domínguez", "K. -W. Hodapp" ], "journal": "A&A 582 L12 (2015)", "doi": "10.1051/0004-6361/201527127", "categories": [ "astro-ph.SR" ], "abstract": "We monitored the recent FUor 2MASS J06593158-0405277 (V960 Mon) since November 2009 at various observatories and multiple wavelengths. After the outburst by nearly 2.9 mag in $r$ around September 2014 the brightness gently fades until April 2015 by nearly 1 mag in $U$ and 0.5 mag in $z$. Thereafter the brightness at $\\lambda>5000 \\AA$ was constant until June 2015 while the shortest wavelengths ($U, B$) indicate a new rise, similar to that seen for the FUor V2493 Cyg (HBC722). Our near-infrared (NIR) monitoring between December 2014 and April 2015 shows a smaller outburst amplitude ($\\sim$2 mag) and a smaller (0.2 $-$ 0.3 mag) post-outburst brightness decline. Optical and NIR color-magnitude diagrams indicate that the brightness decline is caused by growing extinction. The post-outburst light curves are modulated by an oscillating color-neutral pattern with a period of about 17 days and an amplitude declining from $\\sim$0.08 mag in October 2014 to $\\sim$0.04 mag in May 2015. The properties of the oscillating pattern lead us to suggest the presence of a close binary with eccentric orbit.", "revisions": [ { "version": "v1", "updated": "2015-10-22T13:04:43.000Z" } ], "analyses": { "keywords": [ "close binary", "latest fuor", "indication", "post-outburst brightness decline", "smaller outburst amplitude" ], "tags": [ "journal article" ], "note": { "typesetting": "TeX", "pages": 0, "language": "en", "license": "arXiv", "status": "editable" } } }