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dc.contributor.authorSemkov, E. H.
dc.contributor.authorPeneva, S. P.
dc.contributor.authorMunari, U.
dc.contributor.authorTsvetkov, M. K.
dc.contributor.authorJurdana-Šepić, R.
dc.contributor.authorMiguel Agustino, Enrique de 
dc.contributor.authorSchwartz, R. D.
dc.contributor.authorDimitrov, D. P.
dc.contributor.authorKjurkchieva, D. P.
dc.contributor.authorRadeva, V. S.
dc.date.accessioned2014-12-16T12:19:17Z
dc.date.available2014-12-16T12:19:17Z
dc.date.issued2012
dc.identifier.citationSemkov, E.H.. Peneva, S.P., Munari, U., Tsvetkov, M.K., Jurdana-Šepić, R., Miguel Agustino, E., Schwartz, R.D., Dimitrov, D.P., Kjurkchieva, D.P., Radeva, V.S.: "Optical photometric and spectral study of the new FU Orionis object V2493 Cygni (HBC 722)". Astronomy and Astrophysics. Vol. 542, A43 (2012). ISSN 0004-6361
dc.identifier.issn0004-6361
dc.identifier.issn1432-0746 (electrónico)
dc.identifier.urihttp://hdl.handle.net/10272/9543
dc.description.abstractAims. We present new results from optical photometric and spectroscopic observations of the eruptive pre-main sequence star V2493 Cyg (HBC 722). The object has continued to undergo significant brightness variations over the past few months and is an ideal target for follow-up observations. Methods. We carried out CCD BVRI photometric observations in the field of V2493 Cyg (“Gulf of Mexico”) from August 1994 to April 2012, i.e. at the pre-outburst states and during the phases of the outburst. We acquired high, medium, and low resolution spectroscopy of V2493 Cyg during the outburst. To study the pre-outburst variability of the target and construct its historical light curve, we searched for archival observations in photographic plate collections. Both CCD and photographic observations were analyzed using 15 comparison stars in the field of V2493 Cyg. Results. The pre-outburst photographic and CCD photometric observations of V2493 Cyg show low-amplitude light variations typical of T Tauri stars. The recent photometric data show a slow light decrease from October 2010 to June 2011 followed by an increase in brightness that continued until early 2012. The spectral observations of V2493 Cyg are typical of FU Orionis stars absorption spectra with strong P Cyg profiles of Hα and Na I D lines. On the basis of photometric monitoring performed over the past two years, the spectral properties at the maximal light, as well as the shape of long-term light curves, we confirm that the observed outburst of V2493 Cyg is of FU Orionis type.en_US
dc.language.isoengen_US
dc.publisherEuropean Southern Observatoryen_US
dc.rightsAtribución-NoComercial-SinDerivadas 3.0 España*
dc.rights.urihttp://creativecommons.org/licenses/by-nc-nd/3.0/es/*
dc.subject.otherStars: pre-main sequenceen_US
dc.subject.otherStars: variables: T Tauri, Herbig Ae/Been_US
dc.subject.otherStars: individual: V2493 Cygnien_US
dc.titleOptical photometric and spectral study of the new FU Orionis object V2493 Cygni (HBC 722)en_US
dc.typeinfo:eu-repo/semantics/articleen_US
dc.relation.publisherversionhttp://www.aanda.org/articles/aa/abs/2012/06/aa19140-12/aa19140-12.htmlen_US
dc.identifier.doi10.1051/0004-6361/201219140
dc.rights.accessRightsinfo:eu-repo/semantics/openAccessen_US


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