Volume 473, Number 3, October III 2007
|Page(s)||903 - 905|
|Section||Stellar structure and evolution|
|Published online||13 August 2007|
Cygnus X-3 transition from the ultrasoft to the hard state *
INTEGRAL Science Data Centre, Chemin d'Écogia 16, 1290 Versoix, Switzerland e-mail: Volker.Beckmann@obs.unige.ch
2 Observatoire Astronomique de l'Université de Genève, Chemin des Maillettes 51, 1290 Sauverny, Switzerland
3 CSST, University of Maryland Baltimore County, 1000 Hilltop Circle, Baltimore, MD 21250, USA
4 INTEGRAL Science Operations Centre, European Space Astronomy Centre (ESAC), Apartado 50727, 28080 Madrid, Spain
5 Danish National Space Centre, Technical University of Denmark, Juliane Maries Vej 30, 2100 Copenhagen, Denmark
6 Laboratorio de Astrofísica Espacial y Física Fundamental (LAEFF-INTA), POB 50727, 28080 Madrid, Spain
7 INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica di Roma, via Fosso del Cavaliere 100, 00133 Roma, Italy
8 Dipartimento di Astronomia, Universita' degli Studi di Bologna, via Ranzani 1, 40127 Bologna, Italy
9 Centre d'Étude Spatiale des Rayonnements, CNRS/UPS, BP 4346, 31028 Toulouse Cedex 4, France
10 Astrophysics Science Division, NASA Goddard Space Flight Center, Code 661, MD 20771, USA
11 Space Research Institute, Russian Academy of Sciences, Profsoyuznaya 84/32, 117997 Moscow, Russia
12 Observatory, PO Box 14, University of Helsinki, 00014 University of Helsinki, Finland
13 Max-Planck-Institut für extraterrestrische Physik, Gießenbachstraße, 85748 Garching, Germany
Accepted: 3 August 2007
Aims.The nature of Cygnus X-3 is still not understood well. This binary system might host a black hole or a neutron star. Recent observations by INTEGRAL have shown that Cygnus X-3 was again in an extremely ultrasoft state. Here we present our analysis of the transition from the ultrasoft state, dominated by blackbody radiation at soft X-rays plus non-thermal emission in the hard X-rays, to the low hard state.
Methods.INTEGRAL observed Cyg X-3 six times during three weeks in late May and early June 2007. Data from IBIS/ISGRI and JEM-X1 were analysed to show the spectral transition.
Results.During the ultrasoft state, the soft X-ray spectrum is well-described by an absorbed ( ) black body model, whereas the X-ray spectrum above 20 keV appears to be extremely low and hard (). During the transition, the radio flux rises to a level of >, and the soft X-ray emission drops by a factor of ~3, while the hard X-ray emission rises by a factor of ~14 and becomes steeper (up to ).
Conclusions.The ultrasoft state apparently precedes the emission of a jet, which is apparent in the radio and hard X-ray domain.
Key words: stars: individual: Cyg X-3 / X-rays: binaries / X-rays: individuals: Cyg X-3 / stars: Wolf-Rayet / X-rays: stars / stars: binaries: close
© ESO, 2007
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