The 1998 outburst of the X-ray transient XTE J2012+381 as observed with bepposax (Articolo in rivista)

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  • The 1998 outburst of the X-ray transient XTE J2012+381 as observed with bepposax (Articolo in rivista) (literal)
Anno
  • 2002-01-01T00:00:00+01:00 (literal)
Alternative label
  • 1) Campana S., 2) Stella L., 3) Belloni T., 4) Israel G. L.,5) Santangelo A., 6) Frontera F., 7) Orlandini M., 8) Dal Fiume D. (2002)
    The 1998 outburst of the X-ray transient XTE J2012+381 as observed with bepposax
    (literal)
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  • 1) Campana S., 2) Stella L., 3) Belloni T., 4) Israel G. L.,5) Santangelo A., 6) Frontera F., 7) Orlandini M., 8) Dal Fiume D. (literal)
Pagina inizio
  • 163 (literal)
Pagina fine
  • 170 (literal)
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  • Times cited= 7 Impact Factor= 3.781 (literal)
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  • 384 (literal)
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  • Risultati delle osservazioni del candidato Buco Nero XTE J2012+381 fatte dal satellite BeppoSAX. Viene messo in evidenza la variabilità della componente spettrale dura (PDS) mentre la componente più molle (MECS) rimane costante nelle 5 osservazioni. (literal)
Note
  • ISI Web of Science (WOS) (literal)
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  • 1-3)Osservatorio Astronomico di Brera, via E. Bianchi 46, 23807 Merate (Lecco), Italy),2-4)Osservatorio Astronomico di Roma, via Frascati 33, 00040 Monteporzio Italy), 5)Istituto di Fisica Cosmica e Applicazioni all'Informatica, C.N.R., via La Malfa 153, 90146 Palermo, Italy), 6)Universitàdi Ferrara, Dipartimento di fisica, via Paradiso 12, 44100 Ferrara, Italy; -7)Istituto Tecnologie e Studio Radiazioni Extraterrestri, C.N.R., via Gobetti 101, 40129 Bologna, Italy), (literal)
Titolo
  • The 1998 outburst of the X-ray transient XTE J2012+381 as observed with bepposax (literal)
Abstract
  • We report on the results of a series of X-ray observations of the transient black hole candidate XTE J2012+381 during the 1998 outburst performed with the BeppoSAX satellite. The observed broad-band energy spectrum can be described by the superposition of an absorbed disk black body, with an iron line plus a high energy component, modelled with either a power law or a Comptonisation tail. The source showed pronounced spectral variability between our five observations. While the soft component in the spectrum remained almost unchanged throughout our campaign, we detected a hard spectral tail which extended to 200 keV in the first two observations, but became barely detectable up to 50 keV in the following two. A further re-hardening is observed in the final observation. The transition from a hard to a soft and then back to a hard state occurred around an unabsorbed 0.1-200 keV luminosity of 1038 erg s-1 (at 10 kpc). This indicates that state transitions in XTE 2012+281 are probably not driven only by mass accretion rate, but additional physical parameters must play a role in the evolution of the outburst. (literal)
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