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23 April 2024 |
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INTEGRAL and Swift observations of EXO 2030+375 during a giant outburst | | D. Klochkov
; D. Horns
; A. Santangelo
; R. Staubert
; A. Segreto
; C. Ferrigno
; P. Kretschmar
; I. Kreykenbohm
; A. La Barbera
; N. Masetti
; M. McCollough
; K. Pottschmidt
; G. Schoenherr
; J. Wilms
; | | Date: |
27 Jan 2007 | | Abstract: | Aims: We investigate the X-ray spectral and timing properties of the high mass X-ray binary EXO 2030+375 observed during its June-September 2006 giant (type II) outburst. Methods: The data analyzed in this work are from partly simultaneous observations with INTEGRAL Swift. The pulse period P and its temporal derivative P_dot are measured. X-ray pulse profiles in different energy ranges and time intervals are constructed. Pulse averaged X-ray spectra for different time intervals are studied. Results: We report a strong spin-up of the source during the outburst, comparable to that observed in 1985 during the previous giant outburst when the source was discovered. The value of P_dot is found to be linearly related to the X-ray luminosity of the source during the outburst. For the first time the hard X-ray (>25 keV) characteristics of the source during a type II outburst are studied. The X-ray pulse profiles apparently change with luminosity. The X-ray spectral continuum in the 3--120 keV energy range is modeled with an absorbed power law with an exponential cutoff around E ~26 keV. An iron emission line at ~6-7 keV is observed. The spectrum reveals some features between 10 and 20 keV which can be modeled either by a broad emission line at ~13-15 keV (a ``bump’’) or by two absorption lines at ~10 and ~20 keV. | | Source: | arXiv, astro-ph/0701791 | | Services: | Forum | Review | PDF | Favorites | |
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