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(DOI: will be inserted by hand later) The BeppoSAX view on the Galactic Massive X–ray Binary 4U 0114+65

By N. Masetti, M. Orl, D. Dal Fiume, S. Del Sordo, L. Amati, F. Frontera, E. Palazzi and A. Santangelo

Abstract

Abstract. A pointed observation on the galactic high-mass X–ray binary 4U 0114+65 was carried out with BeppoSAX in order to compare the X–ray spectral and timing characteristics observed by this satellite over the broadest range of energies ever (1.5–100 keV) with the information previously obtained with other spacecraft. The light curve of 4U 0114+65 shows a large flare at the beginning of the BeppoSAX pointing and no significant hardness evolution either during the flare or in the low state occurring after the flare itself. The modulation at ∼2.7 hours, attributed to the accreting neutron star (NS) spin periodicity, is not significantly detected in our data, although fluctuations with timescales of ∼3 hours can be seen in the 2–10 keV light curve. Shorter modulations down to timescales of minutes, are also found and interpreted as due to accretion of matter onto the NS. The flaring and the low state spectra of 4U 0114+65 can be equally well fitted either with a power law modulated by a high-energy exponential cutoff or with a Comptonization model. During the low state the presence, although tentative, of a thermal component (with kT ∼ 0.3 keV) at low energies, possibly produced by an ionized plasma cloud around the NS, cannot be excluded. Contrary to previous claims, a cyclotron resonant feature in absorption at ∼22 keV was not detected in the BeppoSAX spectroscopic data, whereas evidence for a Fe emission line aroun

Year: 2005
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