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20 April 2024
 
  » arxiv » 1109.3924

 Article overview


X-Ray and Optical Observations of A 0535+26
A. Camero-Arranz ; M. H. Finger ; C. A. Wilson-Hodge ; P. Jenke ; I. Steele ; M. J. Coe ; J. Gutierrez-Soto ; P. Kretschmar ; I. Caballero ; G. Case ; M. L. Cherry ; J. Yan ; J. Suso ; J. Rodríguez ; S. Guiriec ; V. A. McBride ;
Date 19 Sep 2011
AbstractWe present recent contemporaneous X-ray and optical observations of the Be/X-ray binary system A 0535+26 with the Fermi/Gamma-ray Burst Monitor (GBM) and several ground-based observatories. These new observations are put into the context of the rich historical data and discussed in terms of the neutron star Be-disk interaction. The Be circumstellar disk was exceptionally large just before the 2009 December giant outburst, which may explain the origin of the unusual recent X-ray activity of this source. We found a peculiar evolution of the pulse profile during this giant outburst, with the two main components evolving in opposite ways with energy. A hard 30-70 mHz X-ray QPO was detected with GBM during this 2009 December giant outburst. It becomes stronger with increasing energy and disappears at energies below 25 keV. In the long-term a strong optical/X-ray correlation was found for this system, however in the medium-term the H{alpha} EW and the V-band brightness showed an anti-correlation after sim2002 August. Each giant X-ray outburst occurred during a decline phase of the optical brightness, while the H{alpha} showed a strong emission. In late 2010 and before the 2011 February outburst, rapid V/R variations are observed in the strength of the two peaks of the H{alpha} line. These had a period of sim25 days and we suggest the presence of a global one-armed oscillation to explain this scenario. A general pattern might be inferred, where the disk becomes weaker and shows V/R variability beginning sim6 months following a giant outburst.
Source arXiv, 1109.3924
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