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20 April 2024 |
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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 | Abstract: | We 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 | Services: | Forum | Review | PDF | Favorites |
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