The double-peaked 2008 outburst of the accreting milli-second X-ray pulsar, IGR J00291+5934
. (2010) The double-peaked 2008 outburst of the accreting milli-second X-ray pulsar, IGR J00291+5934. Astronomy & Astrophysics, Vol.517 (No.A72). ISSN 0004-6361
WRAP_Steeghs_double-peaked_aa14382-10.pdf - Draft Version - Requires a PDF viewer such as GSview, Xpdf or Adobe Acrobat Reader
Official URL: http://dx.doi.org/10.1051/0004-6361/201014382
Context. In August 2008, the accreting milli-second X-ray pulsar (AMXP), IGR J00291+5934, underwent an outburst lasting ∼100 days, the first since its discovery in 2004.
Aims. We present data from the 2008 double-peaked outburst of IGR J00291+5934 from Faulkes Telescope North, the Isaac Newton Telescope, the Keck Telescope, PAIRITEL, theWesterbork Synthesis Radio Telescope and the Swift,XMM-Newton and RXTE X-ray missions. We study the outburst’s evolution at various wavelengths, allowing us to probe accretion physics in this AMXP.
Methods. We study the light curve morphology, presenting the first radio-X-ray spectral energy Distributions (SEDs) for this source and the most detailed UV-IR SEDs for any outbursting AMXP. We show simple models that attempt to identify the emission mechanisms responsible for the SEDs. We analyse short-timescale optical variability, and compare a medium resolution optical spectrum with those from 2004.
Results. The outburst morphology is unusual for an AMXP, comprising two peaks, the second containing a “plateau” of ∼10 days at maximum brightness within 30 days of the initial activity. This has implications on duty cycles of short-period X-ray transients. The X-ray spectrum can be fitted by a single, hard power-law. We detect optical variability of ∼0.05 mag, on timescales of minutes,
but find no periodic modulation. In the optical, the SEDs contain a blue component, indicative of an irradiated disc, and a transient near-infrared (NIR) excess. This excess is consistent with a simple model of an optically thick synchrotron jet (as seen in other outbursting
AMXPs), however we discuss other potential origins. The optical spectrum shows a double-peaked Hα profile, a diagnostic of an accretion disc, but we do not clearly see other lines (e.g. He I, II) that were reported in 2004.
Conclusions. Optical/IR observations of AMXPs appear to be excellent for studying the evolution of both the outer accretion disc and the inner jet, and may eventually provide us with tight constraints to model disc-jet coupling in accreting neutron stars.
|Item Type:||Journal Article|
|Subjects:||Q Science > QB Astronomy|
|Divisions:||Faculty of Science > Physics|
|Library of Congress Subject Headings (LCSH):||Pulsars, X-ray sources, Galactic -- Accretion, X-ray bursts, Spectral energy distribution|
|Journal or Publication Title:||Astronomy & Astrophysics|
|Official Date:||July 2010|
|Number of Pages:||15|
|Access rights to Published version:||Open Access|
|Funder:||Dill Faulkes Educational Trust, Nederlandse Organisatie voor Wetenschappelijk Onderzoek [Netherlands Organisation for Scientific Research] (NWO), Science and Technology Facilities Council (Great Britain) (STFC), Harvard University. Milton Fund for Research, Smithsonian Astrophysical Observatory, University of California, Berkeley|
Alpar, M. A., Cheng, A. F., Ruderman, M. A., & Shaham, J. 1982, Nature, 300,
Actions (login required)
Downloads per month over past year