AN ULTRA-FAST X-RAY DISK WIND IN THE NEUTRON STAR BINARY GX 340+0
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Author(s)
Miller, J. M.
Raymond, J.
Cackett, E.
Grinberg, Victoria
Nowak, Michael A.
Date Issued
April 2016
Journal
Astrophysical Journal. Letters
Publisher
IOP Publishing
Citation
Miller, J. M., J. Raymond, E. Cackett, V. Grinberg, and M. Nowak. “AN ULTRA-FAST X-RAY DISK WIND IN THE NEUTRON STAR BINARY GX 340+0.” The Astrophysical Journal 822, 1 (April 2016): L18 © 2016 The American Astronomical Society
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Final published version
Abstract
We present a spectral analysis of a brief Chandra/HETG observation of the neutron star low-mass X-ray binary GX 340+0. The high-resolution spectrum reveals evidence of ionized absorption in the Fe K band. The strongest feature, an absorption line at approximately 6.9 keV, is required at the 5σ level of confidence via an F-test. Photoionization modeling with XSTAR grids suggests that the line is the most prominent part of a disk wind with an apparent outflow speed of v = 0.04c. This interpretation is preferred at the 4σ level over a scenario in which the line is H-like Fe xxvi at a modest redshift. The wind may achieve this speed owing to its relatively low ionization, enabling driving by radiation pressure on lines; in this sense, the wind in GX 340+0 may be the stellar-mass equivalent of the flows in broad absorption line quasars. If the gas has a unity volume filling factor, the mass ouflow rate in the wind is over 10⁻⁵ M ⊙ yr⁻¹, and the kinetic power is nearly 10³⁹ erg s⁻¹ (or, 5–6 times the radiative Eddington limit for a neutron star). However, geometrical considerations—including a small volume filling factor and low covering factor—likely greatly reduce these values.
MIT Department
MIT Kavli Institute for Astrophysics and Space Research
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DOI of Published Version
https://doi.org/10.3847/2041-8205/822/1/l18
