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 5 \sigma 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 = 0.04 c .
This interpretation is preferred at the 4 \sigma level over a scenario in which the line is H-like Fe XXVI at a modest red-shift .
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 ( BALQSOs ) .
If the gas has a unity volume filling factor , the mass ouflow rate in the wind is over 10 ^ { -5 } ~ { } M _ { \odot } ~ { } { yr } ^ { -1 } , and the kinetic power is nearly 10 ^ { 39 } ~ { } { 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 .