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We present a spectral analysis of a brief Chandra/HETG observation of theneutron star low-mass X-ray binary GX~340+0. The high-resolution spectrumreveals 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 levelof confidence via an F-test. Photoionization modeling with XSTAR grids suggeststhat the line is the most prominent part of a disk wind with an apparentoutflow speed of v = 0.04c. This interpretation is preferred at the 4 sigmalevel over a scenario in which the line is H-like Fe XXVI at a modestred-shift. The wind may achieve this speed owing to its relatively lowionization, enabling driving by radiation pressure on lines; in this sense, thewind in GX 340+0 may be the stellar-mass equivalent of the flows in broadabsorption line quasars (BALQSOs). If the gas has a unity volume fillingfactor, the mass ouflow rate in the wind is over 10^-5 Msun/year, and thekinetic power is nearly 10^39 erg/s (or, 5-6 times the radiative Eddingtonlimit for a neutron star). However, geometrical considerations - including asmall volume filling factor and low covering factor - likely greatly reducethese values.

An Ultra-Fast X-ray Disk Wind in the Neutron Star Binary GX 340+0