The bursting pulsar GRO J1744–28 is a Galactic low-mass X-ray binary that distinguishes itself by displaying type-II X-ray bursts : brief , bright flashes of X-ray emission that likely arise from spasmodic accretion . Combined with its coherent 2.1 Hz X-ray pulsations and relatively high estimated magnetic field , it is a particularly interesting source to study the physics of accretion flows around neutron stars . Here we report on Chandra /HETG observations obtained near the peak of its bright 2014 accretion outburst . Spectral analysis suggests the presence of a broad iron emission line centered at E _ { \mathrm { l } } \simeq 6.7 keV . Fits with a disk reflection model yield an inclination angle of i \simeq 52 ^ { \circ } and an inner disk radius of R _ { \mathrm { in } } \simeq 85 ~ { } GM / c ^ { 2 } , which is much further out than typically found for neutron star low-mass X-ray binaries . Assuming that the disk is truncated at the magnetospheric radius of the neutron star , we estimate a magnetic field strength of B \simeq ( 2 - 6 ) \times 10 ^ { 10 } G. Furthermore , we identify an absorption feature near \simeq 6.85 keV that could correspond to blue-shifted Fe xxv and point to a fast disk wind with an outflow velocity of v _ { \mathrm { out } } \simeq ( 7.5 - 8.2 ) \times 10 ^ { 3 } ~ { } \mathrm { km~ { } s } ^ { -1 } ( \simeq 0.025 c - 0.027 c ) . If the covering fraction and filling factor are large , this wind could be energetically important and perhaps account for the fact that the companion star lost significant mass while the magnetic field of the neutron star remained strong .