  X-ray binaries, as bright local sources with short variability timescales for
a wide range of accretion processes, represent ideal targets for
high-resolution X-ray spectroscopy. In this chapter, we present a
high-resolution X-ray spectral perspective on X-ray binaries, focusing on black
holes and neutron stars. The majority of the chapter is devoted to
observational and theoretical signatures of mass ejection via accretion disk
winds: we discuss their appearance (including an overview of photoionization
and thermodynamic processes that determine their visibility in X-ray spectra)
and their life cycles (including efforts to constrain their time-dependent mass
loss rates), and we provide a broad overview of the primary accretion disk wind
driving mechanisms that have been considered in the literature: (1) radiation
pressure, where radiation accelerates a wind by scattering off electrons or
atoms in the disk or its atmosphere; (2) thermal driving, where Compton heating
of the outer accretion disk causes gas thermal velocities to exceed the local
escape speed; and (3) magnetohydrodynamic processes, where gas may be ejected
from the disk via magnetic pressure gradients or magnetocentrifugal effects. We
then turn to spectroscopic constraints on the geometry of accreting systems,
from relativistically blurred emission lines to dipping sources, clumpy,
structured stellar winds, and baryonic jets. We conclude with discussions of
measurements of the interstellar medium and the potential of next-generation
high-resolution X-ray spectroscopy for X-ray binaries.
