2000ApJ...528..702S

We present RXTE observations of LMC X-2 obtained during a 5 day interval in 1997 December, during which the source was radiating at a mean intensity near the Eddington limit and was strongly variable on timescales of seconds to hours. The shapes of the X-ray color-color and hardness-intensity diagrams during the observations, the presence of very low frequency noise and high-frequency noise in the power spectra, and the high intrinsic X-ray luminosity of LMC X-2 (which historically spans 0.4-2.0L_Edd for reasonable estimates of the neutron star mass) are more characteristic of a Z source in its flaring branch than of an atoll source. On this basis, we provisionally reclassify LMC X-2 as a Z source, the eighth such source known and the first to be detected beyond our Galaxy. Using periodogram and Fourier analysis of the X-ray light curve, we detect an apparently significant modulation with a period of 8.160±0.011 hr and a semiamplitude increasing from 14% in the 1.8-4.0 keV range to 40% at 8.7-19.7 keV. This X-ray modulation appears to confirm a candidate orbital periodicity determined from optical photometry 10 years prior to our campaign, but we cannot rule out a chance alignment of intrinsic X-ray flares. Current RXTE All-Sky Monitor light curves and archival EXOSAT observations show no sign of such a pronounced periodicity. The X-ray spectrum of LMC X-2 can be well fit using variations of simple Comptonization models. Fits to phase (≃intensity) resolved spectra show strong correlations between the power-law slope (in one parameterization) or the depth to optical scattering (in another) and phase. We discuss the implications of these results for the inclination, geometry, and emitting regions of the LMC X-2 system.