the view that we are directly seeing the "epicyclic" periods general relativity predicts for the orbital motion of test particles: one related to the well-known general-relativistic precession of Mercury's orbit (but lOI7 times faster because of the strong gravity) and another to the so-called "Lense-Thirring precession" of the orbital plane itself, caused by ''fhne-dragging," a phenomenon in which a spinning object drags space-time around it along with its spin (9). But there seems to be more to it than that. RXTE has discovered the f i t millisecond pulsar in an x-ray binary, a neutron star spinning with a 2.493919753-ms period (lo), and has measured the approximate spins of another six neutron stars with periods of 2 to 4 ms (11). Comparison of these spins with the millisecond quasi-periods suggests that while the fastest of the two quasi-periods seen in each system originates in the orbital motion in the accretion disk, the slower one (still sometimes as fast as 1.2 msec) arises by a nonlinear interaction (a "beat") between the spin and the orbital motion. One model describes a pattern of orbital motion that could explain the observations in detail (7). A few more years of observations, more discoveries, and further high-precision measurements of the new ~henomena will show which of these theories can be maintained and which must be abandoned.RXTE's success has demonstrated that when probing the dynamics in strongly curved space-time, there is no substitute for size. It is the huge effective area of 0.7 m2 of the main x-ray instrument onboard the satellite that gave Rossi the sensitivity to make the first direct measurements of orbital motion near collapsed stars. To fully exploit these discoveries and map out space-time near neutron stars and black holes, an instrument in the 10-m2 class will be required. Although the stream of new data from RXTE continues unabated and a second millisecond timing mission (the Naval Research Laboratory's Unconventional Stellar Aspect experiment on the Argos satellite) was just launched successfully, x-ray astronomers are already considering the new solid-state technologies by which such a "relativity explorer" might be realized. References and Notes 1. H.V. Bradt. R. E. Rothschild.]. H. Swank. Astmn. Astmphys. 97.355 (1993). 2. 1. H. Taylor and 1. M. Weisberg. Astrophys.]. 345.434 (1989). 3. M. van der Klis et al.. ibid. 469. L1 (1996); T. E. Strohmayer et al.. ibid., p. L9. 4. M. van der Klis, preprint available at xxx.lanl.gov/absl astro-phl9812395. 5. E. H. Morgan etal..Astrophys.