STELLAR OSCILLATION MODES KNOWN AS R-MODES CAN CONVERT ROTATIONAL ENERGY OF FAST SPINNING NEUTRON STARS INTO GRAVITATIONAL WAVES AND INTERNAL HEATING. BY MEASURING X-RAY FLUX FROM THE HOT SURFACE OF RAPIDLY ROTATING PULSARS WE CAN CONSTRAIN THE PHYSICS THAT GOVERN R-MODES SUCH AS THE STATE OF NUCLEAR MATTER. WITH A SPIN RATE OF 707 HZ PSR J0952-0607 IS THE FASTEST-SPINNING PULSAR KNOWN OUTSIDE A GLOBULAR CLUSTER. THE LOW INTERVENING NH (4 X 1020 CM-2) AND SMALL SOURCE DISTANCE (0.97-1.74 KPC) INDICATE THAT AN XMM-NEWTON OBSERVATION CAN SIGNIFICANTLY IMPROVE UPON THE X-RAY FLUX CONSTRAINT OBTAINED BY SWIFT. PSR J0952-0607 IS THUS AN EXCELLENT TARGET FOR INVESTIGATING WHAT LIMITS THE SPIN EVOLUTION OF MILLISECOND PULSARS. FINALLY MODELING OF A NONTHERMAL COMPONENT OF THE X-RAY SPECTRUM CAN YIELD VALUABLE INSIGHTS INTO THE INTRABINARY SHOCK BETWEEN PSR J0952-0607 AND ITS COMPANION STAR.