HAUMEA IS A DWARF PLANET IN THE KUIPER BELT THAT IS A RAPID ROTATOR (P=3.9 HR) WITH A PRONOUNCED LIGHT CURVE DESPITE AN APPARENTLY UNIFORM SURFACE IMPLYING A TRIAXIAL ELLIPSOID SHAPE CONSISTENT WITH A JACOBI ELLIPSOID. HAUMEA POSSESSES TWO MOONS AND A RING AND IS THE ONLY KUIPER BELT OBJECT WITH A KNOWN COLLISIONAL FAMILY OF ABOUT A DOZEN ICY FRAGMENTS . IT IS INFERRED TO HAVE SUFFERED A LARGE COLLISION IN THE PAST THAT STRIPPED ITS ICY MANTLE. HAUMEA THEREFORE OFFERS A UNIQUE OPPORTUNITY TO PROBE THE INTERIOR OF AN ICY BODY AND TO INVESTIGATE THE PROPERTIES OF MANTLE-STRIPPING COLLISIONS. THESE ARE PROCESSES ONGOING THROUGHOUT THE SOLAR SYSTEM. THE FIRST GOAL IS TO CONSTRAIN THE SIZE AND SHAPE OF HAUMEA AND THE SIZE AND SHAPE OF ITS ROCKY CORE. UNTIL THIS YEAR IT WAS THOUGHT THAT HAUMEA HAD A LARGE ROCKY CORE AND THIN ICE MANTLE BUT NEW OBSERVATIONS OF HAUMEA'S SHADOW DURING AN OCCULTATION EVENT BY ORTIZ ET AL. (2017) INDICATE A LARGE ICY MANTLE AND POSSIBLY A SHAPE NOT CONSISTENT WITH A FLUID IN HYDROSTATIC EQUILIBRIUM. IT IS IMPORTANT TO CONSTRAIN THE ORIGINS OF THE HAUMEA COLLISIONAL FAMILY TO LEARN ABOUT MANTLE-STRIPPING EVENTS GENERALLY. THERE ARE VARIOUS THEORIES ABOUT ITS ORIGIN INCLUDING THE LEINHARDT ET AL. (2010) "GRAZE-AND-MERGE" SCENARIO AND THE SCHLICHTING&SARI (2009) MOON DISRUPTION SCENARIO. THE LEINHARDT ET AL. (2010) SCENARIO IS CONSISTENT WITH THE ANGULAR MOMENTUM OF HAUMEA BUT NOT AS OBVIOUSLY WITH THE LOW MASS OF EJECTED ICE AND THE LOW DELTA V OF THE COLLISIONAL FAMILY MEMBERS. THE SCHLICHTING&SARI (2009) SCENARIO IS CONSISTENT WITH THE LOW DELTA V BUT REQUIRES TIDAL MIGRATION OF AN IMPACT-FORMED MOON AND IS LESS PROBABLE.