ASTEROID 2008 TC3 WAS TRACKED AND STUDIED FOR ~19 HOURS BEFORE IT IMPACTED IN SUDAN IN OCTOBER 2008. SEARCH CAMPAIGNS IN THE PREDICTED FALL AREA LED BY CO-IS SHADDAD AND JENNISKENS RECOVERED ~600 STONES (~0.2-400 G EACH) THAT WERE NAMED THE ALMAHATA SITTA (AHS) METEORITE. AHS IS THE FIRST METEORITE OBSERVED TO ORIGINATE FROM A SPECTRALLY CLASSIFIED ASTEROID AND PROVIDES AN UNPRECEDENTED OPPORTUNITY TO CORRELATE PROPERTIES OF A METEORITE WITH PROPERTIES OF THE ASTEROID FROM WHICH IT WAS DERIVED. 2008 TC3 WAS ALSO THE FIRST NEAR-EARTH OBJECT (NEO) DETECTED BEFORE IT IMPACTED EARTH WHICH MAKES IT UNIQUE FOR STUDIES IN PLANETARY DEFENSE. THE MAIN AHS COLLECTION IS CURATED AT THE UNIVERSITY OF KHARTOUM (UOK) BY CO-I SHADDAD DOCUMENTED WITH FIND COORDINATES FOR EACH STONE IN THE STREWN FIELD. STUDIES OF 85 OF THESE STONES (61 BY OUR TEAM UNDER A 1-YEAR PROOF-OF-CONCEPT GRANT FROM EMERGING WORLDS) HAVE SHOWN THAT AHS IS A REMARKABLE METEORITE. APPROXIMATELY 80% OF THE STONES ARE UREILITES (CARBON-RICH ULTRAMAFIC ACHONDRITES) WHILE ~20% ARE VARIOUS TYPES OF CHONDRITES SO AHS IS CLASSIFIED AS AN ANOMALOUS POLYMICT UREILITE. FAR FROM BEING A COHERENT MONOLITHOLOGIC ROCK IN SPACE ASTEROID 2008 TC3 WAS A LOOSELY AGGREGATED HETEROGENEOUS OBJECT THAT DISINTEGRATED IN THE ATMOSPHERE WITH ITS CLASTS LANDING ON EARTH AS INDIVIDUAL STONES. DETERMINING THE PHYSICAL AND COMPOSITIONAL STRUCTURE OF THIS ASTEROID IS CRITICAL TO UNDERSTANDING ITS FORMATION THE PROVENANCE OF ITS COMPONENTS ITS ORBITAL AND COLLISIONAL HISTORY AND THE FATE OF RELATED ASTEROIDAL FRAGMENTS. IT IS ALSO OF PARAMOUNT IMPORTANCE TO THE GOALS OF THE NEO PROGRAM AND MISSIONS TO ASTEROIDS. COMPLETE CLASSIFICATION OF THE UOK COLLECTION IS NEEDED TO DETERMINE THE PHYSICAL AND COMPOSITIONAL STRUCTURE OF 2008 TC3. OUR PROOF-OF-CONCEPT WORK SHOWED THAT AHS IS EXTREMELY HETEROGENEOUS AND REVEALED THE FIRST AHS STONES TO CONSIST OF BOTH UREILITIC AND CHONDRITIC MATERIALS. IT IS VIRTUALLY CERTAIN THAT THE REST OF THE COLLECTION HARBORS NEW MATERIALS. FURTHERMORE THE DOCUMENTATION OF FIND COORDINATES FOR EACH STONE ALLOWS DETERMINATION OF THE SPATIAL DISTRIBUTION OF DIFFERENT MATERIALS IN THE ASTEROID. WE PROPOSE TO SELECT AND STUDY ~150 NEW STONES (IN 3 YEARS) FROM THE UOK COLLECTION. THE OBJECTIVES ARE: 1) TO DETERMINE THE FULL DIVERSITY AND PROPORTIONS OF ROCK TYPES AMONG AHS STONES; 2) TO DETERMINE THE PHYSICAL AND COMPOSITIONAL STRUCTURE OF ASTEROID 2008 TC3 INCLUDING GRAIN SIZE AND DISTRIBUTION AND ROCK TYPE DISTRIBUTION; 3) TO CONSTRAIN THE ORIGIN AND HISTORY OF 2008 TC3 INCLUDING MECHANISM(S) AND TIMING OF FORMATION PROVENANCE OF CONSTITUENT MATERIALS COLLISIONAL EVENTS ORBITAL EVOLUTION AND IDENTIFICATION OF RELATED ASTEROIDS. TO ACCOMPLISH THESE WE WILL USE A BATTERY OF ANALYTICAL AND MODELING TECHNIQUES INCLUDING: FE-SEM EMPA AND FIB/TEM (MINERALOGY AND PETROLOGY); BULK AND SIMS OXYGEN ISOTOPE ANALYSIS; VNIR MIR AND MICRO-FTIR REFLECTANCE SPECTROSCOPY; CR ISOTOPE ANALYSIS; AR-AR DATING; NOBLE GAS AND COSMOGENIC NUCLIDE ANALYSIS; LEAST-SQUARES MODELING OF THE 2008 TC3 REFLECTANCE SPECTRUM AND; PREDICTIVE MODELING OF REFLECTANCE SPECTRA OF RELATED ASTEROIDS. THE PROPOSED WORK IS A SERENDIPITOUS ASTEROID SAMPLE RETURN MISSION RELEVANT TO THE STRATEGIC SCIENCE GOAL OF EW TO EXPLORE AND OBSERVE THE OBJECTS IN THE SOLAR SYSTEM TO UNDERSTAND HOW THEY FORMED AND EVOLVED. IT IS AN INTERDISCIPLINARY EFFORT UNITING METEORITE PETROLOGY AND GEOCHEMISTRY WITH ASTEROID SPECTROSCOPY AND METEOR ASTRONOMY TO ADDRESS THE KEY QUESTION OF HOW A HETEROGENEOUS RUBBLE PILE-LIKE ASTEROID FORMED EVOLVED AND EVENTUALLY IMPACTED EARTH. RESULTS WILL AID IN THE DEVELOPMENT OF MISSIONS TO ASTEROIDS. THE WORK ADDRESSES PROCESSES OF ACCRETION COLLISIONAL MIXING OF INNER AND OUTER SOLAR SYSTEM MATERIALS AND REGOLITH FORMATION IN THE EARLY SOLAR SYSTEM BEFORE THE PLANETS WERE IN THEIR MODERN CONFIGURATION AND IS THUS RELEVANT TO EW.