4 INVESTIGATING THE INTERACTION OF SOLAR WIND PROTONS WITH THE MOON USING ARTEMIS DATA GOALS/OBJECTIVES: THE PRIMARY GOAL OF THIS PROPOSAL IS TO ANALYZE ARTEMIS OBSERVATIONS OF SOLAR WIND PROTONS REFLECTED AT OR NEAR THE MOON IN ORDER TO UNDERSTAND THE INTERACTION OF THE SOLAR WIND WITH THE LUNAR SURFACE AND PLASMA ENVIRONMENT. SPECIFICALLY, WE AIM TO ANSWER THE FOLLOWING QUESTIONS: 1. WHAT ARE THE CHARACTERISTICS OF PROTONS REFLECTED FROM THE UN-MAGNETIZED SURFACE AND WHAT DO THEY IMPLY ABOUT THE INTERACTION OF THE SOLAR WIND WITH LUNAR REGOLITH? 2. WHAT ARE THE CHARACTERISTICS OF PROTONS REFLECTED ABOVE MAGNETIZED REGIONS, AND WHAT DO THEY IMPLY ABOUT THE INTERACTION OF THE SOLAR WIND WITH LUNAR CRUSTAL MAGNETIC FIELDS? 3. HOW DO REFLECTED PROTONS SUBSEQUENTLY INTERACT WITH AND/OR MODIFY THE LUNAR SURFACE AND PLASMA ENVIRONMENT? METHODOLOGY: THIS PROPOSAL WILL MAKE USE OF THREE YEARS OF PUBLICLY AVAILABLE DATA (2011-2014) RETURNED BY BOTH PROBES OF THE ACCELERATION, RECONNECTION, TURBULENCE, AND ELECTRODYNAMICS OF THE MOON'S INTERACTION WITH THE SUN (ARTEMIS) MISSION. THE ARTEMIS PROBES MEASURE COMPLETE ENERGY- AND ANGLE-RESOLVED ION AND ELECTRON DISTRIBUTIONS AND MAGNETIC AND ELECTRIC FIELDS, COVERING ALTITUDES FROM 20-20,000 KM, FOR A WIDE RANGE OF LOCAL TIMES AND SELENOGRAPHIC LOCATIONS. WE WILL IDENTIFY REFLECTED SOLAR WIND PROTONS AND CHARACTERIZE THEIR ENERGY AND ANGULAR DISTRIBUTIONS, THEIR DEPENDENCE ON SOLAR WIND CONDITIONS, AND THE LOCATION OF THEIR REFLECTION FROM THE LUNAR SURFACE AND/OR CRUSTAL MAGNETIC FIELDS (TAKING INTO ACCOUNT THE PATH FROM THEIR REFLECTION POINT THROUGH THE COMPLEX MAGNETIC AND ELECTRIC FIELDS AROUND THE MOON). THE RESULT WILL BE A QUANTITATIVE UNDERSTANDING OF HOW PROTONS REFLECT FROM BOTH LUNAR REGOLITH (THE EQUIVALENT OF THE HAPKE PARAMETERS FOR PHOTONS) AND FROM LUNAR CRUSTAL MAGNETIC FIELDS (REFLECTING THE UNIQUE PLASMA PHYSICS ASSOCIATED WITH SMALL-SCALE LUNAR FIELDS). TO QUANTIFY THE EFFECT THAT SPATIALLY AND TEMPORALLY VARIABLE PROTON REFLECTION HAS ON THE SURFACE, WE WILL TRACE REFLECTED PROTON TRAJECTORIES BOTH FORWARDS AND BACKWARDS TO ESTIMATE (1) LOCATIONS WHERE THE SURFACE IS SHIELDED FROM PROTON BOMBARDMENT, THUS MODIFYING THE LOCAL SURFACE CHEMISTRY AND REDUCING THE SPUTTERING OF REGOLITH MATERIAL INTO THE EXOSPHERE AND (2) LOCATIONS WHERE SECONDARY REFLECTED PROTON IMPACT COULD ENHANCE SPUTTERING. THE EFFECTS ON THE NEAR-LUNAR PLASMA ENVIRONMENT WILL BE QUANTIFIED BY (1) IDENTIFYING AND CHARACTERIZING SHOCKS AND/OR INSTABILITIES DRIVEN BY REFLECTED PROTONS AND (2) COMPARING ARTEMIS OBSERVATIONS OF LUNAR WAKE PROCESSES IN THE PRESENCE OF REFLECTED SOLAR WIND PROTONS TO CASES WHEN THEY ARE ABSENT. RELEVANCE: THE PROPOSED WORK IS DIRECTLY RELEVANT TO THE LUNAR DATA ANALYSIS PROGRAM (LDAP), WHICH SEEKS TO "...FUND RESEARCH ON THE ANALYSIS OF RECENT LUNAR MISSIONS IN ORDER TO ENHANCE THEIR SCIENTIFIC RETURN." BY CHARACTERIZING THE POTENTIAL EFFECT THAT REFLECTED PROTONS MIGHT HAVE ON SURFACE SPUTTERING, WE ADDRESS A HIGH-PRIORITY GOAL OF LDAP: "CHARACTERIZATION OF THE GLOBAL VARIABILITY AND STRUCTURE OF THE LUNAR EXOSPHERE". Funding Only Action ($43) 11/21/19 Not listed INVESTIGATING THE INTERACTION OF SOLAR WIND PROTONS WITH THE MOON USING ARTEMIS DATA GOALS/OBJECTIVES: THE PRIMARY GOAL OF THIS PROPOSAL IS TO ANALYZE ARTEMIS OBSERVATIONS OF SOLAR WIND PROTONS REFLECTED AT OR NEAR THE MOON IN ORDER TO UNDERSTAND THE INTERACTION OF THE SOLAR WIND WITH THE LUNAR SURFACE AND PLASMA ENVIRONMENT. SPECIFICALLY WE AIM TO ANSWER THE FOLLOWING QUESTIONS: 1. WHAT ARE THE CHARACTERISTICS OF PROTONS REFLECTED FROM THE UN-MAGNETIZED SURFACE AND WHAT DO THEY IMPLY ABOUT THE INTERACTION OF THE SOLAR WIND WITH LUNAR REGOLITH? 2. WHAT ARE THE CHARACTERISTICS OF PROTONS REFLECTED ABOVE MAGNETIZED REGIONS AND WHAT DO THEY IMPLY ABOUT THE INTERACTION OF THE SOLAR WIND WITH LUNAR CRUSTAL MAGNETIC FIELDS? 3. HOW DO REFLECTED PROTONS SUBSEQUENTLY INTERACT WITH AND/OR MODIFY THE LUNAR SURFACE AND PLASMA ENVIRONMENT? METHODOLOGY: THIS PROPOSAL WILL MAKE USE OF THREE YEARS OF PUBLICLY AVAILABLE DATA (2011-2014) RETURNED BY BOTH PROBES OF THE ACCELERATION RECONNECTION TURBULENCE AND ELECTRODYNAMICS OF THE MOON'S INTERACTION WITH THE SUN (ARTEMIS) MISSION. THE ARTEMIS PROBES MEASURE COMPLETE ENERGY- AND ANGLE-RESOLVED ION AND ELECTRON DISTRIBUTIONS AND MAGNETIC AND ELECTRIC FIELDS COVERING ALTITUDES FROM 20-20 000 KM FOR A WIDE RANGE OF LOCAL TIMES AND SELENOGRAPHIC LOCATIONS. WE WILL IDENTIFY REFLECTED SOLAR WIND PROTONS AND CHARACTERIZE THEIR ENERGY AND ANGULAR DISTRIBUTIONS THEIR DEPENDENCE ON SOLAR WIND CONDITIONS AND THE LOCATION OF THEIR REFLECTION FROM THE LUNAR SURFACE AND/OR CRUSTAL MAGNETIC FIELDS (TAKING INTO ACCOUNT THE PATH FROM THEIR REFLECTION POINT THROUGH THE COMPLEX MAGNETIC AND ELECTRIC FIELDS AROUND THE MOON). THE RESULT WILL BE A QUANTITATIVE UNDERSTANDING OF HOW PROTONS REFLECT FROM BOTH LUNAR REGOLITH (THE EQUIVALENT OF THE HAPKE PARAMETERS FOR PHOTONS) AND FROM LUNAR CRUSTAL MAGNETIC FIELDS (REFLECTING THE UNIQUE PLASMA PHYSICS ASSOCIATED WITH SMALL-SCALE LUNAR FIELDS). TO QUANTIFY THE EFFECT THAT SPATIALLY AND TEMPORALLY VARIABLE PROTON REFLECTION HAS ON THE SURFACE WE WILL TRACE REFLECTED PROTON TRAJECTORIES BOTH FORWARDS AND BACKWARDS TO ESTIMATE (1) LOCATIONS WHERE THE SURFACE IS SHIELDED FROM PROTON BOMBARDMENT THUS MODIFYING THE LOCAL SURFACE CHEMISTRY AND REDUCING THE SPUTTERING OF REGOLITH MATERIAL INTO THE EXOSPHERE AND (2) LOCATIONS WHERE SECONDARY REFLECTED PROTON IMPACT COULD ENHANCE SPUTTERING. THE EFFECTS ON THE NEAR-LUNAR PLASMA ENVIRONMENT WILL BE QUANTIFIED BY (1) IDENTIFYING AND CHARACTERIZING SHOCKS AND/OR INSTABILITIES DRIVEN BY REFLECTED PROTONS AND (2) COMPARING ARTEMIS OBSERVATIONS OF LUNAR WAKE PROCESSES IN THE PRESENCE OF REFLECTED SOLAR WIND PROTONS TO CASES WHEN THEY ARE ABSENT. RELEVANCE: THE PROPOSED WORK IS DIRECTLY RELEVANT TO THE LUNAR DATA ANALYSIS PROGRAM (LDAP) WHICH SEEKS TO "...FUND RESEARCH ON THE ANALYSIS OF RECENT LUNAR MISSIONS IN ORDER TO ENHANCE THEIR SCIENTIFIC RETURN." BY CHARACTERIZING THE POTENTIAL EFFECT THAT REFLECTED PROTONS MIGHT HAVE ON SURFACE SPUTTERING WE ADDRESS A HIGH-PRIORITY GOAL OF LDAP: "CHARACTERIZATION OF THE GLOBAL VARIABILITY AND STRUCTURE OF THE LUNAR EXOSPHERE". ($43) 11/21/19 3 INVESTIGATING THE INTERACTION OF SOLAR WIND PROTONS WITH THE MOON USING ARTEMIS DATA GOALS/OBJECTIVES: THE PRIMARY GOAL OF THIS PROPOSAL IS TO ANALYZE ARTEMIS OBSERVATIONS OF SOLAR WIND PROTONS REFLECTED AT OR NEAR THE MOON IN ORDER TO UNDERSTAND THE INTERACTION OF THE SOLAR WIND WITH THE LUNAR SURFACE AND PLASMA ENVIRONMENT. SPECIFICALLY, WE AIM TO ANSWER THE FOLLOWING QUESTIONS: 1. WHAT ARE THE CHARACTERISTICS OF PROTONS REFLECTED FROM THE UN-MAGNETIZED SURFACE AND WHAT DO THEY IMPLY ABOUT THE INTERACTION OF THE SOLAR WIND WITH LUNAR REGOLITH? 2. WHAT ARE THE CHARACTERISTICS OF PROTONS REFLECTED ABOVE MAGNETIZED REGIONS, AND WHAT DO THEY IMPLY ABOUT THE INTERACTION OF THE SOLAR WIND WITH LUNAR CRUSTAL MAGNETIC FIELDS? 3. HOW DO REFLECTED PROTONS SUBSEQUENTLY INTERACT WITH AND/OR MODIFY THE LUNAR SURFACE AND PLASMA ENVIRONMENT? METHODOLOGY: THIS PROPOSAL WILL MAKE USE OF THREE YEARS OF PUBLICLY AVAILABLE DATA (2011-2014) RETURNED BY BOTH PROBES OF THE ACCELERATION, RECONNECTION, TURBULENCE, AND ELECTRODYNAMICS OF THE MOON'S INTERACTION WITH THE SUN (ARTEMIS) MISSION. THE ARTEMIS PROBES MEASURE COMPLETE ENERGY- AND ANGLE-RESOLVED ION AND ELECTRON DISTRIBUTIONS AND MAGNETIC AND ELECTRIC FIELDS, COVERING ALTITUDES FROM 20-20,000 KM, FOR A WIDE RANGE OF LOCAL TIMES AND SELENOGRAPHIC LOCATIONS. WE WILL IDENTIFY REFLECTED SOLAR WIND PROTONS AND CHARACTERIZE THEIR ENERGY AND ANGULAR DISTRIBUTIONS, THEIR DEPENDENCE ON SOLAR WIND CONDITIONS, AND THE LOCATION OF THEIR REFLECTION FROM THE LUNAR SURFACE AND/OR CRUSTAL MAGNETIC FIELDS (TAKING INTO ACCOUNT THE PATH FROM THEIR REFLECTION POINT THROUGH THE COMPLEX MAGNETIC AND ELECTRIC FIELDS AROUND THE MOON). THE RESULT WILL BE A QUANTITATIVE UNDERSTANDING OF HOW PROTONS REFLECT FROM BOTH LUNAR REGOLITH (THE EQUIVALENT OF THE HAPKE PARAMETERS FOR PHOTONS) AND FROM LUNAR CRUSTAL MAGNETIC FIELDS (REFLECTING THE UNIQUE PLASMA PHYSICS ASSOCIATED WITH SMALL-SCALE LUNAR FIELDS). TO QUANTIFY THE EFFECT THAT SPATIALLY AND TEMPORALLY VARIABLE PROTON REFLECTION HAS ON THE SURFACE, WE WILL TRACE REFLECTED PROTON TRAJECTORIES BOTH FORWARDS AND BACKWARDS TO ESTIMATE (1) LOCATIONS WHERE THE SURFACE IS SHIELDED FROM PROTON BOMBARDMENT, THUS MODIFYING THE LOCAL SURFACE CHEMISTRY AND REDUCING THE SPUTTERING OF REGOLITH MATERIAL INTO THE EXOSPHERE AND (2) LOCATIONS WHERE SECONDARY REFLECTED PROTON IMPACT COULD ENHANCE SPUTTERING. THE EFFECTS ON THE NEAR-LUNAR PLASMA ENVIRONMENT WILL BE QUANTIFIED BY (1) IDENTIFYING AND CHARACTERIZING SHOCKS AND/OR INSTABILITIES DRIVEN BY REFLECTED PROTONS AND (2) COMPARING ARTEMIS OBSERVATIONS OF LUNAR WAKE PROCESSES IN THE PRESENCE OF REFLECTED SOLAR WIND PROTONS TO CASES WHEN THEY ARE ABSENT. RELEVANCE: THE PROPOSED WORK IS DIRECTLY RELEVANT TO THE LUNAR DATA ANALYSIS PROGRAM (LDAP), WHICH SEEKS TO "...FUND RESEARCH ON THE ANALYSIS OF RECENT LUNAR MISSIONS IN ORDER TO ENHANCE THEIR SCIENTIFIC RETURN." BY CHARACTERIZING THE POTENTIAL EFFECT THAT REFLECTED PROTONS MIGHT HAVE ON SURFACE SPUTTERING, WE ADDRESS A HIGH-PRIORITY GOAL OF LDAP: "CHARACTERIZATION OF THE GLOBAL VARIABILITY AND STRUCTURE OF THE LUNAR EXOSPHERE". Other Administrative Action $0 6/29/18 Not listed INVESTIGATING THE INTERACTION OF SOLAR WIND PROTONS WITH THE MOON USING ARTEMIS DATA GOALS/OBJECTIVES: THE PRIMARY GOAL OF THIS PROPOSAL IS TO ANALYZE ARTEMIS OBSERVATIONS OF SOLAR WIND PROTONS REFLECTED AT OR NEAR THE MOON IN ORDER TO UNDERSTAND THE INTERACTION OF THE SOLAR WIND WITH THE LUNAR SURFACE AND PLASMA ENVIRONMENT. SPECIFICALLY WE AIM TO ANSWER THE FOLLOWING QUESTIONS: 1. WHAT ARE THE CHARACTERISTICS OF PROTONS REFLECTED FROM THE UN-MAGNETIZED SURFACE AND WHAT DO THEY IMPLY ABOUT THE INTERACTION OF THE SOLAR WIND WITH LUNAR REGOLITH? 2. WHAT ARE THE CHARACTERISTICS OF PROTONS REFLECTED ABOVE MAGNETIZED REGIONS AND WHAT DO THEY IMPLY ABOUT THE INTERACTION OF THE SOLAR WIND WITH LUNAR CRUSTAL MAGNETIC FIELDS? 3. HOW DO REFLECTED PROTONS SUBSEQUENTLY INTERACT WITH AND/OR MODIFY THE LUNAR SURFACE AND PLASMA ENVIRONMENT? METHODOLOGY: THIS PROPOSAL WILL MAKE USE OF THREE YEARS OF PUBLICLY AVAILABLE DATA (2011-2014) RETURNED BY BOTH PROBES OF THE ACCELERATION RECONNECTION TURBULENCE AND ELECTRODYNAMICS OF THE MOON'S INTERACTION WITH THE SUN (ARTEMIS) MISSION. THE ARTEMIS PROBES MEASURE COMPLETE ENERGY- AND ANGLE-RESOLVED ION AND ELECTRON DISTRIBUTIONS AND MAGNETIC AND ELECTRIC FIELDS COVERING ALTITUDES FROM 20-20 000 KM FOR A WIDE RANGE OF LOCAL TIMES AND SELENOGRAPHIC LOCATIONS. WE WILL IDENTIFY REFLECTED SOLAR WIND PROTONS AND CHARACTERIZE THEIR ENERGY AND ANGULAR DISTRIBUTIONS THEIR DEPENDENCE ON SOLAR WIND CONDITIONS AND THE LOCATION OF THEIR REFLECTION FROM THE LUNAR SURFACE AND/OR CRUSTAL MAGNETIC FIELDS (TAKING INTO ACCOUNT THE PATH FROM THEIR REFLECTION POINT THROUGH THE COMPLEX MAGNETIC AND ELECTRIC FIELDS AROUND THE MOON). THE RESULT WILL BE A QUANTITATIVE UNDERSTANDING OF HOW PROTONS REFLECT FROM BOTH LUNAR REGOLITH (THE EQUIVALENT OF THE HAPKE PARAMETERS FOR PHOTONS) AND FROM LUNAR CRUSTAL MAGNETIC FIELDS (REFLECTING THE UNIQUE PLASMA PHYSICS ASSOCIATED WITH SMALL-SCALE LUNAR FIELDS). TO QUANTIFY THE EFFECT THAT SPATIALLY AND TEMPORALLY VARIABLE PROTON REFLECTION HAS ON THE SURFACE WE WILL TRACE REFLECTED PROTON TRAJECTORIES BOTH FORWARDS AND BACKWARDS TO ESTIMATE (1) LOCATIONS WHERE THE SURFACE IS SHIELDED FROM PROTON BOMBARDMENT THUS MODIFYING THE LOCAL SURFACE CHEMISTRY AND REDUCING THE SPUTTERING OF REGOLITH MATERIAL INTO THE EXOSPHERE AND (2) LOCATIONS WHERE SECONDARY REFLECTED PROTON IMPACT COULD ENHANCE SPUTTERING. THE EFFECTS ON THE NEAR-LUNAR PLASMA ENVIRONMENT WILL BE QUANTIFIED BY (1) IDENTIFYING AND CHARACTERIZING SHOCKS AND/OR INSTABILITIES DRIVEN BY REFLECTED PROTONS AND (2) COMPARING ARTEMIS OBSERVATIONS OF LUNAR WAKE PROCESSES IN THE PRESENCE OF REFLECTED SOLAR WIND PROTONS TO CASES WHEN THEY ARE ABSENT. RELEVANCE: THE PROPOSED WORK IS DIRECTLY RELEVANT TO THE LUNAR DATA ANALYSIS PROGRAM (LDAP) WHICH SEEKS TO "...FUND RESEARCH ON THE ANALYSIS OF RECENT LUNAR MISSIONS IN ORDER TO ENHANCE THEIR SCIENTIFIC RETURN." BY CHARACTERIZING THE POTENTIAL EFFECT THAT REFLECTED PROTONS MIGHT HAVE ON SURFACE SPUTTERING WE ADDRESS A HIGH-PRIORITY GOAL OF LDAP: "CHARACTERIZATION OF THE GLOBAL VARIABILITY AND STRUCTURE OF THE LUNAR EXOSPHERE". $0 6/29/18 Not listed INVESTIGATING THE INTERACTION OF SOLAR WIND PROTONS WITH THE MOON USING ARTEMIS DATA GOALS/OBJECTIVES: THE PRIMARY GOAL OF THIS PROPOSAL IS TO ANALYZE ARTEMIS OBSERVATIONS OF SOLAR WIND PROTONS REFLECTED AT OR NEAR THE MOON IN ORDER TO UNDERSTAND THE INTERACTION OF THE SOLAR WIND WITH THE LUNAR SURFACE AND PLASMA ENVIRONMENT. SPECIFICALLY WE AIM TO ANSWER THE FOLLOWING QUESTIONS: 1. WHAT ARE THE CHARACTERISTICS OF PROTONS REFLECTED FROM THE UN-MAGNETIZED SURFACE AND WHAT DO THEY IMPLY ABOUT THE INTERACTION OF THE SOLAR WIND WITH LUNAR REGOLITH? 2. WHAT ARE THE CHARACTERISTICS OF PROTONS REFLECTED ABOVE MAGNETIZED REGIONS AND WHAT DO THEY IMPLY ABOUT THE INTERACTION OF THE SOLAR WIND WITH LUNAR CRUSTAL MAGNETIC FIELDS? 3. HOW DO REFLECTED PROTONS SUBSEQUENTLY INTERACT WITH AND/OR MODIFY THE LUNAR SURFACE AND PLASMA ENVIRONMENT? METHODOLOGY: THIS PROPOSAL WILL MAKE USE OF THREE YEARS OF PUBLICLY AVAILABLE DATA (2011-2014) RETURNED BY BOTH PROBES OF THE ACCELERATION RECONNECTION TURBULENCE AND ELECTRODYNAMICS OF THE MOON'S INTERACTION WITH THE SUN (ARTEMIS) MISSION. THE ARTEMIS PROBES MEASURE COMPLETE ENERGY- AND ANGLE-RESOLVED ION AND ELECTRON DISTRIBUTIONS AND MAGNETIC AND ELECTRIC FIELDS COVERING ALTITUDES FROM 20-20 000 KM FOR A WIDE RANGE OF LOCAL TIMES AND SELENOGRAPHIC LOCATIONS. WE WILL IDENTIFY REFLECTED SOLAR WIND PROTONS AND CHARACTERIZE THEIR ENERGY AND ANGULAR DISTRIBUTIONS THEIR DEPENDENCE ON SOLAR WIND CONDITIONS AND THE LOCATION OF THEIR REFLECTION FROM THE LUNAR SURFACE AND/OR CRUSTAL MAGNETIC FIELDS (TAKING INTO ACCOUNT THE PATH FROM THEIR REFLECTION POINT THROUGH THE COMPLEX MAGNETIC AND ELECTRIC FIELDS AROUND THE MOON). THE RESULT WILL BE A QUANTITATIVE UNDERSTANDING OF HOW PROTONS REFLECT FROM BOTH LUNAR REGOLITH (THE EQUIVALENT OF THE HAPKE PARAMETERS FOR PHOTONS) AND FROM LUNAR CRUSTAL MAGNETIC FIELDS (REFLECTING THE UNIQUE PLASMA PHYSICS ASSOCIATED WITH SMALL-SCALE LUNAR FIELDS). TO QUANTIFY THE EFFECT THAT SPATIALLY AND TEMPORALLY VARIABLE PROTON REFLECTION HAS ON THE SURFACE WE WILL TRACE REFLECTED PROTON TRAJECTORIES BOTH FORWARDS AND BACKWARDS TO ESTIMATE (1) LOCATIONS WHERE THE SURFACE IS SHIELDED FROM PROTON BOMBARDMENT THUS MODIFYING THE LOCAL SURFACE CHEMISTRY AND REDUCING THE SPUTTERING OF REGOLITH MATERIAL INTO THE EXOSPHERE AND (2) LOCATIONS WHERE SECONDARY REFLECTED PROTON IMPACT COULD ENHANCE SPUTTERING. THE EFFECTS ON THE NEAR-LUNAR PLASMA ENVIRONMENT WILL BE QUANTIFIED BY (1) IDENTIFYING AND CHARACTERIZING SHOCKS AND/OR INSTABILITIES DRIVEN BY REFLECTED PROTONS AND (2) COMPARING ARTEMIS OBSERVATIONS OF LUNAR WAKE PROCESSES IN THE PRESENCE OF REFLECTED SOLAR WIND PROTONS TO CASES WHEN THEY ARE ABSENT. RELEVANCE: THE PROPOSED WORK IS DIRECTLY RELEVANT TO THE LUNAR DATA ANALYSIS PROGRAM (LDAP) WHICH SEEKS TO "...FUND RESEARCH ON THE ANALYSIS OF RECENT LUNAR MISSIONS IN ORDER TO ENHANCE THEIR SCIENTIFIC RETURN." BY CHARACTERIZING THE POTENTIAL EFFECT THAT REFLECTED PROTONS MIGHT HAVE ON SURFACE SPUTTERING WE ADDRESS A HIGH-PRIORITY GOAL OF LDAP: "CHARACTERIZATION OF THE GLOBAL VARIABILITY AND STRUCTURE OF THE LUNAR EXOSPHERE". $101.4k 8/25/17