5 EJECTA AROUND AN IMPACT CRATER IS TYPICALLY CREATED BY BALLISTIC EMPLACEMENT OF EXCAVATED MATERIAL. ON MARS THERE IS A CLASS OF CRATERS THAT HAS MORPHOLOGICALLY DISTINCT EJECTA: THESE ARE TERMED "LAYERED EJECTA" (LE) CRATERS (OR "LOBATE" EJECTA). THESE CRATERS HAVE A NON-UNIFORM SPATIAL DISTRIBUTION, DISPLAY A VARIETY OF SUBCLASSES, AND COMPRISE 24 PERCENT OF CRATERS WITH DIAMETERS D GREATER THAN OR EQUAL TO 3 KM (ROBBINS AND HYNEK, 2012). LE CRATERS ARE ALSO OBSERVED ON GANYMEDE, EUROPA, AND POSSIBLY MERCURY AND EARTH, BUT THEY ARE MOST PREVALENT ON MARS. TWO MODELS HAVE BEEN PROPOSED FOR THEIR FORMATION. THE FIRST POSITS THAT WHEN IMPACTORS HIT VOLATILE-RICH TARGETS, THE ENERGY MELTS OR VAPORIZES THE VOLATILES, AND THE EJECTA ACTS LIKE A FLUID ("FLUIDIZED MODEL" PER CARR ET AL., 1977). THE SECOND MODEL ARGUES THAT LE CRATERS FORM WHEN THE IMPACT CAUSES WIND TO INTERACT WITH THE EJECTA TO CREATE THE LE APPEARANCE ("ATMOSPHERIC MODEL" PER SCHULTZ AND GAULT, 1979). EACH MODEL HAS IMPORTANT IMPLICATIONS ESPECIALLY THE FLUIDIZED MODEL, AS LE CRATERS COULD THEN BE PROXIES FOR A SOURCE OF WATER OR OTHER VOLATILES. ALTHOUGH THE FLUIDIZED MODEL HAS HAD MORE LITERATURE SUPPORT, THERE HAS BEEN NO DEFINITIVE STUDY CONCERNING WHICH IF EITHER MECHANISM IS PREDOMINANT ON MARS. ADDITIONALLY, ANY MODEL MUST BE RECONCILED WITH THE PRESENCE OF LE SUB TYPES ON AIRLESS BODIES, SOMETHING RECENT MARTIAN WORK HAS NOT DONE. WE PROPOSE TO DETERMINE IF SUB CLASSES OF MARTIAN LE REQUIRE THE FLUIDIZED OR ATMOSPHERIC MODEL, REQUIRE BOTH, OR ARE INCONSISTENT WITH BOTH. THIS WORK WILL BRING TOGETHER DIVERSE MARTIAN DATASETS (CRATER DATA, TOPOGRAPHY, SUB SURFACE WATER MAPS, THERMAL INERTIA MAPS, RADAR OBSERVATIONS, GEOLOGIC MAPS, AND HIGH RESOLUTION IMAGERY) TO TEST HYPOTHESES UNIQUE TO EACH FORMATION MECHANISM. WE WILL INCLUDE CONSTRAINTS FROM THE EXISTENCE OF LE CRATERS ON OTHER SOLAR SYSTEM BODIES, BUT ALL DATA ANALYSIS WILL BE FOR MARS. WE EXPECT TO DEMONSTRATE THAT AT LEAST CERTAIN SUB-CLASSES OF LE ARE FORMED EXCLUSIVELY BY ONE METHOD OR THE OTHER. IF WE WERE TO SHOW THAT SPECIFIC SUB-CLASSES FORMED VIA THE FLUIDIZED MODEL, THEN THE ENVIRONS OF THE ASSOCIATED CRATERS COULD BE TARGETS FOR FUTURE CREWED OR AUTONOMOUS MISSIONS UTILIZING IN SITU VOLATILES. THIS PROPOSAL DIRECTLY ADDRESSES THE MARS DATA ANALYSIS PROGRAM (MDAP) SOLICITATION. OUR INVESTIGATION WILL USE MARTIAN DATA ALMOST EXCLUSIVELY (COMPARISONS WILL BE MADE WITH GANYMEDE, EUROPA, AND MERCURY) AND A VARIETY OF THOSE DATASETS: CRATER DATA GEOLOGIC MAPS TOPOGRAPHY OBSERVATIONS BY GRS, TES, THEMIS, AND SHARAD AND IMAGERY). THE PROPOSED STUDY AIMS TO ANSWER AN IMPORTANT QUESTION THAT MAY LEAD TO A TRACER FOR SUBSURFACE WATER AND PROVIDE NEW CLUES TO MARS' AQUEOUS PAST. THIS STUDY WOULD CONTRIBUTE TO MDAP'S GOAL "TO ENHANCE THE SCIENTIFIC RETURN FROM MISSIONS TO MARS CONDUCTED BY NASA AND OTHER SPACE AGENCIES." Funding Only Action ($24) 1/27/22 Not listed EJECTA AROUND AN IMPACT CRATER IS TYPICALLY CREATED BY BALLISTIC EMPLACEMENT OF EXCAVATED MATERIAL. ON MARS THERE IS A CLASS OF CRATERS THAT HAS MORPHOLOGICALLY DISTINCT EJECTA: THESE ARE TERMED "LAYERED EJECTA" (LE) CRATERS (OR "LOBATE" EJECTA). THESE CRATERS HAVE A NON-UNIFORM SPATIAL DISTRIBUTION DISPLAY A VARIETY OF SUBCLASSES AND COMPRISE 24 PERCENT OF CRATERS WITH DIAMETERS D GREATER THAN OR EQUAL TO 3 KM (ROBBINS AND HYNEK 2012). LE CRATERS ARE ALSO OBSERVED ON GANYMEDE EUROPA AND POSSIBLY MERCURY AND EARTH BUT THEY ARE MOST PREVALENT ON MARS. TWO MODELS HAVE BEEN PROPOSED FOR THEIR FORMATION. THE FIRST POSITS THAT WHEN IMPACTORS HIT VOLATILE-RICH TARGETS THE ENERGY MELTS OR VAPORIZES THE VOLATILES AND THE EJECTA ACTS LIKE A FLUID ("FLUIDIZED MODEL" PER CARR ET AL. 1977). THE SECOND MODEL ARGUES THAT LE CRATERS FORM WHEN THE IMPACT CAUSES WIND TO INTERACT WITH THE EJECTA TO CREATE THE LE APPEARANCE ("ATMOSPHERIC MODEL" PER SCHULTZ AND GAULT 1979). EACH MODEL HAS IMPORTANT IMPLICATIONS ESPECIALLY THE FLUIDIZED MODEL AS LE CRATERS COULD THEN BE PROXIES FOR A SOURCE OF WATER OR OTHER VOLATILES. ALTHOUGH THE FLUIDIZED MODEL HAS HAD MORE LITERATURE SUPPORT THERE HAS BEEN NO DEFINITIVE STUDY CONCERNING WHICH IF EITHER MECHANISM IS PREDOMINANT ON MARS. ADDITIONALLY ANY MODEL MUST BE RECONCILED WITH THE PRESENCE OF LE SUB TYPES ON AIRLESS BODIES SOMETHING RECENT MARTIAN WORK HAS NOT DONE. WE PROPOSE TO DETERMINE IF SUB CLASSES OF MARTIAN LE REQUIRE THE FLUIDIZED OR ATMOSPHERIC MODEL REQUIRE BOTH OR ARE INCONSISTENT WITH BOTH. THIS WORK WILL BRING TOGETHER DIVERSE MARTIAN DATASETS (CRATER DATA TOPOGRAPHY SUB SURFACE WATER MAPS THERMAL INERTIA MAPS RADAR OBSERVATIONS GEOLOGIC MAPS AND HIGH RESOLUTION IMAGERY) TO TEST HYPOTHESES UNIQUE TO EACH FORMATION MECHANISM. WE WILL INCLUDE CONSTRAINTS FROM THE EXISTENCE OF LE CRATERS ON OTHER SOLAR SYSTEM BODIES BUT ALL DATA ANALYSIS WILL BE FOR MARS. WE EXPECT TO DEMONSTRATE THAT AT LEAST CERTAIN SUB-CLASSES OF LE ARE FORMED EXCLUSIVELY BY ONE METHOD OR THE OTHER. IF WE WERE TO SHOW THAT SPECIFIC SUB-CLASSES FORMED VIA THE FLUIDIZED MODEL THEN THE ENVIRONS OF THE ASSOCIATED CRATERS COULD BE TARGETS FOR FUTURE CREWED OR AUTONOMOUS MISSIONS UTILIZING IN SITU VOLATILES. THIS PROPOSAL DIRECTLY ADDRESSES THE MARS DATA ANALYSIS PROGRAM (MDAP) SOLICITATION. OUR INVESTIGATION WILL USE MARTIAN DATA ALMOST EXCLUSIVELY (COMPARISONS WILL BE MADE WITH GANYMEDE EUROPA AND MERCURY) AND A VARIETY OF THOSE DATASETS: CRATER DATA GEOLOGIC MAPS TOPOGRAPHY OBSERVATIONS BY GRS TES THEMIS AND SHARAD AND IMAGERY). THE PROPOSED STUDY AIMS TO ANSWER AN IMPORTANT QUESTION THAT MAY LEAD TO A TRACER FOR SUBSURFACE WATER AND PROVIDE NEW CLUES TO MARS' AQUEOUS PAST. THIS STUDY WOULD CONTRIBUTE TO MDAP'S GOAL "TO ENHANCE THE SCIENTIFIC RETURN FROM MISSIONS TO MARS CONDUCTED BY NASA AND OTHER SPACE AGENCIES." ($24) 1/27/22 4 EJECTA AROUND AN IMPACT CRATER IS TYPICALLY CREATED BY BALLISTIC EMPLACEMENT OF EXCAVATED MATERIAL. ON MARS THERE IS A CLASS OF CRATERS THAT HAS MORPHOLOGICALLY DISTINCT EJECTA: THESE ARE TERMED "LAYERED EJECTA" (LE) CRATERS (OR "LOBATE" EJECTA). THESE CRATERS HAVE A NON-UNIFORM SPATIAL DISTRIBUTION, DISPLAY A VARIETY OF SUBCLASSES, AND COMPRISE 24 PERCENT OF CRATERS WITH DIAMETERS D GREATER THAN OR EQUAL TO 3 KM (ROBBINS AND HYNEK, 2012). LE CRATERS ARE ALSO OBSERVED ON GANYMEDE, EUROPA, AND POSSIBLY MERCURY AND EARTH, BUT THEY ARE MOST PREVALENT ON MARS. TWO MODELS HAVE BEEN PROPOSED FOR THEIR FORMATION. THE FIRST POSITS THAT WHEN IMPACTORS HIT VOLATILE-RICH TARGETS, THE ENERGY MELTS OR VAPORIZES THE VOLATILES, AND THE EJECTA ACTS LIKE A FLUID ("FLUIDIZED MODEL" PER CARR ET AL., 1977). THE SECOND MODEL ARGUES THAT LE CRATERS FORM WHEN THE IMPACT CAUSES WIND TO INTERACT WITH THE EJECTA TO CREATE THE LE APPEARANCE ("ATMOSPHERIC MODEL" PER SCHULTZ AND GAULT, 1979). EACH MODEL HAS IMPORTANT IMPLICATIONS ESPECIALLY THE FLUIDIZED MODEL, AS LE CRATERS COULD THEN BE PROXIES FOR A SOURCE OF WATER OR OTHER VOLATILES. ALTHOUGH THE FLUIDIZED MODEL HAS HAD MORE LITERATURE SUPPORT, THERE HAS BEEN NO DEFINITIVE STUDY CONCERNING WHICH IF EITHER MECHANISM IS PREDOMINANT ON MARS. ADDITIONALLY, ANY MODEL MUST BE RECONCILED WITH THE PRESENCE OF LE SUB TYPES ON AIRLESS BODIES, SOMETHING RECENT MARTIAN WORK HAS NOT DONE. WE PROPOSE TO DETERMINE IF SUB CLASSES OF MARTIAN LE REQUIRE THE FLUIDIZED OR ATMOSPHERIC MODEL, REQUIRE BOTH, OR ARE INCONSISTENT WITH BOTH. THIS WORK WILL BRING TOGETHER DIVERSE MARTIAN DATASETS (CRATER DATA, TOPOGRAPHY, SUB SURFACE WATER MAPS, THERMAL INERTIA MAPS, RADAR OBSERVATIONS, GEOLOGIC MAPS, AND HIGH RESOLUTION IMAGERY) TO TEST HYPOTHESES UNIQUE TO EACH FORMATION MECHANISM. WE WILL INCLUDE CONSTRAINTS FROM THE EXISTENCE OF LE CRATERS ON OTHER SOLAR SYSTEM BODIES, BUT ALL DATA ANALYSIS WILL BE FOR MARS. WE EXPECT TO DEMONSTRATE THAT AT LEAST CERTAIN SUB-CLASSES OF LE ARE FORMED EXCLUSIVELY BY ONE METHOD OR THE OTHER. IF WE WERE TO SHOW THAT SPECIFIC SUB-CLASSES FORMED VIA THE FLUIDIZED MODEL, THEN THE ENVIRONS OF THE ASSOCIATED CRATERS COULD BE TARGETS FOR FUTURE CREWED OR AUTONOMOUS MISSIONS UTILIZING IN SITU VOLATILES. THIS PROPOSAL DIRECTLY ADDRESSES THE MARS DATA ANALYSIS PROGRAM (MDAP) SOLICITATION. OUR INVESTIGATION WILL USE MARTIAN DATA ALMOST EXCLUSIVELY (COMPARISONS WILL BE MADE WITH GANYMEDE, EUROPA, AND MERCURY) AND A VARIETY OF THOSE DATASETS: CRATER DATA; GEOLOGIC MAPS; TOPOGRAPHY; OBSERVATIONS BY GRS, TES, THEMIS, AND SHARAD; AND IMAGERY). THE PROPOSED STUDY AIMS TO ANSWER AN IMPORTANT QUESTION THAT MAY LEAD TO A TRACER FOR SUBSURFACE WATER AND PROVIDE NEW CLUES TO MARS' AQUEOUS PAST. THIS STUDY WOULD CONTRIBUTE TO MDAP'S GOAL "TO ENHANCE THE SCIENTIFIC RETURN FROM MISSIONS TO MARS CONDUCTED BY NASA AND OTHER SPACE AGENCIES." Other Administrative Action $0 9/7/19 Not listed EJECTA AROUND AN IMPACT CRATER IS TYPICALLY CREATED BY BALLISTIC EMPLACEMENT OF EXCAVATED MATERIAL. ON MARS THERE IS A CLASS OF CRATERS THAT HAS MORPHOLOGICALLY DISTINCT EJECTA: THESE ARE TERMED "LAYERED EJECTA" (LE) CRATERS (OR "LOBATE" EJECTA). THESE CRATERS HAVE A NON-UNIFORM SPATIAL DISTRIBUTION DISPLAY A VARIETY OF SUBCLASSES AND COMPRISE 24 PERCENT OF CRATERS WITH DIAMETERS D GREATER THAN OR EQUAL TO 3 KM (ROBBINS AND HYNEK 2012). LE CRATERS ARE ALSO OBSERVED ON GANYMEDE EUROPA AND POSSIBLY MERCURY AND EARTH BUT THEY ARE MOST PREVALENT ON MARS. TWO MODELS HAVE BEEN PROPOSED FOR THEIR FORMATION. THE FIRST POSITS THAT WHEN IMPACTORS HIT VOLATILE-RICH TARGETS THE ENERGY MELTS OR VAPORIZES THE VOLATILES AND THE EJECTA ACTS LIKE A FLUID ("FLUIDIZED MODEL" PER CARR ET AL. 1977). THE SECOND MODEL ARGUES THAT LE CRATERS FORM WHEN THE IMPACT CAUSES WIND TO INTERACT WITH THE EJECTA TO CREATE THE LE APPEARANCE ("ATMOSPHERIC MODEL" PER SCHULTZ AND GAULT 1979). EACH MODEL HAS IMPORTANT IMPLICATIONS ESPECIALLY THE FLUIDIZED MODEL AS LE CRATERS COULD THEN BE PROXIES FOR A SOURCE OF WATER OR OTHER VOLATILES. ALTHOUGH THE FLUIDIZED MODEL HAS HAD MORE LITERATURE SUPPORT THERE HAS BEEN NO DEFINITIVE STUDY CONCERNING WHICH IF EITHER MECHANISM IS PREDOMINANT ON MARS. ADDITIONALLY ANY MODEL MUST BE RECONCILED WITH THE PRESENCE OF LE SUB TYPES ON AIRLESS BODIES SOMETHING RECENT MARTIAN WORK HAS NOT DONE. WE PROPOSE TO DETERMINE IF SUB CLASSES OF MARTIAN LE REQUIRE THE FLUIDIZED OR ATMOSPHERIC MODEL REQUIRE BOTH OR ARE INCONSISTENT WITH BOTH. THIS WORK WILL BRING TOGETHER DIVERSE MARTIAN DATASETS (CRATER DATA TOPOGRAPHY SUB SURFACE WATER MAPS THERMAL INERTIA MAPS RADAR OBSERVATIONS GEOLOGIC MAPS AND HIGH RESOLUTION IMAGERY) TO TEST HYPOTHESES UNIQUE TO EACH FORMATION MECHANISM. WE WILL INCLUDE CONSTRAINTS FROM THE EXISTENCE OF LE CRATERS ON OTHER SOLAR SYSTEM BODIES BUT ALL DATA ANALYSIS WILL BE FOR MARS. WE EXPECT TO DEMONSTRATE THAT AT LEAST CERTAIN SUB-CLASSES OF LE ARE FORMED EXCLUSIVELY BY ONE METHOD OR THE OTHER. IF WE WERE TO SHOW THAT SPECIFIC SUB-CLASSES FORMED VIA THE FLUIDIZED MODEL THEN THE ENVIRONS OF THE ASSOCIATED CRATERS COULD BE TARGETS FOR FUTURE CREWED OR AUTONOMOUS MISSIONS UTILIZING IN SITU VOLATILES. THIS PROPOSAL DIRECTLY ADDRESSES THE MARS DATA ANALYSIS PROGRAM (MDAP) SOLICITATION. OUR INVESTIGATION WILL USE MARTIAN DATA ALMOST EXCLUSIVELY (COMPARISONS WILL BE MADE WITH GANYMEDE EUROPA AND MERCURY) AND A VARIETY OF THOSE DATASETS: CRATER DATA; GEOLOGIC MAPS; TOPOGRAPHY; OBSERVATIONS BY GRS TES THEMIS AND SHARAD; AND IMAGERY). THE PROPOSED STUDY AIMS TO ANSWER AN IMPORTANT QUESTION THAT MAY LEAD TO A TRACER FOR SUBSURFACE WATER AND PROVIDE NEW CLUES TO MARS' AQUEOUS PAST. THIS STUDY WOULD CONTRIBUTE TO MDAP'S GOAL "TO ENHANCE THE SCIENTIFIC RETURN FROM MISSIONS TO MARS CONDUCTED BY NASA AND OTHER SPACE AGENCIES." $0 9/7/19 3 EJECTA AROUND AN IMPACT CRATER IS TYPICALLY CREATED BY BALLISTIC EMPLACEMENT OF EXCAVATED MATERIAL. ON MARS THERE IS A CLASS OF CRATERS THAT HAS MORPHOLOGICALLY DISTINCT EJECTA: THESE ARE TERMED "LAYERED EJECTA" (LE) CRATERS (OR "LOBATE" EJECTA). THESE CRATERS HAVE A NON-UNIFORM SPATIAL DISTRIBUTION, DISPLAY A VARIETY OF SUBCLASSES, AND COMPRISE 24 PERCENT OF CRATERS WITH DIAMETERS D GREATER THAN OR EQUAL TO 3 KM (ROBBINS AND HYNEK, 2012). LE CRATERS ARE ALSO OBSERVED ON GANYMEDE, EUROPA, AND POSSIBLY MERCURY AND EARTH, BUT THEY ARE MOST PREVALENT ON MARS. TWO MODELS HAVE BEEN PROPOSED FOR THEIR FORMATION. THE FIRST POSITS THAT WHEN IMPACTORS HIT VOLATILE-RICH TARGETS, THE ENERGY MELTS OR VAPORIZES THE VOLATILES, AND THE EJECTA ACTS LIKE A FLUID ("FLUIDIZED MODEL" PER CARR ET AL., 1977). THE SECOND MODEL ARGUES THAT LE CRATERS FORM WHEN THE IMPACT CAUSES WIND TO INTERACT WITH THE EJECTA TO CREATE THE LE APPEARANCE ("ATMOSPHERIC MODEL" PER SCHULTZ AND GAULT, 1979). EACH MODEL HAS IMPORTANT IMPLICATIONS ESPECIALLY THE FLUIDIZED MODEL, AS LE CRATERS COULD THEN BE PROXIES FOR A SOURCE OF WATER OR OTHER VOLATILES. ALTHOUGH THE FLUIDIZED MODEL HAS HAD MORE LITERATURE SUPPORT, THERE HAS BEEN NO DEFINITIVE STUDY CONCERNING WHICH IF EITHER MECHANISM IS PREDOMINANT ON MARS. ADDITIONALLY, ANY MODEL MUST BE RECONCILED WITH THE PRESENCE OF LE SUB TYPES ON AIRLESS BODIES, SOMETHING RECENT MARTIAN WORK HAS NOT DONE. WE PROPOSE TO DETERMINE IF SUB CLASSES OF MARTIAN LE REQUIRE THE FLUIDIZED OR ATMOSPHERIC MODEL, REQUIRE BOTH, OR ARE INCONSISTENT WITH BOTH. THIS WORK WILL BRING TOGETHER DIVERSE MARTIAN DATASETS (CRATER DATA, TOPOGRAPHY, SUB SURFACE WATER MAPS, THERMAL INERTIA MAPS, RADAR OBSERVATIONS, GEOLOGIC MAPS, AND HIGH RESOLUTION IMAGERY) TO TEST HYPOTHESES UNIQUE TO EACH FORMATION MECHANISM. WE WILL INCLUDE CONSTRAINTS FROM THE EXISTENCE OF LE CRATERS ON OTHER SOLAR SYSTEM BODIES, BUT ALL DATA ANALYSIS WILL BE FOR MARS. WE EXPECT TO DEMONSTRATE THAT AT LEAST CERTAIN SUB-CLASSES OF LE ARE FORMED EXCLUSIVELY BY ONE METHOD OR THE OTHER. IF WE WERE TO SHOW THAT SPECIFIC SUB-CLASSES FORMED VIA THE FLUIDIZED MODEL, THEN THE ENVIRONS OF THE ASSOCIATED CRATERS COULD BE TARGETS FOR FUTURE CREWED OR AUTONOMOUS MISSIONS UTILIZING IN SITU VOLATILES. THIS PROPOSAL DIRECTLY ADDRESSES THE MARS DATA ANALYSIS PROGRAM (MDAP) SOLICITATION. OUR INVESTIGATION WILL USE MARTIAN DATA ALMOST EXCLUSIVELY (COMPARISONS WILL BE MADE WITH GANYMEDE, EUROPA, AND MERCURY) AND A VARIETY OF THOSE DATASETS: CRATER DATA; GEOLOGIC MAPS; TOPOGRAPHY; OBSERVATIONS BY GRS, TES, THEMIS, AND SHARAD; AND IMAGERY). THE PROPOSED STUDY AIMS TO ANSWER AN IMPORTANT QUESTION THAT MAY LEAD TO A TRACER FOR SUBSURFACE WATER AND PROVIDE NEW CLUES TO MARS' AQUEOUS PAST. THIS STUDY WOULD CONTRIBUTE TO MDAP'S GOAL "TO ENHANCE THE SCIENTIFIC RETURN FROM MISSIONS TO MARS CONDUCTED BY NASA AND OTHER SPACE AGENCIES." Other Administrative Action $0 9/10/18