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THIS IS NECESSARY TOWARDS ESTABLISHING A RIGOROUS UNDERSTANDING OF THESE FUNDAMENTAL HYDRODYNAMICAL PROCESSES IN PROTOPLANETARY ACCRETION DISKS.","funder_award_id":"NNX17AK59G","funder_id":"https://openalex.org/F4320306101","funder_display_name":"National Aeronautics and Space Administration"},{"id":"https://openalex.org/G58316358","display_name":null,"funder_award_id":"NAS 526555","funder_id":"https://openalex.org/F4320306101","funder_display_name":"National Aeronautics and Space Administration"},{"id":"https://openalex.org/G6273510985","display_name":null,"funder_award_id":"26555","funder_id":"https://openalex.org/F4320314503","funder_display_name":"Space Telescope Science Institute"},{"id":"https://openalex.org/G6964326402","display_name":"HOW 100 KM PLANETESIMALS FORM FROM SMALLER MM-CM SIZED PEBBLES IS ONE OF THE BIGGEST UNANSWERED QUESTIONS IN SOLAR SYSTEM FORMATION. WITH THE DISCOVERY OF THE STREAMING INSTABILITY  A ROBUST CANDIDATE HAS EMERGED FOR CLUMPING THESE PEBBLES TO THE POINT OF GRAVITATIONAL COLLAPSE  ALLOWING THEM TO FORM LARGER BODIES. HOWEVER  THERE REMAIN TWO LARGELY UNRESOLVED ISSUES WITH THIS PROCESS. FIRST  THE STREAMING INSTABILITY WILL ONLY TRIGGER CLUMPING FOR A SUFFICIENTLY LARGE CONCENTRATION OF PEBBLES  A CONDITION THAT IS NOT ALWAYS EASILY MET IN DISKS WITH A SMOOTH  MONOTONIC RADIAL STRUCTURE. ADDITIONALLY  THE INITIAL PLANETESIMAL SIZE DISTRIBUTION THAT ARISES FROM NUMERICAL SIMULATIONS IS SIGNIFICANTLY MORE  TOP-HEAVY  COMPARED WITH OBSERVED SMALL BODY SOLAR SYSTEM POPULATIONS. ANOTHER ADVANCEMENT IN RECENT YEARS HAS BEEN THE REALIZATION THAT PRESSURE TRAPS  I.E.  LOCAL GAS PRESSURE ENHANCEMENTS  ARE LIKELY PREVALENT IN PROTOPLANETARY DISKS  ARISING FROM A VARIETY OF PROCESSES  E.G.  THE OUTER EDGE OF PLANET-INDUCED GAPS. WHILE THE IMPORTANCE OF THESE TRAPS HAS BEEN REALIZED IN THE CONTEXT OF PLANET FORMATION AS A WHOLE  THEIR ROLE IN PLANETESIMAL FORMATION VIA THE STREAMING INSTABILITY HAS ONLY BARELY BEEN EXPLORED. THUS  STUDYING THE INTERACTION BETWEEN THESE PRESSURE TRAPS AND STREAMING-INDUCED PLANETESIMAL FORMATION IS ESSENTIAL FOR SEVERAL REASONS. FIRST  AS MENTIONED ABOVE  THESE TRAPS ARE MORE LIKELY THAN NOT TO EXIST IN PROTOPLANETARY DISKS. SECOND  WHILE THESE TRAPS MAY LOCALLY ENHANCE THE CONCENTRATION OF PEBBLES TO STREAMING-UNSTABLE VALUES  THESE EFFECTS MUST COMPETE WITH MOMENTUM FEEDBACK FROM THE PEBBLES ONTO THE PRESSURE TRAP  WHICH COULD DEFORM THE TRAP AND ACTUALLY REDUCE CLUMPING. FINALLY  IF THESE TRAPS CAN SURVIVE  THEY COULD POTENTIALLY CHANGE THE INITIAL PLANETESIMAL SIZES (SINCE STREAMING-UNSTABLE WAVELENGTHS WILL DECREASE NEAR THE TRAP PEAK) AND/OR THE SIZE DISTRIBUTION (IF THE TRAPS MAINTAIN A PEBBLE CONCENTRATION CLOSE TO GRAVITATIONALLY INSTABILITY  PLANETESIMALS MAY FORM ONE-BY-ONE  EACH OF ROUGHLY THE SAME SIZE  EQUATING TO A MORE BOTTOM HEAVY DISTRIBUTION). THUS  WE AIM TO TEST WHETHER PRESSURE TRAPS WILL (A) SURVIVE THE MOMENTUM FEEDBACK FROM PEBBLES TO PRODUCE SIGNIFICANT CLUMPING AND (B) CHANGE THE RESULTING PLANETESIMAL SIZES AND/OR SIZE DISTRIBUTION. PRESSURE TRAPS COULD ALSO PLAY A CRUCIAL ROLE IN PLANET FORMATION. FOR EXAMPLE  AS JUPITER IS BEING FORMED  IT WILL OPEN A GAP THAT GENERATES A PRESSURE TRAP EXTERIOR TO ITS ORBIT. PLANETESIMALS FORMED FROM THIS TRAP COULD CRITICALLY INFLUENCE THE EVOLUTION OF THE SOLAR SYSTEM IN ANY COMBINATION OF THREE POSSIBILITIES: THESE PLANETESIMALS MAY MERGE AND/OR ACCRETE PEBBLES TO EVENTUALLY FORM SATURN  BE SCATTERED AWAY FROM THE PLANET  SOME OF WHICH MAY BE DEPOSITED AS VOLATILE RICH ASTEROIDS IN THE MAIN BELT  AND/OR BE ACCRETED BY JUPITER  PROVIDING THE SOURCE OF JUPITER'S OBSERVED SUPER-SOLAR METALLICITY. IN THIS PROPOSAL WE WILL USE STATE-OF-THE-ART CODES ATHENA (A GAS+PARTICLE DYNAMICS CODE) AND LIPAD (A PLANET FORMATION CODE) TO CARRY OUT THE MOST IN-DEPTH STUDY TO DATE TO TEST THESE CRITICAL IDEAS. SPECIFICALLY  OUR PROPOSED WORK IS OUTLINED INTO THREE TASKS: TASK 1: USE ATHENA TO TEST WHETHER PRESSURE TRAPS WILL SURVIVE FEEDBACK FORCES TO ENHANCE CLUMPING. TASK 2: USE ATHENA TO TEST WHETHER PRESSURE TRAPS WILL CHANGE THE SIZES AND/OR SIZE DISTRIBUTION OF PLANETESIMALS. TASK 3: USE LIPAD TO DETERMINE WHETHER PLANETESIMALS PRODUCED IN A PRESSURE TRAP INDUCED BY PROTO-JUPITER WILL LEAD TO THE FORMATION OF SATURN'S CORE  BE SCATTERED INTO THE ASTEROID BELT  AND/OR ENRICH JUPITER'S ATMOSPHERE.","funder_award_id":"80NSSC18K0597","funder_id":"https://openalex.org/F4320306101","funder_display_name":"National Aeronautics and Space Administration"},{"id":"https://openalex.org/G7505990502","display_name":"MAGNETIC FIELDS AND SELF-GRAVITY ARE LIKELY TO PLAY IMPORTANT AND INTERCONNECTED ROLES IN THE EVOLUTION OF PROTOSTELLAR DISKS AROUND NEWLY FORMED STARS. WE PROPOSE TO USE A COMBINATION OF NUMERICAL SIMULATIONS AND ANALYTIC MODELS TO UNDERSTAND HOW NET MAGNETIC FIELDS EVOLVE DURING A SELF-GRAVITATING DISK PHASE  AND WHETHER CONDITIONS IN SUCH DISKS ALLOW FOR THE COLLISIONAL GROWTH OF ICY PARTICLES AS A PRE-REQUISITE FOR EARLY PLANET FORMATION. WE WILL SPECIFICALLY SEEK TO ANSWER THREE MAIN QUESTIONS: (1) HOW DO SELF-GRAVITATING PROTOSTELLAR DISKS THREADED BY NET MAGNETIC FIELDS EVOLVE? TO ADDRESS THIS QUESTION WE WILL DEVELOP SIMULATIONS THAT INCLUDE SELF-GRAVITY AND EITHER IDEAL MAGNETOHYDRODYNAMICS (MHD) OR NON-IDEAL MHD INCLUDING AMBIPOLAR DIFFUSION. WE WILL QUANTIFY THE EFFECT OF NET FIELDS ON ANGULAR MOMENTUM TRANSPORT IN SELF-GRAVITATING DISKS AND DEVELOP A PHYSICAL UNDERSTANDING OF NET FLUX TRANSPORT THAT CAN BE USED IN LONG-TERM EVOLUTIONARY MODELS. (2) HOW DOES THE NET FLUX OF PROTOSTELLAR DISKS EVOLVE OVER LONG TIME SCALES? WE WILL DEVELOP SIMPLIFIED NUMERICAL MODELS THAT BUILD ON PRIOR WORK BY LUBOW  PAPALOIZOU&PRINGLE (1994) AND GUILET&OGILVIE (2014). (3) HOW IS ENERGY DISSIPATED IN SELF-GRAVITATING DISKS? WE WILL USE IDEALIZED NUMERICAL EXPERIMENTS TO QUANTIFY THE BALANCE BETWEEN DISSIPATION IN LARGE-SCALE SPIRAL STRUCTURES VERSUS SMALL-SCALE TURBULENCE. WE WILL USE THE RESULTS TO BETTER UNDERSTAND WHETHER CONDITIONS IN EARLY PROTOSTELLAR DISKS ALLOW FOR THE INITIAL GROWTH OF ICY SOLID PARTICLES TO LARGER SIZES. THE PROPOSED STUDY IS A THEORETICAL INVESTIGATION INTO HOW BASIC PHYSICAL PROCESSES - DISK SELF-GRAVITY AND MAGNETIC FLUX TRANSPORT - AFFECT THE EVOLUTION OF PROTOSTELLAR DISKS DURING THE FORMATION OF STARS AND PLANETARY SYSTEMS. THE EXPECTED RESULTS ARE RELEVANT TO THE DIRECT IMAGING OF DISK STRUCTURE WITH SPACE ASTROPHYSICS MISSIONS  AND TO THE INTERPRETATION OF EXOPLANET POPULATIONS VIA THEORETICAL MODELS THAT START WITH THE COLLISIONAL GROWTH OF SMALL PARTICLES.","funder_award_id":"80NSSC18K0640","funder_id":"https://openalex.org/F4320306101","funder_display_name":"National Aeronautics and Space Administration"},{"id":"https://openalex.org/G767601387","display_name":null,"funder_award_id":"526555","funder_id":"https://openalex.org/F4320306101","funder_display_name":"National Aeronautics and Space Administration"},{"id":"https://openalex.org/G7938012013","display_name":"I PROPOSE TO PERFORM THREE-DIMENSIONAL (3D) PROTOPLANETARY DISK SIMULATIONS TO BETTER UNDERSTAND THE FORMATION OF PLANETESIMALS, THE SUPER-KILOMETER","funder_award_id":"NNX16AP53H","funder_id":"https://openalex.org/F4320306101","funder_display_name":"National Aeronautics and Space Administration"},{"id":"https://openalex.org/G8210229802","display_name":null,"funder_award_id":"NAS 5-26555","funder_id":"https://openalex.org/F4320306076","funder_display_name":"National Science Foundation"}],"funders":[{"id":"https://openalex.org/F4320306076","display_name":"National Science Foundation","ror":"https://ror.org/021nxhr62"},{"id":"https://openalex.org/F4320306101","display_name":"National Aeronautics and Space Administration","ror":"https://ror.org/027ka1x80"},{"id":"https://openalex.org/F4320314503","display_name":"Space Telescope Science Institute","ror":"https://ror.org/036f5mx38"},{"id":"https://openalex.org/F4320314891","display_name":"NASA Exoplanet Science Institute","ror":"https://ror.org/01trfvq12"},{"id":"https://openalex.org/F4320322037","display_name":"Nuclear Safety and Security Commission","ror":"https://ror.org/05qk3ge34"}],"has_content":{"pdf":true,"grobid_xml":true},"content_urls":{"pdf":"https://content.openalex.org/works/W2952048505.pdf","grobid_xml":"https://content.openalex.org/works/W2952048505.grobid-xml"},"referenced_works_count":52,"referenced_works":["https://openalex.org/W1537224157","https://openalex.org/W1540763227","https://openalex.org/W1595248178","https://openalex.org/W1966876068","https://openalex.org/W1971999183","https://openalex.org/W1972360949","https://openalex.org/W1978197081","https://openalex.org/W1984963133","https://openalex.org/W1990388558","https://openalex.org/W1994819743","https://openalex.org/W2002145423","https://openalex.org/W2023963352","https://openalex.org/W2038546547","https://openalex.org/W2046077662","https://openalex.org/W2054844325","https://openalex.org/W2068306188","https://openalex.org/W2073945818","https://openalex.org/W2075415607","https://openalex.org/W2076434287","https://openalex.org/W2080480291","https://openalex.org/W2082823372","https://openalex.org/W2108433712","https://openalex.org/W2113436460","https://openalex.org/W2116091257","https://openalex.org/W2126016524","https://openalex.org/W2128285906","https://openalex.org/W2132340132","https://openalex.org/W2149470802","https://openalex.org/W2149520698","https://openalex.org/W2160998420","https://openalex.org/W2169385518","https://openalex.org/W2331164329","https://openalex.org/W2525196761","https://openalex.org/W2549068182","https://openalex.org/W2553697453","https://openalex.org/W2594921500","https://openalex.org/W2604548264","https://openalex.org/W2607383648","https://openalex.org/W2613482333","https://openalex.org/W2790910494","https://openalex.org/W2818908231","https://openalex.org/W2898014693","https://openalex.org/W2929032168","https://openalex.org/W2946484731","https://openalex.org/W3042923243","https://openalex.org/W3048087219","https://openalex.org/W3083235728","https://openalex.org/W3100418838","https://openalex.org/W3100998258","https://openalex.org/W3103588278","https://openalex.org/W4297939756","https://openalex.org/W6892942005"],"related_works":["https://openalex.org/W2973038978","https://openalex.org/W7220696567","https://openalex.org/W3045102228","https://openalex.org/W6929462625","https://openalex.org/W2910901336","https://openalex.org/W3043738413","https://openalex.org/W2604548264","https://openalex.org/W3103217861","https://openalex.org/W3103496127","https://openalex.org/W3092642636"],"abstract_inverted_index":null,"counts_by_year":[{"year":2026,"cited_by_count":23},{"year":2025,"cited_by_count":27},{"year":2024,"cited_by_count":19},{"year":2023,"cited_by_count":25},{"year":2022,"cited_by_count":14},{"year":2021,"cited_by_count":26},{"year":2020,"cited_by_count":37},{"year":2019,"cited_by_count":11}],"updated_date":"2026-11-10T11:39:43.021295","created_date":"2019-06-27T00:00:00"}