PROTOSTELLAR DISKS (PPDS) ARE THE NURSERIES OF PLANETS AND FEED THE DEVELOPING PROTOSTAR ITSELF. RECENT GROUND AND SPACE-BASED FACILITIES HAVE STUDIED PPDS IN UNPRECEDENTED DETAIL. APART FROM GALACTIC DISKS THEY ARE THE ONLY ASTRONOMICAL ACCRETION DISKS THAT ARE DIRECTLY ANGULARLY RESOLVED. PPDS ALSO OFFER A WEALTH OF ATOMIC AND MOLECULAR LINES AS WELL AS HIGH-ENERGY CONTINUUM RADIATION RANGING FROM THE ULTRAVIOLET THROUGH X-RAY WAVELENGTHS WHICH IN PRINCIPLE SHOULD ALLOW THE PHYSICAL CONDITIONS AND PROCESSES IN THESE DISKS TO BE DIAGNOSED. THE PROCESSES OF ACCRETION ONTO THE PROTOSTAR AND OUTFLOWS IN WINDS OR JETS ARE OF SPECIAL INTEREST BECAUSE THEY LIMIT THE DISK LIFETIME AND HENCE THE TIME AND MASS AVAILABLE TO FORM PLANETS. THEORETICAL MODELING IS REQUIRED TO INTERPRET OBSERVED LINE AND CONTINUUM DATA AND TO CONSTRAIN THESE PROCESSES. TO A STATE-OF-THE-ART NUMERICAL MAGNETOHYDRODYNAMICS CODE ATHENA++ WE HAVE ADDED MODULES TO SOLVE FOR THE THERMAL CHEMICAL AND RADIATIVE STATE OF PROTOSTELLAR DISKS AND THEIR WINDS. WE ARE NOW USING THESE TOOLS TO STUDY PHOTOEVAPORATIVE WINDS DRIVEN BY THE ULTRAVIOLET THROUGH X-RAY IRRADIATION FROM THE CENTRAL PROTOSTAR. THIS PROPOSAL WILL ASK FOR SUPPORT TO EXTEND OUR TOOLS AND MODELS IN TWO MAIN WAYS. FIRST WE WANT TO CALCULATE ATOMIC AND MOLECULAR LINE STRENGTHS AND SHAPES AND COMPARE THESE WITH OBSERVATIONS IN ORDER TO CONSTRAIN E.G. THE RADIAL PROFILE OF MASS LOSS RATES AND PERHAPS ALSO THE PROCESSES RESPONSIBLE FOR ACCRETION. AT THE MOMENT OUR CODE TREATS ONLY THOSE LINES THAT ARE IMPORTANT FOR HEATING AND COOLING AND IN AN APPROXIMATE AGGREGATED FASHION. SECONDLY WE WANT TO ADD MAGNETIC FIELDS WHICH ARE PROBABLY NECESSARY TO EXPLAIN OBSERVED RATES OF ACCRETION ONTO PROTOSTARS AND WHICH MAY LINK OUTFLOW (WIND) TO INFLOW (ACCRETION) RATES. IN FACT WE HAVE ALREADY SUGGESTED THAT ONGOING ACCRETION SEEN IN TRANSITION DISKS WHOSE PLANETFORMING INNER REGIONS ARE LARGELY EVACUATED OF DUST AND PERHAPS ALSO OF GAS MAY BE EXPLAINED BY WIND-DRIVEN ACCRETION (WANG&GOODMAN 2016). WE WANT TO MODEL THIS IDEA IN DETAIL. ATHENA++ IS ALREADY CAPABLE OF HANDLING FLOWS WITH MAGNETIC FIELDS UNDER IDEALIZED CONDITIONS BUT IN PPDS THE COUPLING OF FIELD AND FLOW DEPENDS UPON THE PARTIAL IONIZATION OF THE GAS. WE MUST UPGRADE OUR THERMOCHEMICAL AND RADIATIVE MODELS TO TREAT THIS ACCURATELY. THERE ARE ALSO CHALLENGING ISSUES REGARDING THE RADIAL MIGRATION OF MAGNETIC FLUX THAT RELATE THE LARGE-SCALE DYNAMICS TO THE SMALL-SCALE GAS PHYSICS. MAGNETIC FIELDS MAY DRASTICALLY AFFECT MASS-OUTFLOW RATES AND HENCE DISK LIFETIMES. WE HOPE THAT SUCH FIELDS WILL ALSO MEASURABLY INFLUENCE LINE PROFILES AND DOPPLER SHIFTS SO THAT WE CAN HOPE TO DISTINGUISH MAGNETIZED WINDS FROM PURELY PHOTOEVAPORATIVELY-DRIVEN WINDS SUCH AS THOSE WE ARE NOW COMPUTING. WE WILL NOT BE MODELING EXOPLANET FORMATION PER SE BUT RATHER THE ENVIRONMENT FROM WHICH EXOPLANETS FORM. IN SOME CASES SUCH AS TRANSITIONDISK INNER HOLES WE MAY PROVIDE ALTERNATIVES TO PLANETARY HYPOTHESES. FUNDS WILL BE REQUESTED TO ALLOW THE PI AND HIS CURRENT GRADUATE STUDENT (WANG) TO CONTINUE TO COLLABORATE ON THIS AFTER THE LATTER RECEIVES HIS PHD AND TO RECRUIT NEW GRADUATE STUDENTS OR A POSTDOC TO THE EFFORT. THIS PROJECT IS RELEVANT TO THE FOLLOWING THEMES OF THE ATP: ``STAR AND EXOPLANET FORMATION " AND "STELLAR ASTROPHYSICS AND EXOPLANETS."