|Title||Models of wind-driving protostellar disks|
|Presenter||Raquel Salmeron Zapata (Australian National University)|
|Author(s)||Raquel Salmeron Zapata|
|Session||Mathematical Physics and Industrial Mathematics|
Star formation is induced by the gravitational collapse of molecular clouds cores. During this phase, angular momentum conservation results in the progressive increase of the centrifugal force, which eventually halts the infalling matter and leads to the development of a central mass (“protostar”) surrounded by a disk of material. In the presence of an angular momentum transport mechanism, mass accretion onto the protostar proceeds through this disk, and it is believed that this is how stars typically gain most of their mass. A surprising feature of many of these protostellar accreting systems is their association with powerful outflows of material, which become highly collimated and supersonic as they accelerate away from the source. These jets are thought to play a key role in the dynamics and evolution of these systems, and to the overall process of star and planet formation. In my talk I will present semi-analytical models that calculate the dynamical and thermal structure of protostellar, wind-driving disks, and discuss their application for the analysis of observational data from young stars. I will also present models for the processing of dust particles in wind-driving protostellar disks, the analogues of the early solar system. Our models suggest that these powerful jets may be suitable sites for the formation of chondrules, the primitive, thermally-processed constituents of meteorites whose origin in the cold environment of the early solar nebula has remained elusive for many decades.
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