Abstract
This work presents three-dimensional hydrodynamical simulations with the fully parallel GAGDET2 code, to model a rotating source that emits wind in order to study the subsequent dynamics of the wind in three independent scenarios. In the first scenario we consider several models of the wind source, which is characterized by a rotation velocityVrotand an escape velocityVesc, so that the models have a radially outward wind velocity magnitudeVradgiven by 1, 2, 4, 6, and 8 timesVrot. In the second scenario, we study the interaction of winds emitted from a binary system in two kinds of models: one in which the source remains during the wind emission and a second one in which all the source itself becomes wind. In the third scenario we consider the interaction of a rotating source that emits wind within a collapsing and rotating core. In this scenario we consider only wind models of the second kind built over a new initial radial mesh, such that the angular velocity of the windΩwis 1, 100, and 1000 times the angular velocity of the coreΩc.
Highlights
The star formation process is initiated when random density fluctuations trigger gravitational collapse in large gas structures made of molecular hydrogen
This work presents three-dimensional hydrodynamical simulations with the fully parallel GAGDET2 code, to model a rotating source that emits wind in order to study the subsequent dynamics of the wind in three independent scenarios
We study the interaction of winds emitted from a binary system in two kinds of models: one in which the source remains during the wind emission and a second one in which all the source itself becomes wind
Summary
The star formation process is initiated when random density fluctuations trigger gravitational collapse in large gas structures (called clumps) made of molecular hydrogen. By applying a variant of the sink particle technique described in [16], which was implemented to the public GADGET2 code for dynamically identifying accretion centers, we observe that the first overdensities are formed not in the collision interface of the emitted winds but at the rear of the colliding sources These types of colliding events are not uncommon, as it has been observed that a huge number of massive stars and protostars are forming binary systems with orbital periods short enough for them to be able to exchange mass or even merge during their lifetime; see [17]. We mention the technical problems caused by the very different spatial scales involved; when a source is hosted into the core, the time-step becomes prohibitively small with regard to the achievement of the evolution of the system For this reason, in this paper we have changed the geometry of the initial grid from Cartesian to spherical, so that a set of concentric shells are created and populated with SPH particles. The results of this study showed that wind propagation mainly affects the early evolution of the core, such that the presence of winds does not change the collapsing nature of the rotating core but does slightly change the nature of the filament detected in the densest central region of the core and the resulting products as well
Sign-in/Register to view highlights & summary Sign-in/Register to access full text options 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
