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| EPoS Contribution |
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Simulating accretion and evolution during binary star formation
Rajika Kuruwita NBI, Copenhagen, DK | |
| I present theoretical work done using the AMR MHD code FLASH on the formation of binary stars and the evolution of their discs in these systems. I simulated the collapse of molecular cores until the formation of protostars and followed the early evolution of these systems. I investigated the influence that binarity has on the global evolution of a young stellar system, including looking at mechanisms such as accretion of material, jets and outflows, and dynamical interactions. I find that while in some scenarios binary stars may produce hostile environments for planet formation via the destruction of circumstellar discs, the formation of large circumbinary discs is possible. This can lead to the formation of planets around binary stars to be just as likely as the their formation around single stars. I also present preliminary results on the influence of eccentricity on episodic accretion, independent of separation. | |
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| Caption: Shows phase-folded accretion within the defined eccentricity bins [1.1, 0.7, 0.5, 0.4, 0.3, 0.2, 0.1, 0.0] for a simulation with initial turbulence of Mach=0.2. The transparent blue and orange lines are the median accretion rate for the primary and secondary components of the binary, respectively. The solid green line is the total accretion rate. The error for each bin is taken to be the 16th and 84th percentile. | |
| Collaborators: C. Federrath, ANU, AU T. Haugbolle, NBI, DK |
Key publication
Suggested Session: Cores2Disks |