Simulation of a protoplanetary disk accretion activity due to a collision with a gas stream
Vitaliy Grigoryev, Tatiana Demidova
TLDR
3D simulations show how gas stream collisions with protoplanetary disks drive stellar accretion, matching FU Ori observations.
Key contributions
- Used 3D gas-dynamic simulations to model protoplanetary disk-gas stream collisions.
- Investigated how orbital parameters and stream mass affect stellar accretion activity.
- Found orbital inclination and initial stream mass are key drivers of accretion rate.
- Simulation results for accretion rates align with observations of FU Ori type stars.
Why it matters
This study provides a detailed simulation of how gas stream collisions can trigger accretion bursts in protoplanetary disks. Its findings align well with observations of FU Ori stars, offering a plausible explanation for their variable luminosity. This advances our understanding of early stellar evolution.
Original Abstract
The consequences of a protoplanetary disk collision with a gas stream are being studied using three-dimensional numerical gas-dynamic simulation. The influence of orbital parameters and the stream mass on the accretion activity of the star is examined. It is shown that the orbital inclination and the initial mass of the infalling material are the most influential parameters in determining the accretion rate. The obtained accretion rate dependencies are compared with actual observational data for two FU~Ori type stars. It turns out that not only is the maximum accretion rate consistent with observational estimates, but the behavior of the accretion rate over time is very similar to available long-term light curves.
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