Binary interactions in a static filament
Abstract
From the observational data of Orion A Integral Shaped Filament (ISF), a previous work proposed an oscillatory motion of the gas filament called ``Slingshot Mechanism'' to explain the symmetric spread of older stars (Class II). The wave-like morphology of the filament and the kinematics of the gas and stars support this theory. Using the Astrophysical Multi-purpose Software Enviroment (AMUSE), it was possible to couple an accelerated cylindrical potential with an $N$-body solver to study the dynamics of the stars near the ISF. These simulations were able to reproduce the symmetric spread of the stars around the filament. We are now trying to see if an alternative scenario with a static filament can reproduce the same observational findings. Using MCLUSTER we generate binary systems distributed inside the ridgeline ($r\sim 0.05\,\mathrm{pc}$) of a static analytic filament, to investigate if pure $N$-body interactions can lead to the same final distribution of older stars. Our first test with only 25 binary systems evolved for 2~Myr, and we find that a few stars are ejected from their initial locations to far away distances. However, one low-mass star ($\sim 0.16\,\mathrm{M}_\odot$) was ejected perpendicular to the filament with $v_x \sim -4.1\,\mathrm{km\,s}^{-1}$. As already mentioned in a previous work, using a crude back of the envelope calculation we see that simple $N$-body encounters are not enough to produce the observed symmetric distribution of stars. We still have to check our findings using the correct number of observed stars. These computationally-expensive simulations will be presented in the final thesis of MCM. We also want to check different initial conditions to make sure we can exclude the static filament hypothesis.
- Publication:
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Boletin de la Asociacion Argentina de Astronomia La Plata Argentina
- Pub Date:
- August 2020
- Bibcode:
- 2020BAAA...61R..94M
- Keywords:
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- methods: numerical;
- stars: kinematics and dynamics